宮下 敦

The Kitomyo Schist from Kurosegawa Belt, Shikoku, has been long considered as the oldest records of subduction metamorphism in Japan, based on an early 1970s K-Ar dating of white mica. The schist consists of mafic and pelitic layers and occurs as a tectonic block within serpentinite. Reappraisal of the schist confirmed the schist is characterized by an epidote-amphibolite peak metamorphic facies. The mafic portion is characterized by zoned amphibole + epidote + chlorite + titanite phengite +/- rutile. The presences of relict rutile surrounded by titanite and the barroisitic cores of zoned amphibole suggest a high-pressure intermediate type metamorphism at the metamorphic peak (P = -0.8-1.5 GPa and T = -500-570 degrees C). The presence of Mn-rich garnet and the lack of biotite, oligoclase and paragonite also support high-pressure intermediate type metamorphism that eliminate the possibility of a typical blueschist-facies metamorphism. New SHRIMP and LA-ICPMS zircon U-Pb geochronology on a pelitic sample show detrital grains of Mesoproterozoic and Early Paleozoic ages, suggesting a maximum deposition age for the trench-fill sediment of -440 Ma. Also the U-Pb data confirmed-360 Ma overgrown rims that might have formed during the subduction zone epidote-amphibolite facies metamorphism. Reappraisal revealed that the Kitomyo Schist is not the oldest high-pressure type schist in Japan and rather comparable to the Late Paleozoic Renge Metamorphic Rocks and their equivalents in the Kurosegawa Belt. The Devono-Carboniferous high-pressure metamorphic rocks in Japan might have been paired with their coeval batholiths along the 'Greater South China' margin that was extensively eroded during later tectonic processes. (C) 2020 Elsevier B.V. All rights reserved.

<p>東北日本の東縁に沿って分布する母体-松ヶ平帯中の古生代の年代を示す山上変成岩類は，高変成度の山上変成岩Ⅰと低変成度の山上変成岩Ⅱに区分されている．このうち，山上変成岩Ⅰは主に泥質片岩と角閃岩からなる．泥質片岩中のルチルにパラゴナイトが含まれることや変成鉱物の組成領域の検討から，山上変成岩Ⅰは蓮華帯の高変成度岩類と同等の低温高圧型変成作用を受けていると推定される．また，泥質片岩と角閃岩中のフェンジャイトK-Ar年代は322-287Maを示し，蓮華帯変成岩類と一致する．変成作用の特徴とフェンジャイトK-Ar年代から見て，山上変成岩類は西南日本の蓮華帯の高変成度岩類に直接対比できる可能性が高いと考えられる．</p>

We present optical multicolour photometry of V404 Cyg during the outburst from 2015 December to 2016 January together with the simultaneous X-ray data. This outburst occurred less than sixmonths after the previous outburst in 2015 June-July. These two outbursts in 2015 were of a slow-rise and rapid-decay type and showed large-amplitude (similar to 2mag) and short-term (similar to 10 min-3 h) optical variations even at low luminosity (0.01-0.1L(Edd)). We found correlated optical and X-ray variations in two similar to 1 h time intervals and obtained a Bayesian estimate of an X-ray delay against the optical emission, which is similar to 30-50 s, during those two intervals. In addition, the relationship between the optical and X-ray luminosities was L-opt alpha L-X(0.25-0.29) at that time. These features cannot be easily explained by the conventional picture of transient black hole binaries, such as canonical disc reprocessing and synchrotron emission related to a jet. We suggest that the disc was truncated during those intervals and that the X-ray delays represent the required time for the propagation of mass accretion flow to the inner optically thin region with a speed comparable to the free-fall velocity.

