Bubbles to Chondrites-II. Chemical fractionations in chondrites

We attempt to develop a possible theory of chemical fractionations in chondrites, that is consistent with various features of chondritic components and current observation of protoplanetary disks (PPD). Combining the 3+2 component fitting calculation that simulates chondrule formation process proposed in paper (I) with additional mixing procedures, we investigate essential causes that made various types of chondrites evolve from the uniform solar system composition, the CI-chondritic composition. Seven chemical types of chondrites (CM, CV, CO, E, LL, L and H) are examined, for which reliable chemical compositions for both bulk chondrites and chondrules therein are known. High vaporization degree of the primordial dust aggregates (dustons) required by the calculation vindicates that the chondrule formation was the driving force for the chemical fractionations in all chondrites examined. Various initial redox states in dustons and different timings of CAIs’ invasion to the chondrule formation zone are identified for different chondrite types. These results, together with a good correlation with the D/H ratios of chondrites measured previously, lead us to the notion that PPD evolved from reducing to oxidizing. We explore the heating mechanism for the chondrule formation and the place it occurred. Only heat source being consistent with our chondrule formation model is lightning discharge. We postulate that large vortices encompassing the snow-line are ideal places for large charge separation to occur between dustons and small ice particles, and that direct strikes on dustons should make them boil for ten seconds and longer and allow a swarm of chondrules released from their surfaces. Chemical fractionations are completed by an aerodynamic separation of dustons from chondrules inside the vortex, in such a way that the dustons fall fast into the vortex center and form a planetesimal immediately, while chondrules with dust mantles fall slow and form a thin veneer on the planetesimal surface. During collisional episodes, the veneers are preferentially fragmented and reassemble themselves by a weak self-gravity to form a rubble-piled chondritic asteroid, i.e. chondrite.


Introduction
In pursuit of fundamental rules of chemical fractionations caused by evaporation and condensation of primordial dust aggregates, we have discovered an alternative and compelling route in evolution of chondritic materials in the solar system protoplanetary disk.
From late 1960's to early 1980's, Anders and his group sent out an outstanding array of their research works

Numerical model of chemical fractionation
In our chondrite formation model, we assume the initial material to be primordial dust aggregate having a CI-like composition, CI sil , just as in our paper (I). CI sil is the silicate composition made of the ten oxide elements in CIchondritic proportions, Na, Mg, Al, Si, K, Ca, Ti, Cr, Mn and Fe, only controlled with a parameter f s that is a fraction of Fe oxide in the total Fe in CI. We do this, since Fe can also exist in other redox states such as metal and sulfide (See the detail in paper I).
In our paper (I), as a consequence of jet-droplet ejection in the vapor cloud that enshrouds the duston, we have recognized the three components: jet-droplets, vapor in the cloud (named differential vapor), and fine condensed particles (named integrated vapor). We have modeled chondrule chemistry as a mixture of the three, and successfully reproduced chemical compositions of 75% of the 600 real chondrules. We extend the same method with two more components, on account of the matrix material that coexists with chondrules inside chondrites.

Methods
We wish to solve the five simultaneous linear equations just as in paper (I), A m,n F n = B m (m = 1−5 and n = 1−5).
( 1 ) Here B m represents a molar fraction of element m = 1-4 (Na, Mg, Al and Si in ascending order) in a 'bulk silicate chondrite' . B 5 = 1. F n , an unknown to be determined, represents a mixing proportion (in molar basis) of the five components n = 1-5 (1: jet-droplet, 2: differential vapor, 3: integrated vapor, 4: final integrated vapor and 5: CI * ). By definition n F n = 1. A m,n is a matrix to describe molar fractions of Na, Mg, Al and Si (m = 1-4) among the ten elements in each of the five components (n = 1-5). A 5,n = 1 (n =1-5).
The three components (n = 1-3) are for reproducing a chemical composition of individual chondrules in paper (I). This time they are for an average composition of as many chondrules as available from a single chondrite or from a specified type of chondrites.
The two components (n = 4 and 5) are for making the matrix material in that single chondrite or in that specific type of chondrites. The fourth component (n = 4) represents the integrated vapor composition (viz., a weighted average composition of the total condensed particles) at the end of evaporation from (2021) 8:9 Page 3 of 32 the duston. For simplicity, the vapor lost (both differential and integrated) by reaction with jet-droplets is assumed minimal or zero. The termination of evaporation is signaled with the final VD (vaporization degree) reached by MLB (mother liquid body, viz., melted surface) of the duston, which is made equal to twice the VD that produces the average chondrule composition. It presupposes that the VD for the average chondrule composition is just the halfway of the total evaporation process. CI * (the fifth component) represents the average silicate composition of primordial CI-like dust that has to be mixed with the fourth component to form the matrix material after chondrule formation. CI * is assumed to be omnipresent in PPD, but is distinguished from CI sil which is an immediate source of dustons. We take f s = 0.5 temporarily for CI * . In the following investigation, we have found that Eq. 1 have solutions as long as CI * with f s = 0.3-1.0, but not for CI * with f s < 0.3 for ordinary chondrites. The f s value of CI * has an effect on the relative proportion of the matrix to chondrules, but otherwise it does not affect the calculation result. Hence it is taken as a constant.
A m,n (m = 1-4; n = 1-4) are obtained by calculating the evaporative chemical fractionation similar to the one described in "Model calculation of chondrule chemistry" of paper (I). A m,4 (m = 1-4) is the chemical composition of the final integrated vapor described above and A m,5 (m = 1-4) is that of CI * .
Calculation proceeds with a step size q = 1.001 starting with CI sil for a specified f s , and obtains a set of A m,n at every step number, as described in Paper (I). The q is defined as X Al,k /X Al, , where X Al is a molar fraction of AlO 1.5 in the MLB and k is an evaporation step number, as described in Paper (I). Equation 1 are solved at every step number to give the molar fractions F n . Computation is repeated with f s and step number (viz., VD%) as parameters so as to satisfy the requirement: F n (n = 1 − 5) to be all positive. Only with this requirement, however, multiple solutions exist. We add another constraint to the calculation, the average composition of chondrules. A unique solution is looked for with the parameters f s and VD, that should reproduce the molar fractions of Na and Fe in the average chondrule composition. The choice of Fe is obvious since it is related to the parameter f s . The Na concentration has the largest dynamic range and monotonously changes with VD% over the multiple solutions, making it easy to find a single solution to fit the exact chondrule average value.
The final solution is the one that should satisfy the bulk composition of chondrite as well as the average composition of chondrules included in that chondrite. The number of constraints for the chondrule is two, while four (viz., Na, Mg, Al and Si concentrations) for the bulk chondrite. As explained in paper (I), the four constraints is good enough to fit the composition. However, the two constraints are not enough. For this reason a best fitting is not expected for the average chondrule composition. As it turned out, however, the fitting to the chondrule is also quite satisfactory for the two types of chondrites, L and H.

Handling of CAIs
Unlike fitting individual chondrules in paper (I), the bulk chondrite fitting has two sources of complexity, which are nonetheless very important to understand the chemical fractionations in chondrites. The first one is the existence of inclusions in the bulk chondrites: CAIs (Ca-, Al-rich inclusions) and amoeboid olivine aggregates. They are generally thought to be of foreign origin, from their oxygen isotope composition (e.g., Clayton and Mayeda 1977;Hiyagon and Hashimoto 1999) and other isotopic anomalies (e.g., Wasserburg et al. 1977;Wasserburg et al. 2012), having invaded into the chondrite formation zone. CAIs are very enriched in refractory elements and affect the Al, Ca and Ti concentrations in the bulk chondrite composition (e.g., MacPherson 2014, references therein). Amoeboid aggregates are mostly made of forsterite with some refractory elements (e.g., Grossman and Steele 1976;Hashimoto and Grossman 1987). Their compositions are not so different from the bulk chondrite composition and thus hard to be distinguished from the latter in the calculation. For this reason, they are not considered in the calculation.
We identify two types of CAIs: the ones that later invaded into the chondritic materials and the ones which invaded before the chondrule formation. The former are recognized as CAIs as they are clearly visible in certain types of chondrites (mostly carbonaceous chondrites), while the latter are invisible but only manifest their presence as unusual enrichment in refractory elements in chondrules in certain types of chondrites (e.g., CO chondrites; see Table 1). We call the latter 'ghost CAIs' as we found their existence for the first time.
For the sake of fitting the bulk composition of chondrite that is assumed to consist only of chondrules and matrix, we need to subtract the apparent effect of CAIs that would erroneously raise the concentrations in Al, Ca and Ti in the bulk composition. Therefore, a due amount of CAI is presupposed and subtracted from the bulk composition beforehand. The corrected composition is renormalized to 100 mol% (only the silicate with the ten elements) and then applied with the aforementioned calculation procedure. We try typical CAI compositions and then some atypical composition until a best fit is found. The fitted result should give both the CAI-free bulk chondrite composition and the composition of CAI and its amount, and (2021) 8:9 Page 4 of 32 also the whole rock composition including CAIs, which should be identical to the bulk chondrite composition on the ten element basis. Ghost CAIs are handled in the opposite way. Extra Al, Ca and Ti (and also Mg and Si if necessary) in due amounts are added to the initial composition CI sil , and renormalized to 100 mol% to give a corrected initial composition for the calculation. This corrected initial composition is applied to the aforementioned calculation procedure in order to fit the bulk chondrite composition. We try the simplest Al:Ca:Ti proportion for the added CAIs, which is identical to the CI-chondritic (or solar abundance) ratio and then some atypical proportion until a best fit is found. The fitted result should give the composition of ghost CAI and its amount and also the whole rock composition which should be identical with the bulk chondrite composition.
As will be shown later, both CAIs and ghost CAIs are identified in two types of chondrites (CO and LL). To these chondrites the combination of the two procedures described above is applied.

