贫氢超亮恒星爆炸
Hydrogen-poor superluminous stellar explosions
摘要：
超新星（SNe）是由引力或热核能量驱动的恒星爆炸，以电磁辐射的形式发射数周或更长时间。在所有已知的超新星中，这种辐射都来自内能，这些内能是由新合成的元素（通常是56镍）的放射性衰变、超巨星包层爆炸冲击波所储存的热量，或者是超新星碎片与缓慢移动的富含氢的星周物质之间的相互作用而沉积在喷出物中。在这里，我们报告一类新的发光SNe，其观察到的属性不能解释任何这些已知的过程。其中包括我们发现的四个新的SNe，以及两个之前无法解释的事件（SN 2005 ap; SCP 06 F6），我们现在可以将其确定为成员。这些SNe都比SNe Ia亮10倍左右，没有氢的痕迹，在很长一段时间内发出显著的紫外线（UV）通量，并且具有与放射性不一致的后期衰变率。我们的数据要求观测到的辐射是由分布在大半径（~10^15 cm）上的无氢物质发射的，并且以高速（>10^4 km·s^-1）膨胀。这些长寿命的紫外发光事件可以观测到红移z>4，并为研究原始遥远星系中的恒星形成和星际介质提供了极好的机会。
英文摘要：
Supernovae (SNe) are stellar explosions driven by gravitational or thermonuclear energy, observed as electromagnetic radiation emitted over weeks or more. In all known SNe, this radiation comes from internal energy deposited in the outflowing ejecta by either radioactive decay of freshly-synthesized elements (typically 56Ni), stored heat deposited by the explosion shock in the envelope of a supergiant star, or interaction between the SN debris and slowly-moving, hydrogen-rich circumstellar material. Here we report on a new class of luminous SNe whose observed properties cannot be explained by any of these known processes. These include four new SNe we have discovered, and two previously unexplained events (SN 2005ap; SCP 06F6) that we can now identify as members. These SNe are all ~10 times brighter than SNe Ia, do not show any trace of hydrogen, emit significant ultra-violet (UV) flux for extended periods of time, and have late-time decay rates which are inconsistent with radioactivity. Our data require that the observed radiation is emitted by hydrogen-free material distributed over a large radius (~10^15 cm) and expanding at high velocities (>10^4 km s^-1). These long-lived, UV-luminous events can be observed out to redshifts z>4 and offer an excellent opportunity to study star formation in, and the interstellar medium of, primitive distant galaxies.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