横山一己と共著

堤之恭，佐野貴司と共著

高木秀雄，新井宏嘉と共著

© 2016 Macmillan Publishers Limited. All rights reserved. How black holes accrete surrounding matter is a fundamental yet unsolved question in astrophysics. It is generally believed that matter is absorbed into black holes via accretion disks, the state of which depends primarily on the mass-accretion rate. When this rate approaches the critical rate (the Eddington limit), thermal instability is supposed to occur in the inner disk, causing repetitive patterns of large-amplitude X-ray variability (oscillations) on timescales of minutes to hours. In fact, such oscillations have been observed only in sources with a high mass-accretion rate, such as GRS 1915+105 (refs 2, 3). These large-amplitude, relatively slow timescale, phenomena are thought to have physical origins distinct from those of X-ray or optical variations with small amplitudes and fast timescales (less than about 10 seconds) often observed in other black-hole binaries - for example, XTE J1118+480 (ref. 4) and GX 339â '4 (ref. 5). Here we report an extensive multi-colour optical photometric data set of V404 Cygni, an X-ray transient source containing a black hole of nine solar masses (and a companion star) at a distance of 2.4 kiloparsecs (ref. 8). Our data show that optical oscillations on timescales of 100 seconds to 2.5 hours can occur at mass-accretion rates more than ten times lower than previously thought. This suggests that the accretion rate is not the critical parameter for inducing inner-disk instabilities. Instead, we propose that a long orbital period is a key condition for these large-amplitude oscillations, because the outer part of the large disk in binaries with long orbital periods will have surface densities too low to maintain sustained mass accretion to the inner part of the disk. The lack of sustained accretion - not the actual rate - would then be the critical factor causing large-amplitude oscillations in long-period systems.

林 衛，熊沢峰夫と共著

Continuing the project described in Kato et al. (2009, PASJ, 61, S395), we collected times of superhump maxima for SU UMa-type dwarf novae mainly observed during the 2012-2013 season. We found three objects (V444 Peg, CSS J203937, and MASTER J212624) having strongly positive period derivatives despite the long orbital period (Porb). By using the period of growing stage (stage A) superhumps, we obtained mass ratios for six objects. We characterized nine new WZ Sge-type dwarf novae. We made a pilot survey of the decline rate in the slowly fading parts of SU UMa-type and WZ Sge-type outbursts. The decline time scale was found to generally follow an expected Porb 1/4 dependence, and WZ Sge-type outbursts also generally follow this trend. There are some objects which show slower decline rates, and we consider these objects good candidates for period bouncers. We also studied unusual behavior in some objects, including BK Lyn which made a transition from an ER UMa-type state to a novalike (standstill) state in 2013, and unusually frequent occurrences of superoutbursts in NY Ser and CR Boo. We applied the least absolute shrinkage and selection operator (Lasso) power spectral analysis, which has been proven to be very effective in analyzing the Kepler data, to the ground-based photometry of BK Lyn, and detected a dramatic disappearance of the signal of negative superhumps in 2013. We suggested that the mass-transfer rates did not strongly vary between the ER UMa-type state and novalike state in BK Lyn, and this transition was less likely caused by a systematic variation of the mass-transfer rate. © 2014 The Author.

We carried out photometric observations of the SUUMa-type dwarf nova ERUMa during 2011 and 2012, which showed the existence of persistent negative superhumps even during the superoutburst. We performed a two-dimensional period analysis of its light curves by using a method called "least absolute shrinkage and selection operator" (Lasso) and the "phase dispersion minimization" (PDM) analysis, and found that the period of negative superhumps systematically changed between a superoutburst and the next superoutburst. The trend of the period change can be interpreted as a reflection of the change of the disk radius. This change is in agreement with the one predicted by the thermal tidal instability model. The normal outburst during a supercycle showed a general trend that the rising rate to its maximum becomes slower as the next superoutburst is approaching. The change can be interpreted as the consequence of the increased gas-stream flow into the inner region of the disk as a result of the tilted disk. Some of superoutbursts were found to be triggered by a precursor normal outburst when the positive superhump appeared to develop. The positive and negative superhumps coexisted during the superoutburst. Positive superhumps were prominent only for four or five days after the supermaximum, while the signal of negative superhumps became stronger after the middle phase of the superoutburst plateau. A simple combination of the positive and negative superhumps was found to be insufficient for reproduction of the complex profile variation. We were able to detect the developing phase of positive superhumps (stage A superhumps) for the first time in ER UMa-type dwarf novae. Using the period of stage A superhumps, we obtained a mass ratio of 0.100(15), which indicates that ERUMa is on the ordinary evolutional track of cataclysmic variable stars. © The Author 2014.

