- Research article
- Open Access
Mantle-derived fluids in the Nankai Trough Kumano forearc basin
© The Author(s). 2018
- Received: 1 March 2018
- Accepted: 23 October 2018
- Published: 29 November 2018
Noble gas abundance and isotope data from 12 drilling mud gas samples obtained during IODP Expeditions 338 and 348 provide new insights on fluid origin and fluid migration in the inner accretionary prism below the Kumano forearc basin offshore SE Japan. The samples originate from three adjoining boreholes (C0002F, C0002N and C0002P) spanning depths between 950 and 3050 meters below sea floor (mbsf) and are composed of air and variable contributions of mantle-derived and crustal fluids.
Air-corrected 3He/4He ratios of samples from Exp. 338 fall between 0.44 ± 0.24 Ra and 3.26 ± 0.28 Ra. Samples #1400 and #1800 (sample number denotes depth in mbsf) are more influenced by radiogenic helium (1.33 ± 0.34 Ra resp. 0.44 ± 0.24 Ra), whereas the air-free helium isotopic composition of sample #950 is clearly higher (3.26 ± 0.28 Ra). Enhanced radon activity around 950 mbsf, 1100 mbsf, 1400 mbsf, and 1800 mbsf suggests active flow of fluids at these depths.
The helium isotopic composition of two other samples (#1700 and #1850) collected during Exp. 338 and of all samples obtained during the 1-year-later Exp. 348 are less variable (1.74–2.46 Ra with a mean 3He/4He ratio of ~ 2.4 Ra) and no radon anomalies were observed during sampling. For these samples, we assume migration by diffusive flow of helium-bearing fluids through sediments of the accretionary prism. In contrast, elevated radon activities and the more variable helium isotopic composition of fluids from 950, 1400, and 1800 mbsf from Exp. 338 are better explained by channelized and active fluid flow through temporarily permeable strata, maybe as a short-term episodic flow event caused by reactivation of buried trust faults. The helium isotopic composition of #950 is in good agreement with estimated helium isotope values of the subducting Philippine Sea Plate (PSP) at present (~ 3.4 Ra), whereas fluids from 1400 and 1800 mbsf demonstrate the input of radiogenic helium from a crustal, probably terrestrial source.
- Helium isotopes
- Fluid flow
- Nankai Trough
- Integrated Ocean Drilling Program
Recent 3-D seismic reflection surveys report the presence of several normal faults cutting through the forearc basin (Moore et al. 2009, 2015; Kinoshita et al. 2018), which could serve as possible migration pathways for aqueous fluids and dissolved and free gases. Common fluid migration features at convergent margins, particularly in the Kumano forearc basin, are mud volcanoes, through which fluids and gases are expelled to the hydro- and atmosphere. Mud volcanoes can serve as “tectonic windows” to processes operating at greater depths (e.g. Kopf 2002), where the presence of gases significantly enhances mud mobilization. Gas samples taken from mud volcanoes in the Kumano forearc basin showed a clear thermogenic signal (δ13C ≥ − 40‰ PDB). The overall TOC values of hemipelagic mudstones in the Kumano forearc basin are low, but cutting samples from C0009 (Unit III), located ~ 20 km northwest of Site C0002, are partly enriched in organic material (Doan et al. 2011; Wiersberg et al. 2015). However, formation temperatures and the maturity of the organic material (wood, lignite) are too low to generate significant amounts of thermogenic methane (Wiersberg et al. 2015); it is therefore believed that thermogenic methane from mud volcanos derives from old accreted sediments underlying the basin sediments (Pape et al. 2014). Further landward in the Kumano Basin at IODP Site C0009, the molecular composition of hydrocarbons and the carbon isotope composition of methane (δ13C ~ − 66‰ PDB) in drilling mud gas indicate the presence of microbial methane with only little evidence for mixing with thermogenic hydrocarbons (Wiersberg et al. 2015), making upward migration of deep-sourced gases at this site unlikely.
Drilling mud gas monitoring and sampling at IODP Site C0002 at the southern rim of the Kumano forearc basin revealed the overall dominance of microbial methane to depths down to 1700 mbsf (Hammerschmidt et al. 2014) with increasing contribution of thermogenic gas at greater depth. Estimated formation temperatures at 1700 mbsf, based on long-term temperature monitoring at C0002 (Sugihara et al. 2014), fall between 65 and 70 °C, depending on the assumed thermal conductivity. Although this temperature range marks also the beginning of thermogenic gas generation (Whiticar 1994), the low TOC content at depths below 1700 mbsf at Site C0002 (Tobin et al., 2015) makes significant in situ generation of hydrocarbons by thermal degradation of organic matter little likely. Indeed, we favour migration of thermogenic gas from deeper sources and mixing with shallow bacterial hydrocarbon gas. Evidence for migration of deeper fluids in the Nankai Trough subduction zone is also provided by lithium, iodine and boron isotopes studies (Nishio et al. 2015, Tomaru and Fehn 2014, Hüpers et al. 2016). Unusual light 7Li/6Li ratios in fluids recovered from a Kumano mud volcano (Nishio et al. 2015) are in line with estimated temperatures of up to 310 °C, indicating a deep lithium-bearing fluid source. Iodine ages of pore water samples from C0002 at depths as deep as 984 mbsf are significantly older than ages of the host sediments, iodine must thus have been transported from deeper formations older than 25 Ma (Tomaru and Fehn 2014). Boron concentration and isotope data from silt and sand layers (Hüpers et al. 2016) of the underthrust section of the downgoing plate at Nankai favour fluid flow in seaward direction from depths equivalent to the temperature range of 60 °C to 150 °C.