Correction for the Effect of Aqueous Alteration in the Bulk Chondrites
Another source of complexity is the aqueous alteration of bulk chondrites suggested for certain types of chondrites (e.g., Tomeoka and Buseck 1985;Krot et al. 1998), that should have occurred after accumulation of chondritic components onto a large body, or meteorite parent body as usually supposed. This would have changed the redox state of Fe-bearing phases towards more oxidizing. Specifically Fe metals would have been changed into Fe oxides that could be accommodated into silicate or exist as a certain hydrous oxide phase. The oxidation should be far more effective for matrix materials because of their finegrained and porous nature than for chondrules which are coarse-grained and non-porous. This effect should be removed for the present calculation to be properly executed because it is a secondary effect that has nothing to do with the chondrule formation. The problem is how to recognize and distinguish it from the original redox state of chondrite forming materials before alteration.
A hint is the difference in redox state between the chondrules and the matrix (or the bulk chondrite). The wet-chemical analyses of chondrites distinguish Fe oxides from metals and sulfides. Therefore, the FeO content in the bulk chondrite is known. If it is too abundant as compared with the average FeO content in the chondrules, we should suspect the effect of alteration in the matrix. In order to compensate the FeO content in the bulk chondrite for the effect of alteration, we introduce a (2021) 8:9 Page 5 of 32 factor f w which is the ratio of the FeO concentration in the alteration-free bulk chondrite relative to that in the wet-chemical data. The f w is a factor which is imposed on the FeO concentration in the wet-chemical bulk chondrite data, but not on the average composition of chondrules which are contained in that chondrite. We parameterize f w just like f s in the calculation and find a best fitting value. As it turned out, it is rather easy to find the best fit value within relative errors of 10% or so since other values just do not allow equations to have solutions. As shown later, f w is unity for E, H and L chondrites, while other four types of chondrites have values smaller than unity, implying that aqueous alteration was in action in the latter four chondrites after their accretion to large bodies. Table 1 shows (in the upper columns) the bulk chemical compositions of seven types of chondrites, as well as two CI compositions, on the ten oxide element basis, and also shows (in the lower columns) the average compositions of chondrules contained in each type of chondrites, used in the calculation. The data sources and some adjustments to data are explained in Appendix A.

Results
In the followings we explain the results of numerical fittings in detail for chondrites temporarily grouped according to the fitting procedure commonly applied.

Ordinary Chondrites (L, H and LL types)
Ordinary chondrites are generally presumed CAI-free. Thus the fitting procedure is simple. We obtained a single solution for each chondrite. Figure 1 shows the results of numerical fittings for L, H and LL types of chondrites, by normalizing the abundance of the elements to the CI and Si abundance. The determined parameters as well as proportions of the five components and compositions thereof are thoroughly examined in Section 3.5.
Here we investigate status of the fitting element by element. The four elements calculated, Na, Mg, Al and Si fit exactly the bulk chondrite composition simply because their concentrations are given as known values in the five simultaneous linear equations. The Fe also fits nearly perfectly because it is controlled with parameter f s . The remaining five elements, K, Ca, Ti, Cr and Mn, are left free of preset constraints. As shown in Fig. 1 ('calc bulk' on the left panels), the calculated concentrations in these elements are more or less different from the bulk chondrite values, except for Ca in L and H chondrites. There must be reason or cause for the elements that are not fitted well, which will be explored below.
There are at least two kinds of causes possible. The first is the possibility that the bulk composition and/or the average chondrule composition adopted for the calculation is in error. As long as the bulk compositions of ordinary chondrites are concerned, this possibility is small because only the 'falls' meteorites are used and the average of many chondrite wet-chemical analyses (see Appendix A) are used in the calculation. On the other hand, the EPMA analyses of chondrule compositions may have their own source of error, especially the broad-beam corrections as described in paper (I). Minor elements, i.e., K, Ti, Cr and Mn, may suffer from the problem of detection limits in the EPMA analysis.
Another possibility may be related with the validity including our original experiments that were translated to the volatilities of elements used in the present calculation and our model assumptions about the chondrule and chondrite formation, or with some essential problem such as the initial composition assumed for the primordial dust and some possible effect not included in the calculation.
A survey of the bulk chondrite fitting in Fig. 1 indicates the same trends in all three ordinary chondrites that 1) K, Ti (and maybe Ca) are depleted in the calculation relative to the actual chondrites and 2) Cr and Mn in the calculation are too enriched. The same trends are also seen in the average chondrule fitting in Fig. 1 ('calc cdl ave' on the right panels). The fact implies that these trends are not related with analytical errors in the chondrite and chondrule analyses. They might be attributed to some problem in our calculation, although we cannot think of any defect at the moment. Let us try to find a positive reason for the observed trends. They could originate in the chondrule formation process or be ascribed to the primary features of the dust.
The depletion in Cr and Mn in the actual chondrites and chondrules relative to the calculation may be due to their having partially existed as sulfides in the primordial dust just like Fe-sulfide, which would decrease their concentrations in the silicate dust. Mn and Cr are multi-valent elements like Fe, although they are usually considered most stable as oxides (viz., silicate) in PPD. Mn-bearing and Crbearing iron sulfides are often observed in a reduced type of chondrites such as E chondrites. Some Cr can dissolve into Fe-Ni alloy. For fitting the Cr and Mn concentrations in the bulk ordinary chondrites, ∼20% of Cr and ∼25% of Mn must be removed from the initial CI sil composition. There are two possibilities. (1) Mn and Cr are partially removed in the form of metal and/or sulfide by the metal (+sulfide) -silicate fractionation process, as proposed for explaining the Fe depletion in bulk chondrites relative to CI (Urey and Craig 1953;Larimer and Anders 1970). (2) The wet chemical analyses of bulk chondrites by Jarosewich (1990) do not include the Mn and Cr contents (2021) 8:9 Page 6 of 32 contributed by sulfide and metal. The both possibilities are likely combined to make Mn and Cr depleted in the bulk chondrite compositions relative to the calculation. Table 2 shows the depletion factors to be imposed on the initial CI sil for Cr and Mn to fit the bulk chondrite compositions for seven types of chondrites investigated here. E chondrite, the most reduced type, requires nearly halves of Cr and Mn to be removed from the initial silicate composition. On the other hand, CV and CM (and possibly CO) requires no depletion in Cr, contrary to Mn. This might suggest that Cr favors oxide more than Mn does.
The consistent depletion in K in the calculation (Fig. 1) as compared to the bulk composition and the average chondrule composition is mysterious, especially knowing the fact that the fitting of K is nearly perfect for the other four types of chondrites as will be shown later. Reexamination on the relative volatilities indicates that a factor of two or three more reduction in the relative volatility of K compared to Na is required to explain the K enrichment in the bulk ordinary chondrites. Such an adjustment is against our experimental results which indicated similar relative volatilities for Na and K within errors of a few tens Page 7 of 32 of percent (Nakano and Hashimoto 2020). If the relative volatility of K was adjusted to fit the ordinary chondrites, it should fail for the other four chondrite types. We observe a consistent depletion in Ti (and possibly in Ca) in the calculation relative to both the bulk composition and the average chondrule composition of ordinary chondrites. This implies some enrichment in these elements before the chondrule forming process. It should be related to a CAI invasion before the formation of chondrules, although ordinary chondrites are generally thought being free of CAIs. We will re-examine ordinary chondrites later.

Carbonaceous Chondrites and Enstatite Chondrites
Carbonaceous chondrites contain CAIs up to several volume percent, and need subtraction of their effects before fitting their bulk compositions and average chondrule compositions. Fitting is a process of trial and error by assuming the composition and amounts of CAIs to subtract from the wet-chemical composition of bulk silicate chondrite, while surveying the other parameters, VD, f s and f w at the same time. Let such a tentative, CAI-free bulk composition to be fitted be called, a 'CAI-subtracted bulk composition' . We apply the regular calculation procedure to the CAI-subtracted bulk composition and the average chondrule composition. When the best fitting parameters and appropriate CAI component are found, the bulk composition of chondrite is reconstructed by adding the CAI component, called 'the calculated bulk composition' .
Chondrules in CO chondrites are unusually rich in Al, Ca and Ti as compared to chondrules in any other types of chondrites, as shown in Table 1. The abundances of these elements are 1.6-1.9 times as high as those in CI. This fact suggests that the initial composition of the primordial dust had been pre-enriched in these refractory elements, most probably in the form of invaded CAIs, before the chondrule formation of CO chondrites. We call those CAIs 'ghost CAIs' because they should have become invisible by mixing with the primordial dust during high-temperature melting in the chondrule forming process, but would only appear in the chemistry of the chondrules thus formed. Therefore, CAIs with an adequate composition in an adequate amount must be added to the initial composition CI sil before fitting the bulk and chondrule composition of CO chondrites. We call such a mixed composition a 'CAI-loaded CI silicate composition' . CO chondrites also contain visible CAIs, which can be handled with subtraction of due amounts of CAI just as other carbonaceous chondrites.
Enstatite chondrites are rich in Al in their bulk composition, next to CV as shown in Table 1, although they do not belong to carbonaceous chondrites. As a matter of fact, no solution is obtained without subtracting (Al-rich) CAI before fitting. We have found that 2.3 mol% of an Alrich CAI (Al 0.79 Ca 0.19 Ti 0.02 ; a mixture of more than two phases is possible) is needed to mix after the chondrule formation to reproduce the bulk and chondrule composition of E chondrites. The Ca/Al ratio of E chondrites far lower than that of CI has been an enigma for long. It has been suggested that Ca was mobilized by shock and localized somewhere in the chondrite (Rubin et al. 2009). However, no such occurrence has been found yet. We suggest that E chondrite is unusually enriched in Al due to the incorporation of Al-rich CAI after the chondrule formation. Figure 2 shows the results of numerical fittings for CV, CM, CO and E chondrite. In all of these figures, the bulk Cr and Mn abundances are already fitted with the depletion factors shown in Table 2. The bulk Al, Ca and Ti abundances are fitted with the CAI composition and its amount of subtraction or addition as described above. CV, CM and E chondrites require mixing of CAIs after the chondrule formation. CO chondrites require preenrichment in Al, Ca and Ti (as ghost CAIs) twice as abundant as CI before the chondrule formation, while only a few percent addition of CAIs to the bulk chondrite afterwards. K is left with no fitting effort, which nevertheless shows an extraordinary match between the calculation and the bulk chondrite for all four types of chondrites, as seen in Fig. 2. This is in contrast with the result for ordinary chondrites, which clearly shows a disagreement between the calculation and the bulk chondrites.
The CAIs in CV, CM and CO chondrites predicted by the calculation have chemical compositions of rather common CAIs with the Al:Ca:Ti ratio similar to that of CI composition, consistent with the observation in the real chondrites. The ghost CAIs predicted for CO chondrites also have the same Al:Ca:Ti ratio as CI. The CAIs predicted in E chondrites, however, are very rich in Al and most probably poor in Mg and Si. Such a CAI exists in carbonaceous chondrites, though extremely small in concentration (e.g., MacPherson et al. 1983;Ireland 1988), as compared with common CAIs. In this sense E chondrites, having only Al-rich CAIs predicted, are quite unique and require μm-scaled petrographic study since Al-rich CAIs are usually very small in size. Actually Bischoff et al. (1984) and Guan et al. (2000) have reported such occurrences.
The average chondrule compositions are not so well reproduced by the calculation compared to the bulk compositions, particularly for CV and CM chondrites. It is very likely that the number of chondrules used for averaging is too small, only eight for CV and ten for CM, to be representative of chondrules in those chondrites. Nevertheless the matching to the average chondrule is quite good for Mg and Si, reconfirming the validity of our study.

