PTF11rka: an interacting supernova at the crossroads of stripped-envelope and H-poor superluminous stellar core collapses-猫眼课题宝

DOI：

10.1093/mnras/staa2191

发表时间：

2020-07

期刊：

Monthly Notices of the Royal Astronomical Society

影响因子：

4.8

通讯作者：

中科院分区：

物理与天体物理2区

文献类型：

作者：

E. Pian;P. Mazzali;T. Moriya;A. Rubin;A. Gal-yam;I. Arcavi;S. Ben-Ami;N. Blagorodnova;M. Bufano;A. Filippenko;M. Kasliwal;S. Kulkarni;R. Lunnan;I. Manulis;T. Matheson;P. Nugent;E. Ofek;D. Perley;S. Prentice;Ofer Yaron INAF-OAS Bologna;Italy.;Liverpool John Moores Univ.;Ari;Mpa;Garching;H Germany;Naoj;Mitaka;Tokyo;S. O. Physics;Astronomy;Monash Univ.;Australia.;Eső;B. C. F. Astrophysics;Weizmann Institute of Science;Israel;T. Univ.;Cifar;Canada;Harvard-Smithsonian Cfa;Dept of AstrophysicsIMAPP;Radboud Univ.;Nijmegen;The Netherlands.;Inaf - Catania;D. Astronomy;Univ. of California;Berkeley;Miller Senior Fellow;Cahill Center for Astrophysics;Caltech;O. K. C. -. Astronomy;S. Univ.;NSF's National Optical-Infrared Astronomy Research Laboratory-NSF's-National-Optical-Infrared-Astronomy-Research-1753670520;Tucson;L. B. N. Laboratory;Trinity College Dublin;The University of Dublin

由Palomar Transient Factory报告的贫氢超新星PTF 11 rka（z = 0.0744），在2011年12月5日UT估计爆炸时间后的几天开始被各种望远镜观测到，此后长达432个休息帧天。光变曲线的上升部分仅在RPTF滤波器带中监测，并且在估计的爆炸时间之后的2030个静止帧天达到该带中的最大值。PTF 11 rka的光变曲线和光谱与一个10 M质量的碳氧核的坍缩爆炸相一致，该核是从一个主序质量为25-40 M质量的母核演化而来的，它释放了动能Ek = 4 × 1051 erg，喷出了108 M质量的喷出物，并合成了100.5 M质量的56 Ni。PTF 11 rka的光球光谱的特征是窄吸收线，指向最高喷出物速度（15000 km s−1）的抑制。如果喷出物撞击到一个致密的、混浊的星周介质，这是可以预料的。这反过来又导致它们损失了一小部分能量（105 × 1050 erg），其中不到2%转化为维持最大亮度之前的光变曲线的辐射。这让人想起了超发光的SN 2007 bi，其光变曲线形状和光谱与PTF 11 rka非常相似，尽管后者的亮度低10倍，而且演化速度更快。PTF 11 rka实际上在光度上更类似于伽马射线暴SNe，尽管它具有较低的能量和较低的Ek/Mej比。

The hydrogen-poor supernova (SN) PTF11rka (z = 0.0744), reported by the Palomar Transient Factory, was observed with various telescopes starting a few days after the estimated explosion time of 2011 December 5 UT and up to 432 rest-frame days thereafter. The rising part of the light curve was monitored only in the RPTF filter band, and maximum in this band was reached ∼30 rest-frame days after the estimated explosion time. The light curve and spectra of PTF11rka are consistent with the core-collapse explosion of a ∼10 M⊙ carbon–oxygen core evolved from a progenitor of main-sequence mass 25–40 M⊙, that liberated a kinetic energy Ek≈4 × 1051 erg, expelled ∼8 M⊙ of ejecta, and synthesized ∼0.5 M⊙ of 56Ni. The photospheric spectra of PTF11rka are characterized by narrow absorption lines that point to suppression of the highest ejecta velocities (≳ 15 000 km s−1). This would be expected if the ejecta impacted a dense, clumpy circumstellar medium. This in turn caused them to lose a fraction of their energy (∼5 × 1050 erg), less than 2 per cent of which was converted into radiation that sustained the light curve before maximum brightness. This is reminiscent of the superluminous SN 2007bi, the light-curve shape and spectra of which are very similar to those of PTF11rka, although the latter is a factor of 10 less luminous and evolves faster in time. PTF11rka is in fact more similar to gamma-ray burst SNe in luminosity, although it has a lower energy and a lower Ek/Mej ratio.

PTF11rka: an interacting supernova at the crossroads of stripped-envelope and H-poor superluminous stellar core collapses

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