Noble gas isotopes like 222Rn, 3He and 4He are useful tools to distinguish between active fluid flow through permeable strata and trapping of pore fluids in pore space. 222Rn and 4He are products of the radioactive decay of the parent elements uranium (U) respectively uranium plus thorium (U + Th), while 3He is mainly primordial and associated with mantle-derived fluids. Helium and to a greater extend radon are soluble in water and can be easily transported by active fluid flow. However, while both helium isotopes 3He and 4He are stable, all radon isotopes are subject to further radioactive decay. The most stable isotope of radon, 222Rn, has a half-life of 3.8 days, and contrary to He, 222Rn is characterized by a low diffusivity. Consequently, high concentrations of He and low concentrations of 222Rn suggest high porosity and low permeability, whereas high concentrations of 222Rn and He point to rapid fluid flow. High permeability can be further identified using the 3He/4He isotope ratio (e.g. Aquilina et al. 1998; Kennedy et al. 1997; Wiersberg and Erzinger 2007, 2011; Burnard et al. 2012), which can even indicate active crustal deformation and enhancement in local permeability (Kennedy and van Soest 2007). Aquilina et al. (1998) found 3He/4He ratios of ~ 0.3 Ra in drilling mud gas samples from a borehole that penetrates Triassic sandstones of the northeastern edge of the SE Basin of France. The authors suggest mantle fluid flow from a deeper source into the investigated Triassic reservoirs. The source of mantle fluids is probably related to the rise of the mantle in the Alpine zones and Rhodanian corridor. Kennedy (1997) and Wiersberg and Erzinger (2007, 2011) investigated surface respectively borehole fluids from the SAF. In the absence of recent magmatism around the sampling spots at the SAF, the elevated helium isotope ratios reported in these studies indicate enhanced crustal permeability, promoting fault-controlled advective mantle fluid flow through the brittle-ductile barrier to the surface. The wide spatial distribution of mantle fluids in the SA Fault Zone could be explained by injection of mantle fluids from fluid-bearing faults into the country rock, followed by diffusion. Significant variations in helium isotope compositions on short spatial scale are reported from the San Andreas Fault at seismogenic depths (Wiersberg and Erzinger 2011) and were interpreted as episodic and channelized fluid. Kennedy and van Soest (2007) investigated helium isotopes in surface fluids from the northern Basin and Range Province in the western USA. Helium isotope trends correlate with rates of crustal deformation, caused by the motion of the North American relative to the Pacific Plate, where highest 3He/4He ratios coincide with greatest extension and shear strain.
Helium isotopes are typically reported as 3He/4He ratio and denoted in atmospheric ratios (Ra, (3He/4He)air ≡ 1.388 × 10− 6 ≡ 1 Ra). A helium isotope composition of ~ 0.02 Ra is typical for fluids from crustal sources (Mamyrin and Tolstikhin 1984), whereas ratios of > 1 Ra demonstrate the presence of helium from primordial (i.e. mantle) He sources (Clark et al. 1969).
3He/4He isotope ratios have been reported from plate margins worldwide, e.g. from the Indonesian archipelango (Hilton and Craig 1989), circum-pacific volcanic arcs (Poreda and Craig 1989), the Indian Ocean Ridge (Moreira et al. 2003), from mud volcanoes at the Caucasian continental collision zone (Kopf et al. 2003) and the Congo-Angola margin (Chaduteau et al. 2009) and the eastern and western Pacific Ocean (Chavrit et al. 2016). Hilton et al. (2002) provide a summary of helium isotope variations in arc-related geothermal and volcanic fluids worldwide. In southwest Japan, He isotope ratios from the back-arc region show values similar to the mean ratio of 5.4 ± 1.9 Ra for arc-related volcanism (Hilton et al. 2002). At the Kii Peninsula, 3He/4He ratios are between 1 and 5.4 Ra and show a spatial distribution approximately parallel to the Nankai Trough itself, explained by the upward flow of mantle volatiles originating from the mantle wedge overlying the subducting Philippine Sea Plate (PSP), or from the hydrated mantle of the subducting slab (Wakita et al. 1987, Matsumoto et al. 2003, Doğan et al. 2006, Umeda et al. 2006a, 2006b, 2007a, 2007b, 2012, Sano and Nakajima 2008, Sano et al., 2009). In the forearc region, He isotope ratios are generally lower. Umeda et al. (2012) calculated a helium isotope composition of ≤ 3.4 Ra for the subducting PSP at the present time, considering the subduction of oceanic lithosphere of mid-Miocene age which has undergone altering of the original helium isotope composition (8 Ra) by helium diffusive lost and post-intrusive ingrowth of radiogenic 4He from U and Th decay in the tholeiite basalts (Sano and Nakajima 2008).
