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Hydrogen-poor superluminous stellar explosions

机译:贫氢超发光恒星爆炸

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摘要

Supernovae are stellar explosions driven by gravitational or thermonuclear energy that is observed as electromagnetic radiation emitted over weeks or more~1. In all known supernovae, this radiation comes from internal energy deposited in the outflowing ejecta by one or more of the following processes: radioactive decay of freshly synthesized elements~2 (typically ~(56)Ni), the explosion shock in the envelope of a supergiant star~3, and interaction between the debris and slowly moving, hydrogen-rich circumstellar material~4. Here we report observations of a class of luminous supernovae whose properties cannot be explained by any of these processes. The class includes four new supernovae that we have discovered and two previously unexplained events~(5,6) (SN 2005ap and SCP 06F6) that we can now identify as members of the same class. These supernovae are all about ten times brighter than most type la supernova, do not show any trace of hydrogen, emit significant ultraviolet flux for extended periods of time and have late-time decay rates that are inconsistent with radioactivity. Our data require that the observed radiation be emitted by hydrogen-free material distributed over a large radius (~10~(15) centimetres) and expanding at high speeds (>10~4 kilometres per second). These long-lived, ultraviolet-luminous events can be observed out to redshifts z > 4.%在所有已知超新星中,它们所发射的辐射都来 自被新和成的元素的一次或多次的衰变沉积在 外流喷射物中的内部能量,来自被一颗超大恒 星的外包层中的爆炸激波沉积的存储能量,或 来自碎片与慢速运动的、富含氢的恒星周围物 质之间的相互作用。
机译:超新星是由引力或热核能驱动的恒星爆炸,被观察为数周或更长时间〜1内发出的电磁辐射。在所有已知的超新星中,这种辐射来自于通过以下一种或多种过程沉积在流出的喷射流中的内部能量:新合成元素〜2(通常为〜(56)Ni)的放射性衰变,超级恒星〜3,以及碎片与缓慢移动的富含氢的恒星物质〜4之间的相互作用。在这里,我们报告一类发光超新星的观测结果,其性质无法用这些过程中的任何一个来解释。该班级包括我们发现的四个新超新星和两个我们现在可以识别为同一班级成员的先前无法解释的事件〜(5,6)(SN 2005ap和SCP 06F6)。这些超新星的亮度都比大多数la型超新星明亮约十倍,没有显示出任何痕量的氢,在较长的时间段内会发出大量的紫外线通量,并且其后期衰变速率与放射性不一致。我们的数据要求观察到的辐射是由分布在较大半径(〜10〜(15)厘米)并以高速(> 10〜4公里/秒)扩展的无氢材料发出的。这些长期存在的紫外线发光事件可观察到红移z> 4.%。在所有已知超新星中,其所发射的辐射都来自被新和成的元素的一次或多次的衰变沉积在外流喷射的内部能量,来自被一颗超大恒星的扩展层中的爆炸激波沉积的存储能量,或来自碎片与慢速运动的,伴随氢的恒星周围物质之间的相互作用。 。

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  • 来源
    《Nature》 |2011年第7352期|p.487-489407|共4页
  • 作者单位

    Cahili Center for Astrophysics 249-17, California Institute of Technology, Pasadena, California 91125, USA;

    Cahili Center for Astrophysics 249-17, California Institute of Technology, Pasadena, California 91125, USA;

    Cahili Center for Astrophysics 249-17, California Institute of Technology, Pasadena, California 91125, USA;

    Benoziyo Center for Astrophysics, Faculty of Physics, Weizmann Institute of Science, 76100 Rehovot, Israel;

    Benoziyo Center for Astrophysics, Faculty of Physics, Weizmann Institute of Science, 76100 Rehovot, Israel;

    Department of Physics (Astrophysics), University of Oxford, Denys Wilkinson Building, Keble Road, Oxford 0X1 3RH, UK;

    Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA;

    Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA;

    Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Goleta, California 93117, USA Department of Physics, University of California, Santa Barbara, Broida HalI, Santa Barbara, California 93106, USA;

    Raymondand Beverly Sackler School of Physics & Astronomy, Tel Aviv University, Tel Aviv 69978, Israel;

    Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Goleta, California 93117, USA Kavli Institute for Theoretical Physics,KohnHall, University of California, Santa Barbara, California 93106, USA;

    University of California, San Diego, Department of Physics, 9500 Gilman Drive, La Jolla, California 92093, USA;

    Cahili Center for Astrophysics 249-17, California Institute of Technology, Pasadena, California 91125, USA Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto, Ontario M5S 3H4, Canada;

    Caltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USA;

    Caltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USA;

    Caltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USA;

    Caltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USA;

    Caltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USA;

    Caltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USA;

    Caltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USA;

    Caltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USA;

    Caltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USA;

    Caltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USA;

    Caltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USA;

    Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA Astronomy Department, University of California, Berkeley, 601 Campbell Hall, Berkeley, California 94720, USA;

    Astronomy Department, University of California, Berkeley, 601 Campbell Hall, Berkeley, California 94720, USA;

    Department of Physics, California Institute of Technology, Pasadena,California 91125, USA;

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