UPb ages of detrital zircons and white mica KAr ages are obtained from two psammitic schists from the western and eastern units of the Sanbagawa Metamorphic Belt located in the SakumaTenryu area. The detrital zircons in the sample from the western unit (T1) show an age cluster around 95?Ma, and the youngest age in the detrital zircons is 94.0 +/- 0.6?Ma. The detrital zircons in the sample from the eastern unit (T5) show a main age cluster in the Late Cretaceous with some older ages, and the youngest age in the detrital zircons is 72.8 +/- 0.9?Ma. The youngest zircon ages restrict the older limit of the depositional ages of each sample. White mica KAr ages of T1 and T5 are 69.8 +/- 1.5?Ma and 56.1 +/- 1.2?Ma, respectively, which indicate the age of exhumation and restrict the younger limit on the depositional age of each sample. The results show that the western and eastern units were different in their depositional and exhumation ages, suggesting the episodic subduction and exhumation of the Sanbagawa Belt in the SakumaTenryu area. These results also suggest simultaneous existence of subduction and exhumation paths of metamorphic rocks in the high-P/T Sanbagawa Metamorphic Belt.

Continuing the project described by Kato et al. (2009, PASJ, 61, S395), we collected the times of superhump maxima for 51 SU UMa-type dwarf novae, mainly observed during the 2010-2011 season. Although most of the new data for systems with short superhump periods basically confirmed the findings by Kato et al. (ibid.) and Kato et al. (2010, PASJ, 62, 1525), the long-period system GX Cas showed an exceptionally large positive-period derivative. An analysis of public Kepler data of V344 Lyr and V1504 Cyg yielded less-striking stage transitions. In V344 Lyr, there was a prominent secondary component growing during the late stage of superoutbursts, and this component persisted for at least two more cycles of successive normal outbursts. We also investigated the superoutburst of two conspicuous eclipsing objects: HT Cas and the WZ Sge-type object SDSS J080434.20+510349.2. Strong beat phenomena were detected in both objects, and late-stage superhumps in the latter object had an almost constant luminosity during repeated rebrightenings. The WZ Sge-type object SDSS J133941.11+484727.5 showed a phase reversal around the rapid fading from the superoutburst. The object showed a prominent beat phenomenon, even after the end of the superoutburst. A pilot study of superhump amplitudes indicated that the amplitude of superhumps is strongly correlated with the orbital period, and the dependence on the inclination is weak in systems with inclinations smaller than 80 degrees.

関東山地三波川帯の岩相分布, 温度構造ならびに剪断センスの逆転と, 標本スケールの横臥褶曲の両翼における剪断センスの決定から, 大規模な横臥褶曲の存在を本地域に想定することはできない.剪断センスが明瞭な試料は少なく, 石英のファブリックが異なるセンスを示すドメイン構造が同じ薄片内で認められる.また, 再結晶石英粒子の準三次元形態ならびにc軸ファブリック解析結果などから, 三波川帯全体としては上盤西方の延性剪断変形が卓越しているものの, 変形はZ軸方向に加えてY軸方向の短縮に伴って, X軸方向の一軸伸長変形が卓越していることが明らかにされた.剪断センスの逆転は, 海洋プレートの斜め沈み込み場において不均一に剪断変形が分配されて, 逆の速度勾配が生じたことによるものと考えられる.鉱物の伸長線構造は一貫して西北西-東南東方向であり, 三波川帯の上昇モデルとして, 押し出しモデルを支持する傾斜移動剪断運動の証拠は認められない.