Here we report results from helium isotope ratios (3He/4He) from 12 drilling mud gas samples taken during IODP Expeditions 338 and 348 (Strasser et al. 2014a, 2014b, 2014c; Expedition 348 Scientists and Scientific Participants 2014; Tobin et al. 2015). During both expeditions, riser drilling was conducted in the Kumano forearc basin, southeast offshore the Kii Peninsula (Site C0002; Fig. 1). The drilling operation commenced in Kumano Basin sediments at around 850 mbsf and stopped at around 3050 mbsf in the accretionary prism. The entire interval was subjected to drilling mud gas monitoring and sampling during riser drilling. We explore possible contributions of mantle-derived and crustal helium in the depth interval 950–3050 mbsf and discuss our findings in the context of fluid migration through the accretionary prism. Our data also provide a seaward extension of previously compiled He isotope ratio dataset for southeast Japan (Umeda et al. 2012).
The Nankai Trough, located southeast of the eastern coast of southern Japan, was formed mainly during the Oligocene-Miocene period by a complex subduction-accretion process that probably included migration of a triple junction (Kimura et al. 2014; Underwood 2018). The northwest directed subduction of the PSP beneath the Eurasian Plate initiated around ~ 15 Ma, temporarily ceased at ~ 12 Ma and restarted at ~ 6 Ma (e.g. Taira 2001; Kimura et al. 2014), forming the Kumano forearc basin (Hayman et al. 2012) and resulting in today’s subduction rates of ca. 4.1–6.5 cm/year (Seno et al. 1993; Miyazaki and Heki 2001). A major splay fault (Megasplay fault) within an out-of-sequence-thrust (OOST) fault system separates the inner from the outer accretionary prism overlying the seismogenic and aseismic part of the thrust fault boundary, respectively (Wang and Hu 2006). The Megasplay fault system is suggested to be hydraulically connected to the thrust fault boundary (e.g. Tobin and Saffer 2009). Splay fault activity in the accretionary prism significantly promoted sedimentation in the Kumano forearc basin at around 1.67–1.56 Ma (Strasser et al. 2009).
Site C0002 is situated at the southern rim of the Kumano forearc basin, in the so-called “forearc basin zone” (Moore et al. 2009, 2013; Ashi et al. 2009; Kopf et al. 2011). Based on coring and logging data, the Expedition 315 Scientists (2009, Hole C0002B), Strasser et al. (2014c, Holes C0002F, H, J, K, L) and the Expedition 348 Scientists (2014, Holes C0002N, P) recognized five different lithological units in the southern part of the Kumano forearc basin at Site C0002. Unit I (down to 474 mbsf), Unit II (475–875.5 mbsf in Hole C0002M), Unit III (875.5–975.5 mbsf in Hole C0002N), Unit IV (975.5–1665.5 mbsf in Hole C0002N) and Unit V (1665.5–2325.5 mbsf in Hole C0002N and 1965.5–3058.5 mbsf in Hole C0002P).
Unit I is comprised of mud of clayey silt to silty clay, in which foraminifers are abundant. Unit II is also dominated by mud (clayey silt to silty clay), with silty to sandy interbeds. Unit II is generally coarser than Unit I and is interpreted to consist of distal basin deposits (Expedition 315 Scientists 2009). Unit III comprises basal forearc basin sediments, which are characterized by silty claystone with abundant occurrence of calcareous nannofossils and dewatering structures as well as scattered bioturbation and glauconite-rich zones (Expedition 315 Scientists 2009). Unit IV is interpreted to be the upper accretionary prism, based on a remarkable increase in interbedding of mud-, silt- and sandstone in an otherwise mudstone-dominated interval. Unit IV is further characterized by a decrease in calcareous nannofossils and intense tectonic deformation. Between 1665 mbsf and 1701 mbsf, the lithology becomes predominantly silty claystone, which defines the top boundary Unit V.
In hole C0002B (Exp 315), faults were clustering in two intervals from 920 to 950 mbsf and from 1000 to 1050 mbsf. These two fault clusters display the greatest range in dip as well as the highest dip magnitude (i.e. 90° at 920 mbsf) of all of the faults at this site. The upper cluster of faults is just below the top of Unit IV, although a few faults are also present above the boundary. Expedition 315 Scientists interpreted the upper cluster as a system of out-of-sequence (splay) faults and a significant unconformity at ~ 922 mbsf as a manifestation of uplift along these faults that occurred at ~ 5 Ma (Expedition 315 Scientists 2009). In Hole C0002P, the Unit V top and bottom boundaries are located at 1965.5 and 3058.5 mbsf, respectively; therefore, the top boundary is 300 m deeper than in Hole C0002B. Based on calcareous nannofossil assemblages, Unit V is most likely of Miocene age. The cored interval within Unit V (2163–2219 mbsf) revealed a prominent fault zone at 2205–2206 mbsf.
