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Optical emission from a kilonova following a gravitational-wave-detected neutron-star merger

机译：引力波探测到的中子星合并后，来自千新星的光发射

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摘要

The merger of two neutron stars has been predicted to produce an optical-infrared transient (lasting a few days) known as a 'kilonova', powered by the radioactive decay of neutron-rich species synthesized in the merger(1-5). Evidence that short gamma-ray bursts also arise from neutron-star mergers has been accumulating(6-8). In models(2,9) of such mergers, a small amount of mass (10(-4)-10(-2) solar masses) with a low electron fraction is ejected at high velocities (0.1-0.3 times light speed) or carried out by winds from an accretion disk formed around the newly merged object(10,11). This mass is expected to undergo rapid neutron capture (r-process) nucleosynthesis, leading to the formation of radioactive elements that release energy as they decay, powering an electromagnetic transient(1-3,9-14). A large uncertainty in the composition of the newly synthesized material leads to various expected colours, durations and luminosities for such transients(11-14). Observational evidence for kilonovae has so far been inconclusive because it was based on cases(15-19) of moderate excess emission detected in the afterglows of gamma-ray bursts. Here we report optical to near-infrared observations of a transient coincident with the detection of the gravitational-wave signature of a binary neutron-star merger and with a low-luminosity short-duration gamma-ray burst(20). Our observations, taken roughly every eight hours over a few days following the gravitational-wave trigger, reveal an initial blue excess, with fast optical fading and reddening. Using numerical models(21), we conclude that our data are broadly consistent with a light curve powered by a few hundredths of a solar mass of low-opacity material corresponding to lanthanide-poor (a fraction of 10(-4.5) by mass) ejecta.
机译：预计两个中子星的合并会产生一个光学红外瞬变（持续数天），称为“基洛诺娃”，由合并中合成的富含中子的物质的放射性衰变提供动力（1-5）。越来越多的证据表明，中子星合并也产生了短的伽马射线爆发（6-8）。在这种合并的模型（2,9）中，少量的具有低电子分数的质量（10（-4）-10（-2）太阳质量）以高速（光速的0.1-0.3倍）或由来自新合并对象周围形成的吸积盘的风（10,11）进行。预期该物质将经历快速的中子捕获（r过程）核合成，导致形成放射性元素，这些元素在衰变时释放能量，从而为电磁瞬变提供动力（1-3,9-14）。新合成材料的成分存在很大的不确定性，导致此类瞬态产生各种预期的颜色，持续时间和发光度（11-14）。迄今为止，关于千伏新星的观测证据尚无定论，因为它是基于在伽马射线爆发余辉中检测到中等过量发射的案例（15-19）。在这里，我们报告了一个瞬态的光学到近红外观测结果，该观测值与双星中子星合并的引力波特征的检测以及低发光度的短持续时间伽马射线爆裂相吻合（20）。在引力波触发后的几天内，我们大约每八小时进行一次观测，结果显示出最初的蓝色过量，并且光学褪色和发红迅速。使用数值模型（21），我们得出结论，我们的数据与由几百分之一的低不透明度材料的太阳能质量（对应于贫镧系元素）（质量分数为10（-4.5）的百分之几）驱动的光曲线大致一致弹出。

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  • 来源
    《Nature》 |2017年第7678期|64-66|共3页
  • 作者

    Arcavi Iair; Hosseinzadeh Griffin; Howell D. Andrew; McCully Curtis; Poznanski Dovi; Kasen Daniel; Barnes Jennifer; Zaltzman Michael; Vasylyev Sergiy; Maoz Dan; Valenti Stefano;

  • 作者单位

    Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA|Las Cumbres Observ, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA;

    Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA|Las Cumbres Observ, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA;

    Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA|Las Cumbres Observ, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA;

    Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA|Las Cumbres Observ, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA;

    Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel;

    Lawrence Berkeley Natl Lab, Nucl Sci Div, Berkeley, CA 94720 USA|Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA|Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA;

    Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA;

    Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel;

    Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA|Las Cumbres Observ, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA;

    Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel;

    Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA;

  • 收录信息 美国《科学引文索引》(SCI);美国《工程索引》(EI);美国《生物学医学文摘》(MEDLINE);美国《化学文摘》(CA);
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