Ordinary Chondrites Revisited
Knowing a possible existence of ghost CAIs before the chondrule formation in CO chondrites, we hypothesize a pre-mixing of Ti-rich CAI into the primordial dust before chondrule formation, to explain the depletion in Ti and possibly in Ca in the calculation for ordinary chondrites. Figure 3 shows the calculated bulk compositions as well as the calculated average chondrule compositions for the three types of ordinary chondrites, along with the real chondrite compositions for comparison. As in Fig. 2, the bulk Cr and Mn abundances are fitted with the depletion factors shown in Table 2. The CAI-loaded CI silicate composition explained in Section 3.2, shown in bold black (2021) 8:9 Page 9 of 32 lines in the figures, includes the contribution of ghost CAIs to the CI sil . In case of LL chondrites, the CAI composition to be added after chondrule formation is also shown in thin gray line. The final matching is quite satisfactory for the bulk compositions with the K problem remaining persistently, and is fairly good for the average chondrule compositions. Table 3 shows the amount of oxide elements to be entered as ghost CAIs to the primordial CI-like silicate, In Section 3.2 we suggested invasion of the Al-rich CAI to E chondrites after chondrule formation. Its mass, 2.3 mol%, however, is far larger than those for ghost CAIs for ordinary chondrites, and its composition is not Tienriched but Ca-depleted relative to the CI composition. Thus the ghost CAIs for ordinary chondrites are not only different from that for CO chondrites but from the Al-rich CAI in E chondrites.

Question of CI versus Solar Photosphere
So far we have assumed that the initial composition of the primordial silicate dust was the CI composition throughout the present work, with the FeO content controlled with the parameter f s . Figure 4 shows the elemental abundances in bulk CI chondrites and those in the solar photosphere, in various compilations by Lodders (2003) The most important in the chemical fractionation is the Mg/Si ratio since they are the most abundant elements in the silicate. The solar photospheric elemental abundance (SP) in Lodders (2003) has Mg/Si = 1.00 as compared to Mg/Si = 1.04 in CI in Lodders (2003). The difference of 4% has only a small effect on the fitted parameters such as VD and f s , as we performed calculations using both SP and CI abundances. The Ti abundance is questioned. Is the Ti in CI anomalously low? Or is the Ti in SP in Lodders (2003) anomalously high? The CI composition is the average of the three CI chondrites. Its Ti concentration has a very small dispersion relative to its average value, δTi/Ti ∼0.02, much smaller than the normal analytical error in Ti analysis. Therefore the Ti abundance in CI is trusted. If, on the other hand, the Ti in SP (Lodders 2003) is used in the present calculation, invasion of the Ti-enriched, Al-Ca-Ti oxides is not needed to fit the bulk compositions of ordinary chondrites, because of the high abundance of Ti in SP relative to CI as seen in Fig. 4. In a new compilation of SP abundances by Palme et al. (2014), the Ti abundance is revised to the value nearly identical to that of the CI in Lodders (2003). Then the problem of the high Ti abundance for ordinary chondrites persists, and should be explained by the invasion of Ti-enriched, Al-Ca-Ti oxides as ghost CAIs as described in Section 3.3.
The Mn abundance in SP (Palme et al. 2014) has not been revised. Hence Mn in SP is still ∼25% lower than its CI abundance. If the SP abundance was used for Mn, the depletion factors imposed on it for ordinary chondrites, 0.72-0.74 would become ∼1, requiring no depletion for Mn. For those chondrites with larger depletion factors such as CV, E and CO, however, the depletion problem would remain.
In the revised SP (Palme et al. 2014), K is enriched by ∼10% compared to the CI (Lodders 2003). It would compensate the deficit in K in ordinary chondrite types at least in H and LL. On the other hand, it would cause enrichment in K for the other four chondrites as they are perfectly matched with the CI value, as described in Section 3.2.
The analytical precision in determining concentrations of elements are far better in the laboratory chemical analyses than those in the stellar spectrophotometry. Especially the abundances of minor and trace elements recommended for the solar system abundances depend on the meteorite (CI) analyses. On the other hand, the solar photosphere is no doubt representative of the solar system elemental abundances. We rely on CI simply because its elemental abundance is very similar to that of the solar photosphere.

Comparison between Chondrites
We infer probable reasons from the fitted parameters and the determined unknowns, why the chemical variations among the chondrites resulted from the same source material, viz., CI-like primordial dust. Figure 5 (upper panel) and Table 4 show the VD% for various chondrite types. Here the obtained VD indicates Here the VD for a specified chondrite type is the one that satisfies both its bulk composition and the average composition of chondrules included in it. The VD is ∼40% for CM and CO chondrites, ∼30% for CV, E and LL and ∼25% for H and L. We have assumed in the model calculation that the VD of the average chondrule is just a half of the final VD reached by MLB. Then the final VD reached would be twice as large as the VD, viz., 50-80%. These values are consistent with the calculation made for individual chondrules in paper (I). Figure 5 (lower panel) and Table 4 show the f s values for various chondrite types. CV, CM and E chondrites have small f s values, 0.03-0.04, while CO, LL, H and L have relatively high f s values, 0.20-0.27. The definition of f s is the molar fraction of oxidized Fe relative to the total Fe contained in the primordial dust having the CI composition. Therefore, it is likely that the determined f s values reflect the original redox state of the primordial dust before the chondrule formation. CV and CM chondrites are usually considered as oxidized types, but their f s values suggest that they were originally reduced.
The f w values in Table 4 showing 0.1 for fitting CV and CM chondrites suggest that they were aqueously altered and oxidized after accumulation onto their parent bodies. CO and LL chondrites showing f w < 1 also suggest their post-accretional aqueous alteration. E, H and L chondrites having f w = 1, on the other hand, are considered free of alteration. Figure 6 and Table 5 show molar proportions of the five components for the bulk composition and of the three components for the average chondrule composition, determined by the calculation. We can recognize four patterns in Fig. 6. CV is characterized by its high F 1 and   Figure 7 shows the chemical compositions of the five components for three types of chondrites. The components have their own characteristic compositions, but they are similar between different types of chondrites. Therefore, it is the difference in proportion among the five components that distinguishes and determines the bulk composition and the average chondrule composition of a specific type of chondrite. Specifically, E chondrites are Si-rich for the reason that they contain more F 2 (differential vapor) and F 4 (final integrated vapor), which are enriched in Si but depleted in Mg, as shown in Figs. 6 and 7.  27. Thus we suspect that the invasion of CAIs is related with f s , directly or indirectly, for some reason. This aspect will be focused in Section 4.1.
We come to the point what made the difference in chemical composition between different types of chondrites. The f s value most probably inherits the original redox state of the primordial dust. Hence different types of chondrites must have had different redox states in their source materials. This has a profound implication for the chemical evolution of PPD, as will be discussed in the next section.
The different VD values reached by MLB and the different proportions F n 's for different types of chondrites, on the other hand, must have reflected different physical conditions during the chondrule formation. Our current, jet-droplet & vapor-cloud model is premature to give it a full consideration. We are developing a numerical code that includes necessary physics and boundary conditions (Hashimoto and Nakano, in preparation).

Balance of the Elements Involved in the Chemical Fractionation
We try to estimate the balance of the ten elements, 'used' and 'not used' , in forming various types of chondrites from a duston having the CI sil composition. For simplicity, we choose CM, CV and E chondrites for this analysis, which do not require an admixture of ghost CAIs to the duston before the chondrule formation. L chondrite is also chosen because its minute amount of ghost CAI (a Ti-enriched, Page 13 of 32 Ca-Ti oxide) is negligibly small. The data used in the calculation are (i) the compositions of the four components to be mixed and their proportions, F n 's (n =1-4), (ii) the initial composition of duston, viz., CI sil that takes into account the f s value of the chondrite, (iii) the VD% for the average chondrule composition, (iv) the final VD% reached by MLB, viz., a melted surface of the duston, which is taken twice as large as the VD% for the average chondrule, and (v) the composition of the evolved MLB corresponding to the final VD% (called 'evaporation residue' here). Note that the calculation excludes contribution of CAIs that later invaded into the chondrite forming zones. One unknown factor is the production efficiency of jet-droplets ejected throughout the boiling process from VD = 0 to the final VD%. In our experiments (paper I), the run# 138 and run# SZ6 produced jet-droplets with a production efficiency of their integrated mass relative to the total mass lost (as a combined mass of jet-droplets and vapor) by the sample, 11.0 and 11.9 wt.%, respectively. Some other runs produced jet-droplets in a range of 5-10 wt.% relative to the initial masses of experimental charges. In the following calculation, we adopt a round number, 10 mol% (mol% instead of wt.% because VD is also in mol%) for the jet-droplet mass percentage (JDMP), defined as the molar fraction of total jet-droplets released during the boiling of a MLB relative to the initial MLB, for all types of chondrites for simplicity. Figure 9 shows the proportions of the ten elements relative to their initial abundances in CI sil , which reside in Fig. 9 Proportions of each of the ten elements relative to its initial abundance in CI sil , which reside in (A-1) the chondrite forming material (a total of F 1 through F 4 ), (A-2) the leftover residue of MLB that is not used in forming chondrules, and (A-3) the leftover vapor (or condensates) that is also not used in chondrule formation. Page 14 of 32 (A-1) the chondrite forming material (a total of F 1 through F 4 ), (A-2) the leftover residue of MLB that is not used in forming chondrules, and (A-3) the leftover vapor (or condensates) that is also not used in chondrule formation. A JDMP of 10 mol% relative to the initial MLB is assumed for all four chondrites. Note that the purpose of the present calculation is to reveal whereabouts of the elements included in the initial MLB after the chondrule formation. As shown in Fig. 9, A-1 ('Used') takes the elements in amounts necessary for forming the chondritic silicates, but additional mixing of the unprocessed CI * (F 5 : the fifth component), CAI, metal and sulfide are required to form final bulk chondrites. A-2 is particularly enriched in the most refractory Al, Ca and Ti, and Mg comes second. A-3 is rich in Na and K, but also contains considerable Si, Cr, Mn and Fe. The CM chondrite is most efficient in forming a chondrite mass from the MLB, while L, CV and E chondrites must dump 70-80% of the initial mass as residue and vapor. If the constraint of JDMP of 10 mol% is removed, a maximum possible JDMP can be calculated; 11.3, 18.0, 42.4 and 47.0 mol% for CM, E, CV and L chondrite, respectively. Above these percentages, mass balance is not maintained. On the other hand, a minimum JDMP is not limited down to 0%. Fig. 9 (bottom panel) show the case for L chondrite with a JDMP of 47.0 mol% for example. However, such a presentation with a JDMP much larger than 10 mol% may not be strictly valid because our calculation is based on the assumption that a mass loss of MLB by ejection of jet-droplets is minimal.
The important point is that the two components, A-2 and A-3, described above need to be separated from the component A-1 physically; otherwise chemical fractionations in chondrites are not completed. In Section 4.2, we hypothesize a mechanism how the three components were separated and where they were destined for.