Formation ages and the QMS gas composition data from 12 drilling mud gas samples from IODP Expeditions 338 and 348 covering the depth range 950–3050 mbsf. Analytical errors are ± 20% for helium and ± 5% for all other gases. Formation ages from nannofossils, C0002F: Strasser et al. 2014c; C0002N/P: Tobin et al., 2014
Sample # [mbsf]
Formation age [Ma]a
A suite of 12 drilling mud gas samples was collected during IODP Expedition 338 between October 2012 and January 2013 and Expedition 348 between September 2013 and January 2014 for noble gas isotope analysis. Samples from Expedition 338 were taken during riser drilling of Hole C0002F (875.5–2005.6 mbsf), while samples from Expedition 348 were obtained from Hole C0002N (875.5–2325.5 mbsf) and C0002P (1965.5–3058.5 mbsf). In total, the samples cover a depth range from 950 to 3050 mbsf. The lateral distance between Hole C0002F and C0002N is 16 m, and 39 m between Hole C0002N and Hole C0002P. Holes C0002F and C0002P are 55 m apart.
222Rn decay was monitored in drilling mud gas during drilling of Holes C0002F, C0002N and C0002P with a 650-mL ion-counting chamber in sampling intervals of 10 min, a sensitivity of 100 Bq/m3 and a concentration range between 2 and 2 × 106 Bq/m3 (Strasser et al. 2014b; Expedition 348 Scientists and Scientific Participants 2014).
Gas samples for noble gas analysis were taken from the gas line after gas extraction from the circulating drilling mud. All sampling times and corresponding sample depths were corrected for lag time, i.e. the time the formation gas needs to travel from the bottom of the borehole to the gas-monitoring instruments. The drilling mud gas-monitoring method is reported by Erzinger et al. (2006). The drilling mud gas-monitoring system onboard D/V Chikyu is described in detail in Hammerschmidt (2014). It should be noted that drilling mud is open to air at the mud tanks; hence, a significant portion of the gas extracted from the circulating drilling mud derives from the atmosphere. The gas samples were collected in glass cylinders equipped with two stopcocks following a method described by Hilton et al. (2002).
To avoid significant helium loss from the sample cylinders during sample storage by diffusion, noble gas isotope analysis was conducted within 4 months after sample arrival in the noble gas laboratory. Prior to noble gas isotope analysis, the samples were analysed with a quadrupole mass spectrometer for He, N2, O2, CH4, CO2 and Ar with detection limits of 1 ppm by volume (ppmv) for He, CH4 and Ar, as well as 10 ppmv for O2, N2 and CO2 to prove sample integrity and identify possible diffusion loss and additional air contamination (Table 1).
Noble gas isotope analysis was conducted in the noble gas laboratory of the German Research Centre for Geosciences (GFZ). The determination of noble gas concentrations and isotopic compositions follow protocols described in detail by Niedermann et al. (1997). Here, we present a short summary of the analytical procedure that comprises gas inlet, purification, mass spectrometric analysis and data processing.
The procedure for noble gas isotope analyses includes purification, a mass spectrometric analysis using a VG 5400 mass spectrometer and data processing (see Niedermann et al. (1997) for a comprehensive explanation and statistical evaluation of the procedure). An aliquot with a predefined volume is introduced in the system under a constant pressure. The gas split is transferred to the purification line, where vaporized water is extracted by a dry-ice cooled cold trap. Removal of nitrogen, oxygen and carbon dioxide is accomplished by passing the sample to two titanium sponge getters, which are heated to ca. 1024 K and 674 K, respectively. The setup also comprises two Zr-Al getters, which extract hydrogen, hydrocarbons and remaining carbon dioxide. Prior to the helium and neon analyses, argon, krypton and xenon are separated from the gas phase by two nitrogen-cooled charcoal fingers.
The remaining gas is transferred to two cryogenic cold heads that have temperatures of 50 K and 11 K, respectively. The former allows adsorption of remaining argon, krypton and xenon. Helium and neon are collected with the second cold head. Temperature-controlled release is used to determine noble gas concentrations. For He, the second cryogenic cold head is heated to 35 K, which is followed by a step-wise increase in temperature of the first cold head to measure argon (80 K), krypton (100 K) and xenon (190 K). Afterwards, Ne is released by heating the second cold head to 120 K. For He and Ne measurements, background concentrations of argon and hydrocarbons were suppressed by a stainless steel frit and an activated charcoal finger that was cooled with liquid nitrogen.
The measurements in this study were corrected for initial (“blank”) gas concentrations and influences of atmospheric gas following Niedermann et al. (1997, and references therein. Concentrations of the blanks (in cm3 STP) were typically: 4He ~ 5 × 10− 12, 20Ne ~ 0.5 × 10− 12, 40Ar ~ 5 × 10− 10, 84Kr ~ 0.05 × 10− 12 and 132Xe ~ 0.02 × 10− 12 (Niedermann et al. 1997; Wiersberg et al. 2011). These concentrations were all well below the concentrations in the samples; therefore, a blank correction was not necessary. The influence of isobaric interferences is minimized by correlating the mass spectrometer background values with the efficiency for double-charged ion production (Niedermann et al. 1997).
