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Repetitive patterns in rapid optical variations in the nearby black-hole binary V404 Cygni

机译：附近黑洞二进制V404 Cygni中快速光学变化的重复模式

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摘要

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(1). 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 339-4 (ref. 5). Here we report an extensive multi-colour optical photometric data set of V404 Cygni, an X-ray transient source(6) containing a black hole of nine solar masses(7) (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(1). 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.
机译：黑洞如何增加周围物质是天体物理学中一个基本但尚未解决的问题。通常认为物质是通过吸积盘吸收到黑洞中的，吸盘的状态主要取决于质量吸积率。当该速率接近临界速率（爱丁顿极限）时，内盘会发生热不稳定性，从而在数分钟至数小时的时间尺度上引起大幅度X射线可变性（振荡）的重复模式（1）。实际上，仅在具有高质量积聚率的源（例如GRS 1915 + 105）（参考文献2、3）中观察到了这种振荡。这些大振幅，相对较慢的时标现象被认为具有不同于X射线或光学变化的物理起源，而在其他黑洞二进制文件中通常观察到这种现象具有较小的振幅和快速的时标（小于约10秒）。 ，XTE J1118 + 480（参考文献4）和GX 339-4（参考文献5）。在这里，我们报告了V404 Cygni的广泛的多色光学测光数据集，这是一个X射线瞬变源（6），其中包含一个黑洞，该黑洞有9个太阳质量（7）（和一个伴星），相距2.4千帕秒（参考8）我们的数据表明，在质量增加速率比先前认为的低十倍以上的情况下，在100秒到2.5小时的时间尺度上可能发生光振荡（1）。这表明，吸积率不是诱发内部磁盘不稳定性的关键参数。相反，我们建议较长的轨道周期是这些大振幅振荡的关键条件，因为具有较长轨道周期的双星中大盘的外部将具有太低的表面密度，以致无法维持恒星内部的质量累积磁盘。那么，缺乏持续的积聚（不是实际的速率）将成为导致长周期系统中大振幅振荡的关键因素。

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  • 来源
    《Nature》 |2016年第7584期|54-58|共5页
  • 作者

    Kimura Mariko; Isogai Keisuke; Kato Taichi; Ueda Yoshihiro; Nakahira Satoshi; Shidatsu Megumi; Enoto Teruaki; Hori Takafumi; Nogami Daisaku; Littlefield Colin; Ishioka Ryoko; Chen Ying-Tung; King Sun-Kun; Wen Chih-Yi; Wang Shiang-Yu; Lehner Matthew J.; Schwamb Megan E.; Wang Jen-Hung; Zhang Zhi-Wei; Alcock Charles; Axelrod Tim; Bianco Federica B.; Byun Yong-Ik; Chen Wen-Ping; Cook Kem H.; Kim Dae-Won; Lee Typhoon; Marshall Stuart L.; Pavlenko Elena P.; Antonyuk Oksana I.; Antonyuk Kirill A.; Pit Nikolai V.; Sosnovskij Aleksei A.; Babina Julia V.; Baklanov Aleksei V.; Pozanenko Alexei S.; Mazaeva Elena D.; Schmalz Sergei E.; Reva Inna V.; Belan Sergei P.; Inasaridze Raguli Ya.; Tungalag Namkhai; Volnova Alina A.; Molotov Igor E.; de Miguel Enrique; Kasai Kiyoshi; Stein William L.; Dubovsky Pavol A.; Kiyota Seiichiro; Miller Ian; Richmond Michael; Goff William; Andreev Maksim V.; Takahashi Hiromitsu; Kojiguchi Naoto; Sugiura Yuki; Takeda Nao; Yamada Eiji; Matsumoto Katsura; James Nick; Pickard Roger D.; Tordai Tamas; Maeda Yutaka; Ruiz Javier; Miyashita Atsushi; Cook Lewis M.; Imada Akira; Uemura Makoto;

  • 作者单位

    Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan;

    Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan;

    Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan;

    Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan;

    Japan Aerosp Explorat Agcy, Human Spaceflight Technol Directorate, JEM Mission Operat & Integrat Ctr, 2-1-1 Sengen, Tsukuba, Ibaraki 3058505, Japan;

    RIKEN, MAXI Team, 2-1 Hirosawa, Wako, Saitama 3510198, Japan;

    Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan|Kyoto Univ, Hakubi Ctr Adv Res, Kyoto 6068302, Japan;

    Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan;

    Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan;

    Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA;

    Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan;

    Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan;

    Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan;

    Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan;

    Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan;

    Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan|Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19125 USA|Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA;

    Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan;

    Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan;

    Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan;

    Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA;

    Univ Arizona, Steward Observ, Tucson, AZ 85721 USA;

    NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA;

    Yonsei Univ, Dept Astron, Seoul 120749, South Korea|Yonsei Univ, Univ Observ, Seoul 120749, South Korea;

    Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan|Natl Cent Univ, Dept Phys, Chungli 32054, Taiwan;

    Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan;

    Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany;

    Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan;

    Stanford Univ, KIPAC, 452 Lomita Mall, Stanford, CA 94309 USA;

    Crimean Astrophys Observ, Nauchnyi, Crimea, Ukraine;

    Crimean Astrophys Observ, Nauchnyi, Crimea, Ukraine;

    Crimean Astrophys Observ, Nauchnyi, Crimea, Ukraine;

    Crimean Astrophys Observ, Nauchnyi, Crimea, Ukraine;

    Crimean Astrophys Observ, Nauchnyi, Crimea, Ukraine;

    Crimean Astrophys Observ, Nauchnyi, Crimea, Ukraine;

    Crimean Astrophys Observ, Nauchnyi, Crimea, Ukraine;

    Russian Acad Sci, Space Res Inst, Moscow 117997, Russia|Natl Res Nucl Univ, MEPhI Moscow Engn Phys Inst, Moscow, Russia;

    Russian Acad Sci, Space Res Inst, Moscow 117997, Russia;

    Leibniz Inst Astrophys, Potsdam, Germany;

    Fesenkov Astrophys Inst, Alma Ata, Kazakhstan;

    Crimean Astrophys Observ, Nauchnyi, Crimea, Ukraine;

    Ilia State Univ, Kharadze Abastumani Astrophys Observ, Tbilisi, Rep of Georgia;

    Mongolian Acad Sci, Inst Astron & Geophys, Ulaanbaatar 13343, Mongol Peo Rep;

    Russian Acad Sci, Space Res Inst, Moscow 117997, Russia;

    Russian Acad Sci, Keldysh Inst Appl Math, Moscow, Russia;

    Univ Huelva, Fac Ciencias Expt, Dept Fis Aplicada, Huelva 21071, Spain|Observ CIECEM, Ctr Backyard Astrophys, Parque Dunar, Almonte 21760, Huelva, Spain;

    Baselstr 133D, CH-4132 Muttenz, Switzerland;

    6025 Calle Paraiso, Las Cruces, NM 88012 USA;

    Vihorlat Observ, Mierova 4, Humenne, Slovakia;

    VSOLJ, 7-1 Kitahatsutomi, Chiba 2730126, Japan;

    Furzehill House, Swansea SA2 7LE, W Glam, Wales;

    Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA;

    AAVSO, 13508 Monitor Lane, Sutter Creek, CA 95685 USA;

    Russian Acad Sci, Inst Astron, Peak Terskol 361605, Kabardino Balka, Russia|Natl Acad Sci Ukraine, Int Ctr Astron Med & Ecol Res, 27 Akad Zabolotnoho St, UA-03680 Kiev, Ukraine;

    Hiroshima Univ, Sch Sci, Dept Phys Sci, 1-3-1 Kagamiyama, Hiroshima 7398526, Japan;

    Osaka Kyoiku Univ, 4-698-1 Asahigaoka, Osaka 5828582, Japan;

    Osaka Kyoiku Univ, 4-698-1 Asahigaoka, Osaka 5828582, Japan;

    Osaka Kyoiku Univ, 4-698-1 Asahigaoka, Osaka 5828582, Japan;

    Osaka Kyoiku Univ, 4-698-1 Asahigaoka, Osaka 5828582, Japan;

    Osaka Kyoiku Univ, 4-698-1 Asahigaoka, Osaka 5828582, Japan;

    1 Tavistock Rd, Chelmsford CM1 6JL, Essex, England;

    BAA VSS, Burlington House, London W1J 0DU, England|3 Birches, Leominster HR6 9NG, Hereford, England;

    Hungarian Astron Assoc, Polaris Observ, Laborc Utca 2-C, H-1037 Budapest, Hungary;

    112-14 Kaminishiyama Machi, Nagasaki, Nagasaki 8500006, Japan;

    Observ Cantabria, Carretera Rocamundo Sin Numero, Valderredible, Cantabria, Spain|CSIC UC, Inst Fis Cantabria, Ave Los Castros Sin Numero, E-39005 Santander, Cantabria, Spain|Agrupac Astron Cantabra, Apartado 573, Santander 39080, Spain;

    Seikei High Sch, Seikei Meteorol Observ, Kichijoji Kitamachi 3-10-13, Tokyo 1808633, Japan;

    Ctr Backyard Astrophys Concord, 1730 Helix Court, Concord, CA 94518 USA;

    Kyoto Univ, Kwasan Observ, Yamashina Ku, Kitakazan Ohmine Cho, Kyoto 6078471, Japan|Kyoto Univ, Hida Observ, Yamashina Ku, Kitakazan Ohmine Cho, Kyoto 6078471, Japan;

    Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Kagamiyama 1-3-1, Hiroshima 7398526, Japan;

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