Constraints to the Chemical Evolution of PPD
Following the quantitative analyses in configuring bulk chemistry of various types of chondrites (Section 3), we distinguish chondrites between three generation groups in accord with the order of events, CAI incorporation versus chondrule formation. G-1: CAIs were incorporated into chondrite-forming components 'after' the chondrule formation event, as represented by CV, CM and E chondrites. G-2: CAIs were incorporated 'during' the chondrule formation, like CO and LL. G-3: CAIs were incorporated 'before' the chondrule formation, like H and L. If the CAIs formation and their subsequent migration to the outer disk had occurred during a limited period in the PPD evolution, it can be used as a time pivot for whatever processes that are related to the CAIs. Thus the three generations of chondrites recognized above are interpreted as reflecting a formation sequence in the order, G-1 through G-3, as to their chondrule forming events , on condition that the chondrule forming location, viz. its radial distance from the protostar, is fixed.
In Sections 4.2 and 4.4.3, we propose the snowline in the disk as an ideal place for chondrule formation. Thus, if the snowline moved radially in a time scale comparable to or shorter than the CAI migration timescale, the order (G-1 through G-3) might not represent the formation sequence. Here, we continue our investigation by assuming that the snowline was relatively stationary in the radial direction during the period of CAI migration.
As indicated in Section 3.5, f s (a redox indicator of primordial dust or duston) ascends in the order, CV, CM, E, CO, LL, H and L chondrites. This is exactly the same order as G-1→G-2→G-3.
With these facts and the assumption, together with other observational information of chondrites and comets, we attempt to make a prediction about a possible evolutionary sequence of primordial PPD materials.

Evolution in redox state
The increase in f s with the order G-1→G-2→G-3 suggests that the redox state of primordial dust or dustons evolved towards oxidizing with time. We speculate when, where and how it happened.
In their chemical network model of PPD, Walsh et al. (2015) have indicated that gas phase reactions dominate in the inner disk (≤10 au) because of high temperatures and that the reaction of atomic O (produced by photodissociation of CO) with OH (produced by reaction O + H 2 ) proceeds to form molecular oxygen, (2) Furuya et al. (2013), in their reaction network model of PPD, have suggested that at 10 au (∼60 K) ultra-fine ice grains (∼0.1 μm) are continuously supplied to the disk surface by turbulent vertical mixing and destroyed to atoms by stellar UV photons and X-rays, which in turn come back to the disk midplane by turbulence. Atomic oxygen is then converted to molecular oxygen by reaction 2, which becomes a predominant O-bearing species in the disk, given enough time (>10 5 ys).
We propose that the molecular oxygen was radially transported by turbulent diffusion and made the disk gradually oxidized inward as well as outward. This picture qualitatively matches the chronological order of the generation groups of chondrites, G-1 through G-3.
As an alternative, the cometary O 2 can be a source of oxidizer in PPD. The comet 67P/Churyumov-Gerasimenko is known to have kept producing a neutral gas coma with unusually abundant O 2 molecules (O 2 /H 2 O = 0.01-0.1)  during its period of observation. In their model calculations of the chemical evolution of material from the pre-stellar core to the midplane of PPD, Taquet et al. (2016) and Mousis et al. (2016) have investigated the yield of O 2 ice in cometary ice inventories and concluded that the high abundance of O 2 in 67P, if produced solely as O 2 ice by radiolysis, is only adequately explained as having formed in the parent cloud. Eistrup and Walsh (2019) have found a sweet spot parameters for production of O 2 ice in the pre-solar nebula midplane at a level matching those in 67P and 1P/Halley, but preferred a primordial origin in the parent cloud, having considered a sensitivity of such a result to the assumed chemical parameters.
If true, the O 2 -rich cometary materials such as 67P and 1P might be a source for dustons that formed the generation group G-3 (viz., H and L chondrites), while the O 2 -free or -poor cometary materials like most other comets could be a source for the generation group G-1 (viz., CV, CM and E chondrites) and perhaps G-2.
Whichever mechanism of O 2 enrichment in PPD is true, the O 2 molecules must have reacted with metal and sulfide embedded in the primordial dust to form iron oxides. Figure 10 shows D/H ratios in various substances in our solar system and extrasolar environments. CV and CM chondrites which have the lowest f s values and hence are the most reduced types in our study, show the lowest D/H ratios (< 1 × 10 −4 ) among the chondrites (Alexander et al. 2012). LL chondrites which have a higher f s value in our study, show a high D/H ratio (∼ 3 × 10 −4 ) (Alexander et al. 2012). R chondrites, which are not included in our study due to the lack of composition data, is known as the most oxidized type and have the highest D/H ratio (7.26 × 10 −4 ) (McCanta et al. 2008). The comet 67P/Churyumov-Gerasimenko, in spite of its being a J. F. Comet, have the highest D/H ratio (5.3 × 10 −4 ) among the comets ever observed . This comet contains unusually abundant O 2 molecules as described above. All these evidence points to a strong correlation between the high oxidation state and the high D/H ratio.

Evolution in D/H ratio
The water ice is mostly responsible for the D/H ratios of chondrites and comets except some contribution of the organic hydrogen (Alexander et al. 2012). Interstellar ices show the highest D/H ratio of ∼ 10 −2 in the galaxy (Fig. 10). It is postulated that H 2 D + is preferentially produced by ion-neutral reactions in a molecular cloud core and is subsequently turned into ices in the coldest (∼10 K) environment (Cleeves et al. 2014). All matters including gas, ice, silicate and organics in PPD come from a molecular cloud core (e.g., Williams and Cieza 2011). In fact, the D/H ratios of all the solar system materials lie between 10 −2 and 2 × 10 −5 (that of the Sun) as shown in Fig. 10. This implies that some amount Page 16 of 32 of interstellar ice survived the formation of the solar system and was incorporated into planetesimal bodies (Cleeves et al. 2014). Furuya et al. (2013) proposed a model that explains the decrease in D/H ratio of water ice in PPD. Depending on the temperature in the midplane (either <40 K or >60 K), atomic oxygen is either transformed into water ice (regeneration of water ice) by reaction with adsorbed hydrogen on the ice surface, or into molecular oxygen in the gas phase reaction such as reaction 2. Given enough time (> 10 5 ys), the regeneration of water ice reduces the D/H ratio of water ice (Furuya et al. 2013). In the latter case, on the other hand, the initial D/H ratio of water ice tends to be maintained in exchange for depletion of the water ice, and the disk gas becomes gradually loaded with O 2 as described above.
The role of atomic oxygen, however, is not one-sided since both ice-regeneration and O 2 -formation should concur (Furuya et al. 2013) and it is a matter of bias depending on the midplane disk temperature. We postulate that the disk conditions had changed with a timescale ∼ 10 5 years in such a way that the average midplane temperature increased.
The reason why the increase in the D/H ratio of chondrites and comets has a good correlation with the increase in their oxidation states is easily understood because both require the production of free oxygen in PPD.

Chronology of chondrules and CAIs
Here we examine whether the generation sequence of chondrites, G-1→G-2→G-3, is consistent with the chronological information of chondrules and CAIs, on condition that the chondrule forming location, viz., its radial distance from the protostar, is fixed as explained in Section 4.1.
CAIs typically have excess 26 Mg, a trace of extinct radionuclide 26 Al at the canonical level of initial 26 Al/ 27 Al ∼ 5 × 10 −5 , while CAIs with less or no excess 26 Mg are also abundant (see review by MacPherson et al. 1995). Chondrules, on the other hand, generally have no excess 26 Mg, while some have initial 26 Al/ 27 Al ∼ 8 × 10 −6 (e.g., Hutcheon and Hutchison 1989;Russell et al. 1996). With the half-life of 26 Al = 7.3 × 10 5 yr, it has been interpreted that there is an age difference between CAIs and chondrules of ∼2.5 Myr or more. It looks like an immediate contradiction because the chondrule formation of the generation group G-1 (viz., CV, CM and E) occurred before the invasion of CAIs. The generation group G-3, on the other hand, requires that it should have taken CAIs for >2.5 Myr to travel from its formation zone (perhaps the inner rim of the disk; e.g., Dullemond et al. 2007) to the zone of chondrule formation (∼3 au if it coincides with the asteroid belt) because the chondrule formation of the group G-3 (viz., H and L) occurred after CAI invasion.
Considering the mass accretion rate of T-Tauri stars typically of ∼ 10 −8 M per year (Hartmann et al. 2016), such an age difference is comparable to or longer than the time scale for dissipation of the gas disk, and thus unlikely.
Our result implies an irrefutable possibility that the 26 Al ages for chondrules (Davis and McKeegan 2014, references therein) are not real. In our investigation, chondrites except for CV, CM and E types contain ghost CAIs, indicating that chondrules formed from silicate liquids made from a mixture of primordial CI-like dust and invading CAIs. Even if the primordial dust contains no 26 Al, chondrules should have 26 Al as a result of mixed CAIs in the silicate liquid. In fact, CO and LL chondrites for which the invasion of abundant ghost CAIs are implied from the present analysis contain many chondrules having excess 26 Mg, and this is particularly so for their unmetamorphosed types (3.0 or 3.1) (Kita et al. 2000;Mostefaoui et al. 2002;Kunihiro et al. 2004;Kurahashi et al. 2008). Chondrules with high Al contents are preferentially analyzed because of their high precision in determination of 26 Al/ 27 Al (e.g., Kita and Ushikubo 2012). As a matter of fact, the high-Al chondrules exhibit highest 26 Al/ 27 Al values, ∼1/5 of the canonical CAI value (Davis and McKeegan 2014), reinforcing our prediction. We presume that chondrules with high concentrations of live 26 Al simply represent jet-droplets from portions of the silicate liquid in MLB, that is inhomogeneously mixed with large CAIs. We conclude that the 26 Al chronology for chondrules is subject to a serious problem in that their real ages are indeterminable because of the pre-mixing of CAIs which are high in Al and 26 Al. Connelly et al. (2012) and Bollard et al. (2017) have shown that the ages of six among twenty-two chondrules measured with the U-corrected Pb-Pb dating method agree with the average age of four CAIs (4567.30±0.16 Myr) within errors. With this result they claim that chondrules and CAIs are coeval, and that the assumption of the uniform distribution of 26 Al in PPD is wrong. If they are coeval, the time interval for chondrule formation between the group G-1, G-2 and G-3 could be as short as 0.16 Myr, although only six chondrules show such a sign and only four data are available for CAIs ages. Their results, however, appear contradictory because the ages of thirteen chondrules from NWA 5697 (L3) span between 4563.64 and 4567.61 (±0.50) Myr, viz., ∼4 Myr interval. It seems improbable that a single chondrite could reserve chondrules that had been continuously produced in PPD for as long as 4 Myr.
The Pb-Pb chronology for chondrules appears to be free of the problem of CAI mixing unlike 26 Al, but the wide age span of chondrules in a single chondrite cast a doubt on using it as a constraint on the timing of chondrule formation. We explore a little more about the age data. The four CAIs used for determination of their Pb-Pb ages (Bollard et al. 2017) are limited to those in CV chondrites (three from Efremovka and one from Allende). In our study, CV in the generation group G-1 is actually Efremovka itself. The U-corrected Pb-Pb method analyzed only two chondrules that belong to CV chondrites (Connelly et al. 2012). They are Allende chondrules, one of which shows 4567.32±0.42 Myr in good agreement with the CAI age although another is a Myr younger. Thus the chondrules and CAIs in CV chondrites (viz., Efremovka and Allende), as far as the existing data concerned, agree in their ages within analytical errors except one chondrule. This is consistent with our observation of the generation G-1 in which chondrules formed prior to the invasion of CAIs, as long as the time needed for CAIs to migrate to the zone of chondrule formation is short. We therefore suggest that a comparative chronology should be made on chondrules and CAIs that belong to the same chondrite or at least to the same chemical type of chondrites.