Shipboard results, including 222Rn, are comprehensively outlined in Strasser et al. (2014c) and Expedition 348 Scientists and Scientific Participants (2014). Here, the main findings will be briefly reviewed. At C0002F, 222Rn was peaking around 950 mbsf, 1100 mbsf, 1400 mbsf and 1800 mbsf, which can be interpreted as active fluid inflow (see, e.g. Aquilina et al. 1998) into the borehole. Gas samples from 950, 1400 and 1800 mbsf also show atypical 3He/4He isotope ratios (from 1100 mbsf, we do not have a gas sample). Surprisingly, during re-drilling this interval in Hole C0002N, the concentrations of 222Rn remained low (below 100 Bq/m3) but show maximum activities (≤ 200 Bq/m3) between 2050 and 2100 mbsf and below 2210 mbsf. For the depth interval 1965.5–2325 mbsf, which was penetrated by both holes, C0002N and C0002P, radon measurements show much higher activity for C0002P, albeit no significant radon peaks between 2050 and 2100 mbsf and below 2210 mbsf, as it was the case for C0002N. C0002P displays a general trend of increasing radon activity down to ~ 2500 mbsf with local maxima at ~ 2090 and 2160 mbsf. Below ~ 2500 mbsf, radon activities in C0002P, albeit showing some variations, are relatively constant with ~ 250 Bq/m3.
Noble gas nuclide abundances (4He, 20Ne, 40Ar, 84Kr and 132Xe), isotope ratios (3He/4He, 20Ne/22Ne, 21Ne/22Ne, 40Ar/36Ar, and 38Ar/36Ar), nuclide ratios (4He/20Ne and 3He/20Ne), air-corrected 3He/4He ratios and the relative proportions of atmospheric, crustal and mantle helium from 12 drilling mud gas samples covering the depth range 950–3050 mbsf from site C0002
Sample # [mbsf]
Crustal He (%)
Mantle He (%)
0.00515 ± 0.00026
0.01367 ± 0.00068
7.75 ± 0.39
0.000544 ± 0.000027
0.0000229 ± 0.0000014
1.348 ± 0.041
9.798 ± 0.010
0.02896 ± 0.00024
296.9 ± 1.6
0.18707 ± 0.00094
0.3770 ± 0.0029
7.05E−07 ± 2.2E−08
3.26 ± 0.28
0.00531 ± 0.00027
0.01446 ± 0.00072
7.47 ± 0.37
0.000495 ± 0.000025
0.0000185 ± 0.0000013
1.044 ± 0.045
9.8331 ± 0.0088
0.02900 ± 0.00025
294.7 ± 1.4
0.1882 ± 0.0012
0.3675 ± 0.0029
5.33E−07 ± 2.3E−08
1.33 ± 0.34
0.00539 ± 0.00027
0.01559 ± 0.00078
8.43 ± 0.42
0.000557 ± 0.000028
0.0000210 ± 0.0000015
1.114 ± 0.037
9.832 ± 0.010
0.02900 ± 0.00025
294.8 ± 1.3
0.1878 ± 0.0011
0.3460 ± 0.0027
5.35E−07 ± 1.8E−08
2.46 ± 0.49
0.00553 ± 0.00028
0.01482 ± 0.00074
8.07 ± 0.40
0.000552 ± 0.000029
0.0000215 ± 0.0000015
0.919 ± 0.034
9.8109 ± 0.0090
0.02896 ± 0.00043
0.3731 ± 0.0029
4.76E−07 ± 1.8E−08
0.44 ± 0.24
0.00538 ± 0.00027
0.01617 ± 0.00081
9.03 ± 0.45
0.000643 ± 0.000033
0.0000233 ± 0.0000015
1.067 ± 0.031
9.7926 ± 0.0082
0.02894 ± 0.00024
296.6 ± 1.4
0.1884 ± 0.0011
0.3330 ± 0.0026
4.93E−07 ± 1.5E−08
2.59 ± 0.79
0.00614 ± 0.00031
0.01870 ± 0.00093
10.78 ± 0.54
0.000761 ± 0.000038
0.0000309 ± 0.0000019
1.034 ± 0.046
9.7930 ± 0.0089
0.02895 ± 0.00027
295.9 ± 1.3
0.1884 ± 0.0011
0.3304 ± 0.0026
4.74E−07 ± 2.1E−08
1.99 ± 1.35
0.00632 ± 0.00032
0.01900 ± 0.00095
10.33 ± 0.52
0.000718 ± 0.000036
0.0000305 ± 0.0000064
1.054 ± 0.045
9.7977 ± 0.0089
0.02897 ± 0.00027
297.5 ± 1.4
0.1884 ± 0.0013
0.3345 ± 0.0027
4.89E−07 ± 2.1E−08
2.17 ± 0.99
0.00608 ± 0.00030
0.01769 ± 0.00088
9.93 ± 0.50
0.000717 ± 0.000036
0.0000264 ± 0.0000018
1.100 ± 0.036
9.7904 ± 0.0087
0.02897 ± 0.00028
295.2 ± 1.4
0.1882 ± 0.0011
0.3457 ± 0.0027
5.28E−07 ± 1.8E−08
2.29 ± 0.48
0.00627 ± 0.00031
0.01889 ± 0.00094
10.79 ± 0.54
0.000750 ± 0.000038
0.0000275 ± 0.0000057
1.033 ± 0.035
9.8013 ± 0.0089
0.02900 ± 0.00027
296.6 ± 1.5
0.1883 ± 0.0012
0.3338 ± 0.0027
