arXiv 2103.026112021-03astro-ph.HE

发光和双峰的Ic型超新星2019stc：多能源的证据

The Luminous and Double-Peaked Type Ic Supernova 2019stc: Evidence for Multiple Energy Sources

Sebastian Gomez, Edo Berger, Griffin Hosseinzadeh, Peter K. Blanchard, Matt Nicholl, V. Ashley Villar

备注：: 14 pages, 13 figures, Accepted to ApJ
发表信息：: The Astrophysical Journal, 2021 June 4, Volume 913, Number 2
DOI：: 10.3847/1538-4357/abf5e3

摘要：

本文报道了一颗红移为$z=0.117$的罕见Ic型超新星（SN Ic）SN 1，2019stc（= ZTF 19acbonaa）的光度学和光谱学。SN\，2019 stc显示出宽的双峰光变曲线，第一个峰的绝对星等为$M_r=-20.0$ mag，第二个峰的绝对星等为$M_r=-19.2$ mag，大约80个静止帧天后，总辐射能量很大，为$E_{\rm rad}\approx 2.5\times 10^{50}$ erg。尽管SN\，2019 stc的亮度很大，接近I型超亮超新星（SLSNe）的亮度，但它仍表现出典型的SN Ic光谱，弥补了SLSNe和SNe Ic之间的差距。光谱表明存在Fe峰元素，但仅用放射性加热对第一光变曲线峰进行建模导致$f_{\rm Ni}\approx 31\%$（$M_{\rm Ni}\approx 3.2$ M $_\odot$）的镍质量分数异常高。相反，如果我们用组合的磁星自旋下降和放射性加热模型来模拟第一个峰，我们发现与$M_{\rm ej}\approx 4$ M $_\odot$、$P_{\rm spin}\approx 7.2$ ms的磁星自旋周期和$B\approx 10^{14}$ G和$f_{\rm Ni}\lesssim 0.2$的磁场更好地匹配（与SNe Ic一致）。突出的第二个峰不能自然地与放射性加热或磁星自旋下降相适应，而是可以解释为与位于$\approx 400$ AU的无氢物质的$\approx 0.7$ $M_\odot$的星周相互作用。在$\approx 6.5$ M $_\odot$爆炸之前，包括残余质量导致CO核心质量。宿主星系的金属丰度为$\approx 0.26$ Z $_\odot$，低于SNe Ic，但与SLSNe一致。总的来说，我们发现SN1，2019stc是正常SNe Ic和SLSNe之间的过渡对象。

英文摘要：

We present optical photometry and spectroscopy of SN\,2019stc (=ZTF19acbonaa), an unusual Type Ic supernova (SN Ic) at a redshift of $z=0.117$. SN\,2019stc exhibits a broad double-peaked light curve, with the first peak having an absolute magnitude of $M_r=-20.0$ mag, and the second peak, about 80 rest-frame days later, $M_r=-19.2$ mag. The total radiated energy is large, $E_{\rm rad}\approx 2.5\times 10^{50}$ erg. Despite its large luminosity, approaching those of Type I superluminous supernovae (SLSNe), SN\,2019stc exhibits a typical SN Ic spectrum, bridging the gap between SLSNe and SNe Ic. The spectra indicate the presence of Fe-peak elements, but modeling of the first light curve peak with radioactive heating alone leads to an unusually high nickel mass fraction of $f_{\rm Ni}\approx 31\%$ ($M_{\rm Ni}\approx 3.2$ M$_\odot$). Instead, if we model the first peak with a combined magnetar spin-down and radioactive heating model we find a better match with $M_{\rm ej}\approx 4$ M$_\odot$, a magnetar spin period of $P_{\rm spin}\approx 7.2$ ms and magnetic field of $B\approx 10^{14}$ G, and $f_{\rm Ni}\lesssim 0.2$ (consistent with SNe Ic). The prominent second peak cannot be naturally accommodated with radioactive heating or magnetar spin-down, but instead can be explained as circumstellar interaction with $\approx 0.7$ $M_\odot$ of hydrogen-free material located $\approx 400$ AU from the progenitor. Including the remnant mass leads to a CO core mass prior to explosion of $\approx 6.5$ M$_\odot$. The host galaxy has a metallicity of $\approx 0.26$ Z$_\odot$, low for SNe Ic but consistent with SLSNe. Overall, we find that SN\,2019stc is a transition object between normal SNe Ic and SLSNe.

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。

摘要：

英文摘要：

相关论文