Completion of the Chemical Fractionations
Chemical fractionations in chondrites are not completed until the leftover refractory residue of MLB and the leftover volatile vapor (or condensates) are separated from the chondrite-forming ingredients, viz., chondrules and matrix.
The physical separation is only possible through aerodynamic actions operating on objects with different sizes. The leftover evaporation residue is a few-mm thick, oncemolten, surface layer of a large duston with the radius R > 0.01 m. Bodies with R in the 0.01-10 m range lose their angular momentum per unit mass much faster compared to bodies of other sizes, due to their differential motions against the gas. According to Weidenschilling (1977), a body with R = 1 m (solid ρ ∼3 g cm −3 , gas ρ ∼ 10 −9 g cm −3 and T ∼300 K) would migrate to the sun in ∼50 yr per au, while it takes ∼5000 yr per au for R = 0.01 or 10 m (for the same parameters). On the other hand, grains smaller than chondrules (R ≤0.001 m) take ≥ 10 5 yr per au (ibid) and should remain in the chondrule formation zone for a long time.
We propose that dustons were trapped in a large-scale vortex in the protoplanetary disk and that the chondrule formation took place inside the vortex immediately after their entrapment. There the Coriolis force is at work, which pushes dustons of appropriate size, 0.01-10 m in radius, to the center of the vortex in a few rotation periods (e.g., Tanga et al. 1996;Chavanis 2000). The result would be that small objects such as chondrules and finer dust are left near the outer edge of the vortex. Small grains with diameter <1 cm tend to bail out to the outside of the vortex due to turbulent diffusion (Chavanis 2000). Therefore chondrules must grow in size by attaching fine dust rather efficiently (Beitz et al. 2012). Once chondrule-cored nodules and their multiple clusters grow in size >1 cm, they would run after dustons but at a slower pace. In this way we expect three populations being separated from one another as a result of aerodynamic effects: (Pop-1) the chondrule-cored nodules and their clusters that follow the dustons much later in time, (Pop-2) the dustons with refractory residues that settle in the center of the vortex in a short time scale, and (Pop-3) the fine dust, a mixture of the volatile-rich condensate and the primordial CI-like dust, which escape from the vortex. The three populations correspond to the three components that are produced in the chemical fractionation process during the chondrule formation, (A-1), (A-2) and (A-3) as described in Section 3.6, except that Pop-2 consists of A-2 and a nonmelted portion of dustons, and Pop-3 is a mixture of A-3 and the primordial dust.
We discuss the two populations that remain in the vortex. The dustons (Pop-2) are so effectively trapped into the center of vortex (e.g., Barge and Sommeria 1995;Fromang and Nelson 2005;Surville et al. 2016) that a gravitational instability is triggered to generate a large planetesimal (e.g., Tanga et al. 1996). A swarm of the late-arriving, chondrule-cored nodules, viz., Pop-1, would be gravitationally attracted by the planetesimal and accumulate onto its surface, forming a layer of 'chondrite' . As a result the chemical fractionation is completed because the chondrite is spatially segregated from the dustons that form the core of the planetesimal and represent most of its mass. Vortices may not be only attractor of dustons. Any mechanism that attract dustons preferentially (e.g., a dustloaded ring: Surville et al. 2016) could provide a place for forming planetesimals and late veneers of chondrites around them.
As a logical consequence we cast doubt on a hypothetical, meteorite (or chondrite) parent body. The petrologic types (from 3.0 to 7) of chondrites have long been believed as representing thermal metamorphic grades which reflected depths of the sources where the chondrites came from after destruction of the parent body. Rubin (2003Rubin ( , 2004 and Rubin and Wasson (2011) found that the common occurrence of shocked and annealed ordinary and enstatite chondrites is consistent with collisional heating being a major mechanism responsible for metamorphosing those chondrites. Friedrich et al. (2014) found that 26 Al was too depleted to have caused high degrees of thermal metamorphism and partial melting of LL7 chondrites and that heating due to impact is the most likely heat source for the recrystallized chondrites. We'd like to point out that the outermost layers of planetesimals should have been most prone to shocks and disruption by impacts of other bodies. Disrupted pieces may have accumulated on their original planetesimal surface or formed independent rubble piles that were loosely tied with weak gravity, as seen in extant asteroid belts (Walsh 2018). The third population (Pop-3) may have been further mixed with a CI-like dust in the disk and diluted to an insignificant concentration. Recent rendezvous missions to comets, however, revealed high concentrations of crystalline silicates in cometary comas, which are highly enriched in Na and Si relative to Mg (Schulz et al. 2015;Engrand et al. 2016;Bardyn et al. 2017). The enrichment of volatile Na (and K), and Si relative to Mg is exactly a feature of the volatile condensates in the third population (Fig. 9). The third population may also give a hint to the origin of GEMS (Keller and Messenger 2011), UCAMMs (Dobrica et al. 2012) and CPMMs (Noguchi et al. 2015), all of which are suspected to have genetic links to comets.

Comparison with the Equilibrium Condensation Model
Having discussed our new ideas on the origin of the chemical fractionations in chondrites, we come to a point where we could compare our model with those developed by Anders and his group. As described in Section 1, their model basis, viz., the equilibrium condensation of chondritic materials, has lost its reasoning. However, it might be beneficial for us and all to do this since essential points would be clarified. In addition to the chemical aspects which will be described below, there are several physical difficulties attached to their model. 1) The grain size of particles that condense from a gas of low density should be too small to be separated from the gas (Weidenschilling 1977), making the fractionation absolutely ineffective. 2) No reason is given for any particular temperatures at which they claim the fractionations should occur. 3) Chondrules, the most abundant constituent of chondrites, is not taken into consideration.

Lithophile element fractionation
We refer to the major element or refractory lithophile element fractionations in chondrites (Larimer and Anders 1970;Larimer 1979). Larimer and Anders (1970) have proposed that a partial loss of high-temperaturecondensation minerals at appropriate temperatures and a subsequent condensation of minerals which followed from the remaining gas reservoir could explain major chemistry of ordinary and enstatite chondrites, starting from the CI-composition gas. They derived chemical compositions (for the five major elements, Si, Mg, Ca, Al and Ti) similar to those of bulk ordinary (and enstatite) chondrites, by subtracting 15 (25), 23 (45) and 40 (60) % of Si, Mg and Ca (same for Al and Ti), respectively, from the CI composition. Those minerals were identified as typical CAI minerals and forsterite. As they pointed out, these percentages are examples and other combinations are possible. Larimer (1979), based on his analysis on the condensation track of major elements and average compositions of ordinary and enstatite chondrites, have proposed that the bulk mineral chemistry to be subtracted from the CI composition was uniquely determined. His estimates of mass subtraction are not so different from those by Larimer and Anders (1970). In order to explain the bulk chemical compositions of CII and CIII (now classified as CM for CII, and CO and CV subtypes for CIII), Larimer and Anders (1970) inexplicitly and Larimer (1979) explicitly suggested the addition of CAI minerals in appropriate proportions to the CI composition. Larimer and Anders (1970) concluded that the chondrule formation had nothing to do with the lithophile element fractionations, and that chondrules were simply molten droplets of the existing solids.
An essential difference between our model and their model is that we consider the chondrule formation and the subsequent dynamical processes as a primary driving force for the lithophile element fractionation, while they do not. Let us recapitulate our model for the sake of comparison.
As shown in Fig. 9, the initial CI-like material, duston, is processed into three kinds of materials as a result of chondrule formation process in the vapor cloud that forms around it. The chondrule-and matrix-forming components, F 1 through F 4 in the calculation, when combined, are depleted in refractory elements such as Al, Ca and Ti relative to Mg and Si ( Fig. 9; 'Used'). As a result, not only enstatite and ordinary chondrites but also carbonaceous chondrites suffer from depletion in the refractory elements once. The difference among these chondrites is the amount of CAIs which invaded into a zone of chondrite formation. For carbonaceous chondrites, refractory elements (in the form of CAIs) invaded and mixed with chondritic components in amounts more than compensating the lost fraction during the chondrule formation. Enstatite chondrites incorporated Al-rich CAIs in quantity too small to compensate the largest depletion in the refractory elements caused during the chondrule formation. Ordinary chondrites (L and H types) incorporated no CAI except for a trace of ghost CAI, thus remained depleted in the refractory elements. Ordinary chondrites (LL type) incorporated both CAI and ghost CAI, but their combined mass was too small to compensate the depletion in the refractory elements. Such is a brief explanation in our model for the lithophile element fractionations in chondrites.
To complete the chemical fractionation, however, the leftover residue which is enriched in the refractory elements ( Fig. 9; 'Residue'), must be removed from the chondrule-forming zone. This is automatic because the residue is a once-molten surface layer of a large duston which subsequently falls into the center of a large-scaled vortex by the aerodynamic process. The equilibrium condensation model, on the other hand, has no means to remove the high-temperature condensates from their formation zone since they are ultra-fine-grained particles that strongly couple with the gas.
The removal of excess volatiles that are not incorporated into chondrite-forming materials ( Fig. 9; 'Vapor') is also automatic in our model because the vapor condensates, fine-grained in nature, would effectively move away from the vortex by turbulent diffusion. The removed volatiles in the form of low-temperature condensates must include not only Na and K but also highly volatile elements (e.g., Pb, Bi, In, Tl). Therefore, our model does not have to invoke any extra chemical fractionation process such as accretion-temperaturecontrolled fractionation of volatiles proposed by Keays et al. (1971) and Laul et al. (1973) (viz., Chem. fract. in meteorites-IV & -VI).