4.79E−07 ± 1.7E−08
1.74 ± 0.80
0.00672 ± 0.00034
0.01977 ± 0.00099
11.24 ± 0.56
0.000794 ± 0.000040
0.0000288 ± 0.0000060
1.090 ± 0.034
9.7987 ± 0.0090
0.02897 ± 0.00027
295.9 ± 1.3
0.1883 ± 0.0011
0.3421 ± 0.0027
5.18E−07 ± 1.7E−08
2.33 ± 0.52
0.00800 ± 0.00040
0.01610 ± 0.00081
9.48 ± 0.47
0.000674 ± 0.000034
0.0000243 ± 0.0000050
1.522 ± 0.039
9.798 ± 0.017
0.02899 ± 0.00028
296.4 ± 1.6
0.1884 ± 0.0013
0.5000 ± 0.0040
1.056E−06 ± 2.8E−08
2.44 ± 0.11
0.00655 ± 0.00033
0.01952 ± 0.00098
10.98 ± 0.55
0.000763 ± 0.000039
0.0000307 ± 0.0000063
1.048 ± 0.030
9.7966 ± 0.0092
0.02897 ± 0.00027
296.3 ± 1.6
0.1886 ± 0.0010
0.3375 ± 0.0027
4.91E−07 ± 1.5E−08
1.88 ± 0.56
Abundances of the noble gas nuclides 4He, 20Ne, 40Ar, 84Kr and 132Xe are denoted in millibar (mbar). For 20Ne, 40Ar, 84Kr and 132Xe, some samples show abundances higher than air, while others are lower, with a general trend of increasing nuclide concentrations with depth. Gas samples with noble gas nuclide abundances higher than air show oxygen concentration in the gas phase lower than the atmosphere, probably due to chemical consumption of oxygen during the drilling process. In turn, gas samples with noble gas abundances lower than air contain additional formation gases (methane), which reduces the noble gas abundances. However, for all samples, the 20Ne normalized noble gas nuclide abundance (X/20Ne) are atmospheric for 40Ar, 84Kr and 132Xe. In contrast, 3He/20Ne and 4He/20Ne ratios are higher than atmospheric for all samples, indicating the presence of helium-bearing formation fluids.
Three samples from Exp 338 (#950, #1400 and #1800) show enhanced and rather uniform 4He/20Ne ratios (~ 0.37), compared to the other samples (< 0.35). These three samples derive from depths, which also show elevated radon activity. From these samples, #950 is also enriched in 3He (3He/20Ne = 7.05 ± 0.22 × 10− 7), while all other samples have 3He/20Ne ratios of ~ 5 × 10− 7.
Irrespective of the expedition on which the samples were taken, the air-corrected 3He/4He ratios are within 2σ uncertainty rather uniform at depths below 1850 mbsf. Samples from Exp 338 obtained between 950 and 1850 mbsf are more variable. The air-corrected helium isotope ratio declines from 2.46 ± 0.49 at 1700 mbsf down to 0.44 ± 0.24 at 1800 mbsf and then increases to 2.59 ± 0.79 at 1850 mbsf. While samples #1700 and #1850 are, within analytical uncertainties, indistinguishable from the mean 3He/4He ratio (~ 2.40 Ra), the ratio for #1800 is significantly lower.
In this section, we want to relate the results from drilling mud gas analysis to fluid migration processes in the Nankai Trough accretionary prism. Except for samples from 950, 1400 and 1800 mbsf, collected from hole C0002F during Exp 338, all samples from the depth interval from 1700 to 3050 mbsf demonstrate, within a 2σ error, similar air-corrected helium isotope compositions with mean 3He/4He values of ~ 2.4 Ra. As the helium isotope composition from nearby samples can be as low as 0.44 ± 0.24 Ra (#1800), we suggest that the relatively constant 3He/4He ratios for #1700, #1850, and all samples from Exp 348 (1.74–2.59 Ra) were not significantly influenced by in situ radiogenic 4He from radioactive decay of U and/or Th to the observed helium isotope ratios. Higher and more variable U and Th concentrations would alter the helium isotope composition towards lower, more crustal values ((3He/4He)crust ~ 0.02 Ra, Mamyrin and Tolstikhin 1984), as it applies for #1400 and #1800.
