千新星

千新星（kilonova 或 r-process 超新星），是一类发生于双致密天体（如双中子星，中子星与黑洞）并合过程中的暂现天文事件^[1]。由于在并合过程中产生各向同性的物质抛射和重的R-過程元素的放射性衰变，千新星被认为可以发出短伽玛射线暴和强电磁辐射。

這位藝術家的視頻顯示了兩顆微小但非常密集的中子星如何通過引力波輻射合併，然後爆炸成一個千新星。

人类利用哈勃空间望远镜于2013年首次观测到千新星事件^[1]。

理论

双致密天体的绕转与并合过程是强的引力波源^[2]。千新星被认为与短伽玛暴^[2] (GRB) 的前身星密切相关，它是宇宙中稳定的r过程重元素的最主要来源。^[1] “千新星”的概念由 Metzger 等人于2010年提出^[2]，它因峰亮度可达经典新星的1000倍而得名。中子星并合的基本模型由李立新和玻丹·帕琴斯基于1998年提出。^[3]

观测

哈伯觀測到的第一顆千新星。^[4]

千新星事件的第一次明确观测发生于2013年, 这一事件与短伽玛暴 GRB 130603B 成协, 这一遥远的发射信号由哈勃空间望远镜观测到^[1]。

2017年10月16日, LIGO与Virgo 团队联合宣布第一次同时探测到引力波 (GW170817) 信号及其电磁辐射对应体（GRB 170817A, SSS17a）^[5]，并且证明电磁辐射信号的源是双中子星并合过程产生的千新星^[6]。在短GRB之后，人们又接收到了持续数周的光学暂现源（AT 2017gfo），它位于相对邻近的星系 NGC 4993。^[7]

参见

参考资料

^ ^1.0 ^1.1 ^1.2 ^1.3 Tanvir, N. R.; Levan, A. J.; Fruchter, A. S.; Hjorth, J.; Hounsell, R. A.; Wiersema, K.; Tunnicliffe, R. L. A 'kilonova' associated with the short-duration γ-ray burst GRB 130603B. Nature. 2013, 500 (7464): 547–9. Bibcode:2013Natur.500..547T. PMID 23912055. arXiv:1306.4971  . doi:10.1038/nature12505.
^ ^2.0 ^2.1 ^2.2 Metzger, B. D.; Martínez-Pinedo, G.; Darbha, S.; Quataert, E.; et al. Electromagnetic counterparts of compact object mergers powered by the radioactive decay of r-process nuclei. Monthly Notices of the Royal Astronomical Society. August 2010, 406 (4): 2650. Bibcode:2010MNRAS.406.2650M. arXiv:1001.5029  . doi:10.1111/j.1365-2966.2010.16864.x.
^ Li-Xin Li and Bohdan Paczyński. Transient Events from Neutron Star Mergers. The Astrophysical Journal. 1998, 507: L59-L62.
^ Hubble observes source of gravitational waves for the first time. www.spacetelescope.org. [18 October 2017]. （原始内容存档于2017-10-19）.
^ Abbott, B. P.; Abbott, R.; Abbott, T. D.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.; Adya, V. B. GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral. Physical Review Letters. 16 October 2017, 119 (16). doi:10.1103/PhysRevLett.119.161101. 已忽略未知参数|collaboration= (帮助)
^ Miller, M. Coleman. Gravitational waves: A golden binary. Nature. 16 October 2017,. News and Views. doi:10.1038/nature24153.
^ Berger, Edo. Focus on the Electromagnetic Counterpart of the Neutron Star Binary Merger GW170817. Astrophysical Journal Letters. IOP Science. 16 October 2017 [16 October 2017]. （原始内容存档于2018-09-13）.

外部链接

List of all known kilonovae（页面存档备份，存于互联网档案馆） at The Open Kilonova Catalog（页面存档备份，存于互联网档案馆）.

[Tanvir2013-1] 1.0 ^1.1 ^1.2 ^1.3 Tanvir, N. R.; Levan, A. J.; Fruchter, A. S.; Hjorth, J.; Hounsell, R. A.; Wiersema, K.; Tunnicliffe, R. L. A 'kilonova' associated with the short-duration γ-ray burst GRB 130603B. Nature. 2013, 500 (7464): 547–9. Bibcode:2013Natur.500..547T. PMID 23912055. arXiv:1306.4971  . doi:10.1038/nature12505.

[Metzger2010-2] 2.0 ^2.1 ^2.2 Metzger, B. D.; Martínez-Pinedo, G.; Darbha, S.; Quataert, E.; et al. Electromagnetic counterparts of compact object mergers powered by the radioactive decay of r-process nuclei. Monthly Notices of the Royal Astronomical Society. August 2010, 406 (4): 2650. Bibcode:2010MNRAS.406.2650M. arXiv:1001.5029  . doi:10.1111/j.1365-2966.2010.16864.x.

[LiPaczynski1998-3] Li-Xin Li and Bohdan Paczyński. Transient Events from Neutron Star Mergers. The Astrophysical Journal. 1998, 507: L59-L62.

[4] Hubble observes source of gravitational waves for the first time. www.spacetelescope.org. [18 October 2017]. （原始内容存档于2017-10-19）.

[Abbott_et_al._2017-5] Abbott, B. P.; Abbott, R.; Abbott, T. D.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.; Adya, V. B. GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral. Physical Review Letters. 16 October 2017, 119 (16). doi:10.1103/PhysRevLett.119.161101. 已忽略未知参数|collaboration= (帮助)

[miller2017-6] Miller, M. Coleman. Gravitational waves: A golden binary. Nature. 16 October 2017,. News and Views. doi:10.1038/nature24153.

[berger2017-7] Berger, Edo. Focus on the Electromagnetic Counterpart of the Neutron Star Binary Merger GW170817. Astrophysical Journal Letters. IOP Science. 16 October 2017 [16 October 2017]. （原始内容存档于2018-09-13）.

[1]

[2]

[3]

[4]

[5]

[6]

[7]