Redox state and metal-silicate fractionation
Different types of chondrites have different redox states of Fe and different total Fe contents (Urey and Craig 1953). Fe exists in meteorites typically with three different states: oxides (mostly as FeO) in silicates, metals and sulfides. In the latter two, Ni and Co are invariably included as minor elements, which under most redox conditions are not oxidized. Larimer and Anders (1970) examined concentrations of Fe and Ni in various chondrites and ascribed the depletion in total Fe in L and LL chondrites as opposed to H and C chondrites, to the metal-silicate fractionation that had occurred between ∼1050 K and 680 K (temperature for FeS formation) before accumulation of chondritic materials into large bodies.
Larimer and Anders regarded the redox state of minerals in chondrites as reflecting their final equilibration temperatures with the nebular gas. In the equilibrium condensation model of high temperature nebular gas with the solar elemental abundances, Fe metal condenses at ∼1450 K at 10 −3 bar in total pressure (Grossman 1972) and at ∼1280 K at 10 −5 bar (Wood and Hashimoto 1993). No other Fe-bearing phase appears down to ∼900 K where a trace of Fe metal is oxidized and accommodated into Mg-silicates (forsterite and enstatite), but it is not until 700 K (10 −3 bar) or 600 K (10 −5 bar) where olivine takes FeO/(MgO + FeO) = 0.05, which is close to the FeO concentration in enstatite in E-chondrites and in forsterite in a reduced type of CV chondrite, viz., Efremovka. In order to oxidize Fe to a level of FeO/(MgO + FeO) ∼0.2 in olivine typically in ordinary chondrites, temperatures as low as 520 K is required (Wood and Hashimoto 1993).
We point out a contradiction between the above two arguments. The Fe/Ni molar ratios of bulk chondrites are 16.6 for H, 18.6 for L and 19.3 for LL (Jarosewich 1990), while the Fe/Ni ratio in CI chondrites is 18.1 (Lodders 2003). Comparison of the temperature range for the metal-silicate fractionation with those for oxidation of Fe metal, however, implies that the metal-silicate fractionation occurred before the oxidation. If so, the Fe/Ni ratio of chondrites should keep 18.1 if CI was their starting composition. Hence their model with respect to the redox states and metal-silicate fractionation bears an internal inconsistency.
The Fe/Ni ratios of bulk chondrites higher than 18.1 indicates that the oxidation of Fe occurred before the metal-silicate fractionation. L and LL chondrites must have lost a significant mass of metal before their accretion to large bodies. The lower Fe/Ni ratio of H chondrites relative to CI, on the other hand, suggests a gain of excess metal or a loss of silicate before their accretion.
In contrast with Larimer and Anders (1970), the discussions made in Sections 3 and 4.1.1 strongly argue for the possibility that the redox state of Fe in the primordial dust was predetermined before the chondrule formation process and that it evolved with time from reducing to oxidizing, corresponding to the generation sequence of chondrites, G-1 through G-3. This is consistent with the order of the events indicated by the Fe/Ni ratios of chondrites, that the oxidation is followed by the metal-silicate fractionation, since the latter should have occurred during or after the chondrule formation in our model.

In Search of Possible Heat Sources
Our model assumes that the surface of duston was heated above their boiling temperature with some external source of heat. Let us scrutinize possible heating mechanisms in PPD suggested for chondrule formation. Rubin (2000) has considered ten constraints that are related with petrologic and geochemical features of chondrules and made a check list for sixteen heating mechanisms with these constraints (figure 5 in his paper). He has pointed out the three mechanisms being consistent with all the constraints: nebular lightning, magnetic reconnection flares, and gas dynamic shock waves.
We introduce two lines of evaluation procedures apart from his. The first line has to do with the coexistence of chondrules with a matrix. In chondrites the finegrained matrix materials fill interstices between chondrules. Their abundance in volume ranges from 20 to 80%, depending on the type of chondrites. They are free of melting process and generally rich in volatiles including organic materials and water, being characteristic of lowtemperature origin. It means that any heating mechanism which violates the presence and features of the matrix materials is not appropriate for chondrule formation. The second line is the consistency with our chondrule and chondrite formation model, and is considered after the first line.
We apply our evaluation procedures to the following heating mechanisms from Rubin (2000,  Page 20 of 32 lightning, supernova shock waves, magnetic reconnection flares, gas dynamic (nebular) shock wave and planetesimal bow shocks. We also evaluate the following mechanisms, that were postulated since Rubin (2000): shocks in the envelopes of giant protoplanets (Nelson and Ruffert 2005) and current sheets in magnetically active nebula regions (Joung et al. 2004).

Constraints from the coexistence with the matrix, and scrutinization of various heat sources
The first line of evaluation considers the following five constraints. With them, we attempt to scrutinize the heating mechanisms.
a) The matrix materials are characterized by their very fine-grained nature, typically subμm to μm in size. Such fine dust move with gas and are unable to be decoupled from the gas. b) The matrix contains abundant materials and elements that are stable at low temperatures. Although recondensation or regeneration (if such processes followed the destruction during chondrule formation events) might partially restore their low-T features, most indigenous materials such as IOMs (e.g., Alexander et al. 2007) which are suggested as having inherited their isotopic signatures from the low-T, outer disk environments or from the molecular cloud would not survive even a moderate temperature rise. c) The matrix contains presolar grains whose isotopic compositions (e.g., Zinner 1998) are very distinct from those of the common chondrite-forming minerals. Any event, thermal or shock, strong enough to destroy or alter the grains is prohibited. d) The most stringent of all the constraints comes from the D/H ratios of water and organic materials in matrices in various chondrites, which differ from those of the sun and the earth. As already described in Section 4.1.2, different chondrite types appear to possess characteristic ranges in the D/H ratio, which are most likely attributed to the ion-molecule reactions in the molecular cloud (e.g., Tielens 2013) followed by modification in the low-T outer disk (e.g., Alexander et al. 2012;Cleeves et al. 2014). The D/H ratio of water should be easily reset to that of the nebular gas, ∼ 2 × 10 −5 , if temperature exceeded 500 K (Lécluse and Robert 1994) in the presence of the nebular gas. e) Complementary nature of the matrix to the chondrules. Two kinds of complementarity may be identified. 1) Chondrules and matrix show similar isotopic compositions and redox states, as in the case of ordinary and enstatite chondrites. Carbonaceous chondrites, whose matrices are relatively H 2 O-rich, possess oxidized matrices and reduced chondrules, but the oxidation of the matrices are known to have resulted from later hydrothermal actions after accumulation onto a large parent body (e.g., DuFresne and Anders 1962;Clayton and Mayeda 1984). 'Similarity' rather than complementarity may be a better term, but it indicates that both come from the same source, not a chance mixture of different origins.
2) Excess or deficit in abundances of particular elements or isotopes in either of chondrules or matrix cancels out to normal values when chondrules and matrix are combined in their chondritic proportion, viz., the bulk chondrite. It is recognized that chondrules are depleted in metallic elements, as opposed to enrichment in these elements in the matrix, while the bulk chondrite have approximately CI abundances in these elements (Bland et al. 2005). This suggests that the metallic elements lost from the chondrules were mostly recovered by the matrix (e.g., Grossman and Wasson 1985). Isotopic complementarity is a very severe restriction, especially in non-mass-dependent isotopic fractionations, as it suggests some sort of genetic link between them Budde et al. (2016a, b ).
The above four constraints, viz., a, b, c and d disqualify the heat sources or heating mechanisms which raise temperatures of the gas on a large scale in the disk, where fine dust, a source of matrix materials, are immersed. They include supernova and nebular shock waves, magnetic reconnection flares, current sheets, and shocks in the envelopes of giant protoplanets. Planetesimal bow shock and lightning discharge should involve only localized heating of the disk gas, thus most of the fine dust in the disk would escape from heating. They are scrutinized by the second line of evaluation method in the followings.

Scrutinization of planetesimal bow shock model
As described in "Origin of Chondrule Chemistry" in paper (I) and in Section 3.5 in the present paper, jetdroplets are postulated to have ejected from the boiling surface of dustons starting with vaporization degree of MLB from less than 10% and ending with more than 80%. In our experiments (paper I), the MLB completed evaporation (VD >90%) within several seconds. A large size of duston would require more time, typically ≥10 seconds for jet-droplets to be ejected with a wide range of VD.
A high speed planetesimal moving in PPD (with a typical speed of 6 km s −1 relative to the gas) accompanies a bow shock on its front side. According to Ciesla et al. (2004), the thickness of bow shocked zone is about three times of the radius R p of the planetesimal. With R p = 10, 100 or 1000 km, its thickness is 30, 300 or 3000 km. Hashimoto and Nakano Progress in Earth and Planetary Science (2021) 8:9 Page 21 of 32 Then, large dust aggregates immersed in the gas would be heated for duration of 5, 50 or 500 seconds, which is long enough in our criteria. The calculated temperature of a compact dust aggregate of 0.1 cm in diameter in the bow shock, however, reaches only 1600 K. Even with an assumed emissivity of dust being 0.1, which is unrealistically low, the maximum temperature reached is 2000 K, which is still too low to make the dust aggregate boil. Hood (1998) obtained a maximum temperature 2000 K for a dust aggregate by assuming a planetesimal of R p = 70 km and the same values for size and emissivity of dust grain as Ciesla et al. (2004). Much larger dust aggregates like dustons (>3 cm) would decouple from the gas more efficiently and hence would be more strongly heated in bow shock, although we do not have a quantitative estimate. Even if boiling occurred, however, the vapor cloud would be immediately destroyed by shock wave. Dustons would be also smashed into pieces by impact with the planetesimal. Miura et al. (2010) have proposed a possibility of liquid condensation for origin of chondrules that fine dust in the bow shock once evaporate and then condense. They, however, admitted that the condensed material should have the same composition as that of the former dust. Then it would not cause chemical fractionations in chondrules and chondrites from the dust.
We conclude that the bow shock is not a viable heat source for our model of chondrule formation.