The overall 222Rn activity in the depth interval 1700–3050 mbsf was relatively high during drilling of the C0002P borehole (~ 300 Bq/m3) but does not show significant variations with depth, similar to the helium isotopes. The consistently high 222Rn activity at site C0002P could be an artifact from constant inflow of radon-rich fluids from another nearby source into the open hole section during drilling, because the samples from #1700 and #1850 mbsf from C0002F have low radon activity (~ 100 Bq/m3) but similar, albeit somewhat higher air-corrected 3He/4He ratios (2.46 ± 0.49 and 2.59 ± 0.39 Ra), compared to samples from Exp 348. Based on rather constant air-corrected helium isotope composition (1.74–2.59 Ra with a mean ratio of ~ 2.4 Ra) with no radon anomalies and little helium excess, we assume diffusive migration of fluids containing a mantle helium component through pore space along mineral grain boundaries. Nevertheless, the (3He/4He)air-corr. in this depth interval is lower than for sample #950 mbsf (3.3 Ra). If we assume that the helium isotope composition of #950 mbsf is close to the actual values of the subducting PSP in southwest Japan (Umeda et al. 2012) and mantle helium in the interval 3050–1700 mbsf derives from the same source, then admixing of crustal helium must have occurred at depths between ~ 9 kmbsf (depth of the subducting PSP, Strasser et al. 2014c), and 3050 mbsf (C0002P borehole depth) to yield a mean helium isotope ratio of ~ 2.4 Ra. Admixing with crustal helium is obvious for samples #1400 and #1800 with 3He/4He ratios of 0.44 ± 0.24 and 1.33 ± 0.34, resp.).
With given age and known concentrations of uranium, thorium, 3He and 4He, the 3He/4He ratio of subducting PSP can be calculated. Umeda et al. (2006a) assume high 3He (5 × 10− 11 cm3/g STP), uranium (2.21 ppm) and thorium (5.03 ppm) initial concentrations in magma related to Neogene volcanism occurring 14 Ma ago to explain 3He/4He ratios ≤ 2.5 Ra in hot springs on Shikoku Island. Their calculation yields a 3He/4He ratio of ~ 3.4 Ra for the subducting PSP at present. Sano and Nakajima (2008) use concentration values two order of magnitudes lower as basis for their calculation of the 3He/4He ratio of the subducting PSP (3He = 7 × 10− 13 cm3/g STP, U = 0.09 ppm) and thorium (0.17 ppm), assuming an age of 20 Ma for the slab at the trench and an uncertainty of factor 3 for the 3He concentration. Their calculation, however, yields the same 3He/4He ratio of ~ 3.4 Ra.
An age of 20 Ma is in agreement with the findings of Okino et al. (1994), verified by coring at Site C0012 (Underwood et al. 2010). However, after 20 Ma, significant helium diffusion losses from oceanic crust should have occurred. Also, the high uranium and thorium concentrations reported by Umeda et al. (2006a) and local enrichments of U in the upper part of the accretionary prism reported for interstitial waters sampled at Site C0002 (Expedition 315 Scientists 2009; Strasser et al. 2014b; Expedition 348 Scientists and Scientific Participants 2014) indicate crustal input. We therefore favour the helium input data from Sano and Nakajima and the uranium and thorium concentrations of clay-rich deep-sea sediments (Turekian and Wedepohl 1961) for further calculations. The upward fluid flow rate q can then be estimated according to Kennedy et al. 1997 with
where Hcr is the thickness of the crust from the bottom of hole C0002 down to the subducting PSP as source of the mantle fluids (approx. 6 km, Moore et al. 2015), ρS = 2.6 cm3/g is the density of the sediments, ρf = 1.025 cm3/g is the fluid density, [4He]f,ma is the concentration of helium in the subducting Philippine Plate = 1.5 × 10− 7 cm3/g [STP] (Sano and Nakajima 2008). (R/Ra)meas, crust, mantle is, relative to the atmospheric ratio, the measured 3He/4He ratio (2.4 Ra), the average helium production ratio in the crust (~ 0.02 Ra, Ballentine and Burnard 2002) and the helium isotope ratio of subducting Philippine Sea Plate (~ 3.4 Ra, Umeda et al. 2012). P (He) is the annual radiogenic production and depends on the concentrations of the parent element nuclides (U, Th). P(He) can be calculated according to Craig and Lupton (1976) as.
P(He) = 0.2355 × 10− 12 × U (1 + 0.123(Th/U − 4)).
Parent element concentrations of U = 1.2 ppm and Th = 7 ppm for the accretionary prism (Turekian and Wedepohl 1961) results in an annual radiogenic production P (He) of 3.46 × 10− 13 cm3/g [STP] and a resulting flow rate q of ~ 7 cm/a. Assuming that instead of vertical flow the fluids would migrate along faults, fractures and bedding planes with a dipping angle of 60°, the calculated flow rate would change to ~ 10 cm/a and to 9 cm/a at a 75° dipping angle, respectively. Given these uncertainties and the not well-constrained helium concentration and helium isotope ratio of the subducting PSP, we suggest a fluid flow on the centimeter scale per year, which is in good agreement with fluid flow calculations in the Nankai Trough based on chlorine measurements (Spivack et al. 2002).
With an estimated fluid flow in the range of 1–10 cm per year, it would take ~ 10–100 ka for fluids to travel 6 km from the subducting PSP at 9-km depth through the accretionary prism to reach the hole bottom depth of C0002P (3050 mbsf). During this time, helium with an isotopic composition (3He/4He) of 3.4 Ra would alter to 3.3–2.8 Ra. This finding underlines that additional input of crustal helium is required to yield the 3He/4He ratio found in most samples of our study.
Based on the distribution of gas hydrates in the Nankai Trough, Baba and Yamada (2004) and Yamada et al. (2013) described two mechanisms of fluid migration in accretionary prisms: diffusive fluid flow through intra-granular pore spaces and advective fluid flow through permeable faults. In the deeper part of the prism, fluids expelled by the overburden pressure mainly flow through faults, while diffusive flow is lower in the deeper parts due to lower porosity, and less susceptible to fluctuations. At shallower depths, diffusion is the leading process of fluid migration, leading to a widespread distribution of gas hydrates within the Nankai Trough. According to Yamada et al. (2013), fluid flow in accretionary prisms is also subject to spatial and temporal variations, mainly as a function of faulting and changes in stress field. Possible mechanisms that could be involved here are, e.g. hydrofracturing of low-permeable strata, caused by reduction of pore space during deformation at accretionary prisms (Behrmann 1991) and subsequent increase in pore fluid pressure. Numerical models and analog experiments suggested that fluid flow along the thrust faults at the prism toe is generally active, but in periods of inactivity, older, otherwise inactive, thrust faults more landward in the prism are re-activated.
Arc-related volcanism and associated geothermal fluids show generally somewhat lower helium isotope ratios than the canonical 8 Ra for MORB due to possible contamination with crustal fluids during fluid or magma ascent. Hilton et al. 2002 calculated a mean 3He/4He ratio of 5.4 ± 1.9 Ra for fluids from arc-related volcanism worldwide. 3He/4He ratios in agreement with these values were, e.g. observed in samples from hot springs and water wells in the Kinki district (Sano et al. 2009) and in southwest Japan (Chuguko region, Umeda et al. 2012). Supported by seismic tomography and magnetotelluric investigations, which identified a large low-velocity and conductive zone extending from the upper mantle to the middle crust, Umeda et al. (2012) interpreted the high 3He/4He ratios in southwest Japan close to the volcanic front with upward migration of mantle fluids from an upwelling astenospheric body. For the Kinki district, where high helium isotope ratios were found up to 200 km away from the volcanic front, Sano et al. (2009) suggest fluid or magma rise from an extinct and subducted mid-ocean ridge.
In contrast, medium Ra values (~ 2–4 Ra) in the southwest Japan forearc region were explained by fluid release from the young PSP slab (Sano et al. 2009; Umeda et al. 2012), maybe with additional contribution of crustal fluids. Such medium Ra values are in good agreement with our dataset. Fluid migration from the slab could explain the occurrence of deep non-volcanic tremors in the region. Also the lack of Quaternary volcanism makes a significant contribution of fluids from the asthenosphere to the total fluid budget at site C0002 little likely. We interpret the 3He/4He ratios measured in C0002 mud gas samples as a mixture of air, introduced by the downward pumped drilling mud, crustal helium and mantle helium released from the subducting PSP.
Helium isotope and radon data from 12 drilling mud gas samples obtained between 950 and 3050 mbsf during IODP Expeditions 338 and 348 at the Kumano forearc basin in SW Japan suggest diffusive fluid flow along mineral grain boundaries through the accretionary prism for all samples from Exp 348 and for two of five samples (#1700, #1850) from Exp 338. Radon and helium isotope data of three samples from Exp 338 (#950, #1400, #1800) indicate channelized fluid flow, by which helium from 950 mbsf exhibits a 3He/4He ratio (3.3 Ra) close to the calculated helium isotope ratio of the subducting Philippine Sea Plate (~ 3.4 Ra). Two samples (#1400 and #1800 mbsf) indicate admixing of crustal helium from a nearby source enriched in uranium and thorium. We suggest that elevated fluid flow caused the observed helium and radon signals of these three samples, according to the fluid flow model from Yamada et al. 2013. Application of the fluid velocity model from Kennedy et al. (1997) results in average fluid velocities in the range of centimeters per year in the accretionary prism of the Kumano Basin.
We want to thank Sean Toczko, Lena Maeda, Yusuke Kubo, Nobu Eguchi, Tomohiro Toki, and the whole crew onboard D/V Chikyu for their excellent support during IODP Expeditions 338 and 348. ECORD, IODP Germany and the IODP Priority Program of the German Research Foundation (DFG SPP 527) are greatly acknowledged for funding. The people in charge of noble gas laboratory of the GFZ German Research Centre for Geosciences, namely Enzio Schnabel and Samuel Niedermann, were of tremendous help in conducting the noble gas analyses. Editor Michael Underwood and two anonymous referees provided helpful and constructive reviews.
ECORD, IODP Germany and the IODP Priority Program of the German Research Foundation (DFG SPP 527) are greatly acknowledged for funding.
JE, AK, SH and TW proposed the topic and conceived and designed the study. SH and SF carried out the offshore measurements and SH and TW the onshore measurements. TW and SH analysed and interpreted the data. All authors collaborated with the corresponding author in the construction of the manuscript. All authors read and approved the final manuscript.
The authors declare that they have no competing interest.
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