Lightning discharge: our last hope
In the terrestrial atmosphere, lightning discharge releases its energy in an extremely confined path (a typical discharge path width is ∼2 mm; Pilipp et al. 1992). This leaves most of the atmospheric volume free of heating except for vicinity of the path which are heated with radiation (Whipple 1966). The path width of lightning discharge postulated for PPD is ∼5000 times of the electron mean free path, viz., ∼5 km for gas density n(H 2 ) ∼ 10 20 m −3 (Pilipp et al. 1992), which is very narrow considering the spatial scale of PPD. Therefore, the lightning discharge clears the first line of evaluation procedure, the coexistence of the matrix. Muranushi (2010) has raised three problems to be overcome for the lightning discharge to be a feasible heat source for chondrule formation: energetics problem, neutralization problem, and destruction problem. We add another constraint: charging-mechanism problem. In the followings we give preliminary but plausible solutions to the four problems, and show that the lightning discharge is compatible with our model of chondrule and chondrite formation.
Charging mechanism The generally accepted concept for the development of the thundercloud charge dipole in the terrestrial atmosphere is the physical separation of oppositely charged particles within the cloud (Saunders 2008). The principal charge carriers are believed to be H 2 O ice particles and their charge separation mechanism has been studied for a long time (reviewed by National Research Council 1986). The H 2 O ice is the most abundant solid substance in PPD and is naturally assumed as a main charge carrier for lightning discharge in space.
We postulate that the chondrule formation occurred in large vortices in PPD as described in Section 4.2. Theoretical works predict that a pressure bump near the snow-line (e.g., Kretke and Lin 2007) induces Rossby wave instability by which anticyclonic vortices develop (e.g., Lovelace and Romanova 2014;Lin and Pierens 2018). If a large vortex (Huang et al. 2018) encompasses the snow-line, the icy dust trapped in it would experience evaporation and condensation in its every rotation period.
According to Saunders (2008), the most promising of all possible charging mechanisms of ice grains in the terrestrial atmosphere is a charging induced by condensation: If the growth rate of ice grains is fast during condensation, more defects (pairs of OH − and H 3 O + ) are created on the ice surface. The H 3 O + diffuses into inside of the ice grains, leaving OH − trapped on the surface. When small ice particles collide with the large ice grains, they remove OH − and become negatively charged, while the large ice grains having lost OH − become positively charged. Takahashi (1978) and Takahashi and Miyawaki (2002) conducted ice charging experiments showing that an ice crystal (∼10 μm in diameter) removed a maximum charge of ∼ 3.3 × 10 −14 C per collision, which translates into a charge surface density of 10 −4 C m −2 . This is more than enough to explain activities of terrestrial thunderclouds (Takahashi 1978). According to Takahashi (1978), however, the charge surface density and its polarity depend strongly on temperature and density of H 2 O molecules in the atmosphere. Since there are no data available for the range of temperature and H 2 O density in PPD, it may be premature to conclude the charging efficiency per collision for nebular ice.
We find a similar situation in the vortex which by anticyclonic rotation would bring trapped dustons from warm (inside the snow-line) to cold (outside) environment. If the mass function of stony dust is biased to large sizes, viz., dustons and their embryos rather than fine dust, most of H 2 O vapor would not immediately condense but supersaturate up until homogeneous condensation generates a numerous number of ultra-fine ice particles (probably sub-micron in size). Dustons and their embryos, on the other hand, would be covered with an icy layer or frost. Dustons gradually decouple from the gas (which also contains fine dust of ice and stone) and spiral down into the center of the vortex, while the fine dust collide with the front and bottom sides of the dustons.
(2021) 8:9 Page 22 of 32 They are similar to the large ice grains in the terrestrial atmosphere, that grow by condensation of water in updrafts of thunderclouds while small ice particles continuously collide with their bottoms. The separation of positively charged dustons and negatively charged ice particles develops an electric field between the two populations.
Once the electric field is established, the dustons and their embryos are electrically polarized so that rebounding ice particles can deprive more negative charges from them, leaving them more positively charged. This results in an enforcement of the field (Saunders 2008). If the vortex radius is comparable to the scale height of the disk gas, it would look like a cylindrical capacitor with electric charges of opposite polarities arranged in concentric circles.
Energetics problem This problem has been recognized as a most formidable one since Whipple (1966) suggested a lightning discharge as a heat source of chondrules. The ultimate energy source (gravitational potential of the protoplanetary disk) is sufficient to melt the chondrules, but most of the energy earned by ingoing larger dust go to the outgoing gas by the angular momentum exchange; little contribute to the random motion, the energy source for the lightning (Muranushi 2010). According to our new chondrule formation mechanism, however, the energy shortage seems easy to overcome because only the surface, a few mm in thickness, of dustons needs melting and evaporation to generate chondrules. The larger the duston's average size, the smaller the total energy would be required if the total stony dust mass in the protoplanetary disk is assumed constant.
The energy source of lightning discharge in the terrestrial atmosphere is the latent heat of water vapor during its condensation in thunderclouds, partially transferred to turbulence and updraft in the developed cells, then partially to charge separation between icy grains (Rakov and Uman 2003). We assume the latent heat of water vapor as the source of the electric energy stored in the nebular vortex, and calculate the minimum radius of the average dustons, whose surface is exposed to lightning discharge and boils to produce jet-droplets and vapor cloud.
For simplicity, the mass ratio of ice to stone in the vortex is assumed to be 3 : 1, and all the stone is used for making dustons of single size (radius, R). It is assumed that all ice once evaporates on a warm side of the vortex and then condense totally on a cold side, releasing the latent heat. This latent heat is eventually used to heat the dustons. We further assume that the duston's surface with a thickness of R is kept molten at 2600 K, and that its one-third thickness, (1/3) R evaporates. The initial temperature of the duston is assumed to be 100 K. A thermal diffusion into the duston below the thickness R is not considered. The adopted duston's thermodynamic properties are: C p = 1.46 kJ kg −1 K −1 ; H m = 6.27 × 10 2 kJ kg −1 ; H v = 8.37 × 10 3 kJ kg −1 (all data refer to enstatite liquid; Chase et al. 1985). The water's heat of vaporization is 2.45 × 10 3 kJ kg −1 . The radiative loss of energy (emissivity = 1) from the duston surface is assumed equal to that for silicate vaporization, which is valid at 2600 K (Hashimoto and Nakano, in preparation).
We obtain R/ R ∼4.0 −1 c , where c is the energy conversion efficiency of the water latent heat to the total energy involved in lightning discharge, multiplied by the conversion efficiency of the latter to the heating of dustons. If R = 3 mm and c = 1, R = 12 mm. This would be a minimum size of dustons, but c would be significantly smaller than 1; if c = 0.001 (for the same R = 3 mm), the duston's radius should be as large as 12 m, which may be too large. Not all dustons would be struck by thunderbolts, but only their small proportion would be, considering the rarity and unpredictable nature of lightning on earth. This would reduce the optimum size of dustons significantly. If we presume c much smaller than 0.001, the productivity of chondrules should be very low, but it would be more favorable from the energy limitation.

Neutralization problem
The protoplanetary disk is not an ideal place for electric fields to build due to its low gas density. If the gas is even slightly ionized, the field is rapidly neutralized by Ohmic currents (Muranushi 2010). Because of the large mean free path of electrons in PPD compared to that in the earth atmosphere, the breakdown field is very small, of the order of ∼10 V m −1 (Muranushi et al. 2015), while on earth it is ∼ 10 6 V m −1 (Rakov 2013). This prevents a large electric field from building up, as small discharges always wipe it out. Nevertheless, Pilipp et al. (1998) contended that global electric fields strong enough to induce lightning could have been generated by gravitational sedimentation of dust particles and size sorting due to gas drag on these particles (Morfill et al. 1993), (1) only if charge transfer processes operated in grain-grain collisions, (2) if the gas phase ionization rate were much lower than that usually assumed for molecular clouds, almost as low as that resulting from decay of long-lived radioactive elements ( 40 K) trapped in the grains alone, (3) if precursors of chondrules were compact with a specific mass density not much lower than 1 g cm −3 , (4) and if the electrical energy was stored in much larger structures. We agree to their assertions except that the driving force for charge separation is the Coriolis force in vortices rather than the disk gravity. The vertical component of gravity in the disk midplane, where much of dust are concentrated, is negligibly small; therefore an updraft with large velocities of unknown origin is needed to lift dust of various sizes to high altitudes, e.g., a disk scale height, where the vertical component becomes significant and causes separation of dust by size difference.
The vortices must have formed in an MRI-inactive, 'dead zone' (e.g., Kretke and Lin 2007), where the ionization source would be limited to radioactive elements and cosmic rays. Pilipp et al. (1998) assumed only 40 K for ionization source, which they found marginal to keep a maximum allowable ionization from triggering global discharges. They did not consider a decay of 26 Al, which could be a strong source of ionization. As Desch and Cuzzi (2000) pointed out, we may take it in a reversed logic that the chondrule formation occurred because 26 Al was already dead due to the time gap between chondrules and CAIs, or because 26 Al was not present in the chondrule formation zone due to its heterogeneous distribution (e.g., Larsen et al. 2011;Krot et al. 2012). We consent to the latter possibility because some types of chondrites (CO and LL chondrites) must have formed at the same time as CAIs, and another types of chondrites (CV, CM and E chondrites) could have formed even before the CAI formation. We also propose that any radioactive elements could not have been an effective ionization source because of the large size of dustons and because of the mass function biased to large aggregates. The electron (and perhaps positron) penetration depth is proportional to their energy, ∼1.7 mm per MeV (Kanaya and Okayama 1972). Therefore, only a few mm surface layer of the dustons may be liable to contribute to ionization of the gas; most of the mass which resides inside the dustons would not. Muranushi (2010), in his rebuttal argument to the experiment by Güttler et al. (2008), pointed out that either the electron mean free path is many orders of magnitude shorter or the electron kinetic energy is much larger compared to the protoplanetary disk environment.

Destruction problem
We rather pay attention to the conclusion by Güttler et al. (2008) that the fragmentation of experimental dust aggregates is attributed to the expansion of the discharge channel. In PPD the discharge channel is presumably very wide (e.g., 5 km; Morfill et al. 1993) compared to that in the experiment (Güttler et al. 2008; no description but maybe ≤1 mm) and the discharge would continue for much longer duration (e.g., 10-100 s; Morfill et al. 1993) as compared to ∼60 μs in their experiment. Therefore, dust aggregates in the discharge channel in PPD would be completely molten before the channel explosively expands as a result of the vanishing magnetic fields around the channel.

Lightning discharge: consistency with our new model
We place three conditions on evaluating the lightning discharge as a possible heating mechanism for chondrule formation: (i) the temperature of the duston's surface is kept above its boiling point for duration of 10 s or longer; (ii) the vapor cloud is kept for the same duration; and (iii) the matrix-forming fine dust coexist nearby at low temperatures. We also add one more condition, (iv) that the chondrules that formed in the lightning bolt should possess a large NRM (natural remnant magnetization) because of the magnetic field formed around the discharge path. Morfill et al. (1993) estimated the energy available from a high temperature plasma of ∼30 eV for heating dust grains in the discharge path, using a scaling of the typical terrestrial bolt of lightning applied to a low density nebular gas. Due to a large mean free path of electrons, ∼1 m for n(H 2 ) ∼ 10 20 m −3 , the discharge path width is ∼5000 m and the duration of a lightning pulse is of the order 10-100 s (Morfill et al. 1993). Because of the wide cross section of the path and the prolonged duration of heating, the energy to impart to dust grains is diluted as opposed to the terrestrial one (width ∼1 mm; duration <1 millisecond). This could be enough to melt grains as small as chondrules (Morfill et al. 1993;Horányi et al. 1995), but is in no way sufficient for boiling the surface of dustons.
We predict a new mechanism for heating dustons, a direct strike by the lightning bolt. The allowable electric field in the nebula is restricted by the dielectric strength of the molecular hydrogen. This limits the electric field inside vortices of the order of 10 V m −1 (0.14-30 V m −1 depending on the models of dielectric strength; Muranushi et al. (2015). This field is so weak compared to a typical terrestrial thundercloud field of 1-2×10 5 V m −1 (Rakov 2013) that a large scale charge separation, 10 6 -10 8 m, is required to build an electric potential of 10 7 -10 9 V, typical of terrestrial thunderclouds. Therefore, the discharge path in the nebular gas might be a very long trail. Our concern, however, is not the trail itself (which is usually assumed a heating scene of involved dust aggregates) but its destination: how the discharge tip of the stepped leader (e.g., Rakov and Uman 2003), a pathfinder so to speak, finds its partner in opposite polarity. Our hypothetical dustons are the one, since their 'point charge' fields stand out in the general field, like trees and lightning rods as a terrestrial analogue. One unlucky duston struck by the leader is among a large number of dustons which we postulate distributing equally-spaced in a plane that extends laterally more than thousands of km. A swarm of secondary electrons and ions from the attacked duston may find another duston nearby, and the discharge process should cascade.
Once the duston's surface temperature rises high enough for evaporation of the icy layer and other volatiles, the first vapor cloud forms whose density exceeds that of the nebular gas by orders of magnitude. This would (2021) 8:9 Page 24 of 32 make a mean free path shorter by the same magnitude and converge the wide discharge path into a narrow string similar to the terrestrial lightning. From this on until discharge ends (for 10-100 s), the duston's surface continues to boil and the vapor cloud is maintained.
The cold fine dust exists outside of the discharge path. If the path is more confined by being shepherded by dustons, rather than being spread over kilometers, a nearby volume of the nebular gas around the vapor clouds may be also free of heating and ready to mix its contained fine dust with chondrules. Wasilewski and Dickinson (2000) found that the tetrataenite-bearing chondrules in Bjurbole (L/LL4) and Chainpur (LL3) chondrites exhibited very high REM values (the ratio of NRM/SIRM) of > 100 × 10 −3 , indicating that these chondrules were magnetized in a strong magnetic field of the order of 100 mT (1000 G). According to their arguments, this high REM in the terrestrial rocks is associated only with a direct strike by lightning discharge. In our new chondrule formation mechanism, supercooled liquid droplets solidify and cool below the curie temperature (770°C for tetrataenite; Herndon and Rowe 1974) inside the vapor cloud that exists only during the lightning discharge because the discharge path expands explosively at the moment electric currents vanish.
Our postulate, the lightning discharge as a heat source of boiling dustons, needs quantitative interrogation. We do not deny a more plausible mechanism to be found in future.

Conclusions
In paper (I), Nakano and Hashimoto have carried out evaporation and condensation experiments and applied the results to chondrules, explaining all the primary features of chondrules including their chemistry. On this basis they proposed a new model of chondrule formation that begins with dense and large aggregates of primordial CI-like dust, called 'dustons' . Jetdroplets are ejected from the boiling surface of duston and react with the vapor and the condensate while their traveling through the vapor cloud. Origin of chondrules.
This paper started as a sequel to paper (I), in that basically the same model and calculation procedure are applied to the bulk chemistry of chondrites, but having seen entirely new results on the origin of chondrites, we have expanded our view to the evolution of PPD materials to planetesimals. We highlight the following aspects in conclusions.
(i) The duston-vapor cloud model include the five components: jet-droplets, differential vapor, integrated vapor, final integrated vapor and CI * dust. The first three components make chondrules and the last two components make the matrix of chondrites, altogether forming the bulk chondrite. CAIs which later mixed with the chondrite-forming components is added as a sixth and foreign component to the model to explain CAI-bearing chondrites. We have found that in four types of chondrites CAIs had mixed with the primordial dust before the chondrule formation. and it occurred after the CAI invasion for H and L. The concomitant increase in f s values with this chronological sequence indicates that the PPD environment changed from reducing to oxidizing in time.
We have found that this sequence is also related to the D/H ratios of various solar system and extrasolar substances. We propose that the D/H ratio and the concentration of O 2 molecules in PPD increased with time as PPD evolved.
(iv) The chronological order of the chondrule formation and the CAI invasion revealed in this study is in conflict with the 26 Al chronology of CAIs and chondrules. We have found that dating of chondrules with live 26 Al is an artifact due to invasion of ghost CAIs before the chondrule formation, which contaminated the primordial dust with a live 26 Al. The Pb-Pb dating of CAIs and chondrules seems compatible with our result as long as CAIs and chondrules in the same chondrite are used. (v) To complete the chemical fractionation, the chemically fractionated materials must be physically separated. Our model offers a natural selection according to the principle of aerodynamic friction in PPD because as a result of chondrule formation, materials are divided into three populations with different size ranges. The chondrule-cored, dust-mantled nodules and their clusters are supposed to be millimeters to centimeter in size; the dustons with heat-scorched surfaces are more than 3 cm in diameter; and the leftover fine condensates and indigenous primordial dust, that fail to stick to chondrules, would be typically less than μm in size. (vi) We propose that the chondrule formation occurred inside the large vortices which encompass the snowline in PPD. We envisage that the dustons, whether heat-scorched or kept intact, fall faster into the center of the vortex and ultimately form a planetesimal while the chondrule-cored nodules fall slower and form a veneer on the planetesimal, thus completing a physical separation. The fine dust would not fall but slowly bail out from the vortex. (vii) Having discussed our new ideas on the origin of the chemical fractionations in chondrites, we compare our model with those developed by Anders and his group, viz. the equilibrium condensation model. Our model provides a better explanation for the lithophile element fractionations in chondrites particularly because it explains the completion of the fractionation as a natural consequence of the chondrule formation from dustons, while the equilibrium condensation model has no clue to this problem. The condensation theory is in conflict with the metalsilicate fractionation observed in chondrites, while our model can be compatible because the fractionation must have occurred during or after the chondrule formation. (viii) We have scrutinized a dozen heat sources for chondrule formation based on our new measures. Only one possible heat source is left compatible with our chondrule and chondrite formation model: lightning discharge. We propose that a large-scaled charge separation, 10-100 thousand kilometers apart inside the vortex, is possible between dustons and ice particles with opposite charges and induces direct discharge strikes on the surface of dustons for more than 10 seconds, energetic enough to make dustons boil and generate a swarm of chondrules. A direct strike is also compatible with the large NRM recorded in chondrules. (ix) Chondrites are full of shocked records, which could be explained by their formation history that during the era of planet formation, violent planetesimalplanetesimal collisions should have caused their chondritic veneers stripped off. Fragments were later bound together with a weak self-gravity: rubble piled asteroids, which are likely sources of chondritic meteorites.
Finally, we have not positively included oxygen isotope data in the argument since our model, as it stands now, is not in need of those to construct it. A plethora of the isotopic data on chondrules, chondrites, CAIs, and other solar system materials, including Earth and Moon requires a full of consideration, which is difficult to do due to space limitation. Tactically, however, it will be wise to use the whole data not only for assessing our proposed model but also for guiding our coming works (Hashimoto et al., in preparation).

APPENDIX (A) Data
All data in Table 1 are chemical compositions of silicates in mol% on the ten element basis. The bulk chemical compositions of chondrites are mostly from the wetchemical analyses compiled by Jarosewich (1990). The wet-chemical method has several advantages compared to others, which are crucial in the present study. It usually uses a bulk of rock sample of 8-20 grams for each chondrite. Chondrites contain various petrographic units and mineral phases which are different in size, composition and chemical state. They are not necessarily homogeneously distributed inside the bulk chondrite, so that a few grams of rock sample may not represent its bulk composition. According to Jarosewich (1990), 20 grams of meteorite, whenever possible, is routinely allocated in order to assure homogeneous and representative powders. The wet-chemical analysis distinguishes between Feoxides, metals and sulfides. This is also necessary in our study.
The average composition of chondrules is a simple average of broad-beam EPMA data of individual chondrules that belong to a single chondrite or to a specified type of chondrites. Precision and reliability of such analyses are described in paper (I). Here the important fact is that those EPMA data represents only silicate portions of chondrules because metals and sulfides included in chondrules are routinely avoided in the analyses.