The Early Light Curve of the Type Ia Supernova 2021hpr in NGC 3147: Progenitor Constraints with the Companion Interaction Model
The Early Light Curve of the Type Ia Supernova 2021hpr in NGC 3147: Progenitor Constraints with the Companion Interaction Model
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DOI：
10.3847/1538-4357/acc10c
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发表时间：
2023-03
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通讯作者：
G. Lim;M. Im;G. S. Paek;Sung-Chul Yoon;Changsu Choi;Sophia Kim;J. Wheeler;B. Thomas;J. Vinkó;Dohyeong Kim;Jinguk Seo;W. Kang;Taewoo Kim;H. Sung;Yonggi Kim;J.-N. Yoon;Hae-Yeon Kim;Jeong-Gyu Kim;Hana Bae;S. Ehgamberdiev;O. Burhonov;D. Mirzaqulov
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作者：
G. Lim;M. Im;G. S. Paek;Sung-Chul Yoon;Changsu Choi;Sophia Kim;J. Wheeler;B. Thomas;J. Vinkó;Dohyeong Kim;Jinguk Seo;W. Kang;Taewoo Kim;H. Sung;Yonggi Kim;J.-N. Yoon;Hae-Yeon Kim;Jeong-Gyu Kim;Hana Bae;S. Ehgamberdiev;O. Burhonov;D. Mirzaqulov
Ia 型超新星 (SNe Ia) 的前身系统预计是一个由碳/氧白矮星 (WD) 和非简并恒星或另一个 WD 组成的紧密双星系统。在这里，我们展示了对螺旋星系 NGC 3147 中的 SN 2021hpr 进行高节奏监测观测的结果，以及基于其早期多色光曲线数据对祖系统的约束。首先，我们根据 SN 2021hpr 的长期光度和光谱数据将其归类为正常的 SN Ia。更有趣的是，我们发现光变曲线在简单的幂律∼t 2 演化过程中存在显着的“早期过剩”。在第一周内，早期光曲线从蓝色演变为红色，再演变为蓝色。为了解释这一点，我们将 BVRI 波段光变曲线的早期部分与由喷射物-伴星相互作用和简单幂律模型组成的二元模型进行了拟合。早期的过量现象及其颜色可以用半径为 8.84 ± 0.58 R ⊙ 的伴星引起的激冷发射来解释。我们还检查了哈勃太空望远镜爆炸前的图像，没有发现任何候选祖星，这与上述结果一致。然而，我们无法检测到来自非简并伴星的大量剥离质量的迹象（对于 Hα 发射，≲0.003 M ⊙）。多波段光曲线中的早期多余光支持 SN 2021hpr 祖先系统中的非简并伴星。与此同时，未检测到发射线为其他方法解释这一事件打开了大门。
The progenitor system of Type Ia supernovae (SNe Ia) is expected to be a close binary system consisting of a carbon/oxygen white dwarf (WD) and a nondegenerate star or another WD. Here, we present results from high-cadence monitoring observations of SN 2021hpr in a spiral galaxy, NGC 3147, and constraints on the progenitor system based on its early multicolor light-curve data. First, we classify SN 2021hpr as a normal SN Ia from its long-term photometric and spectroscopic data. More interestingly, we found a significant “early excess” in the light curve over a simple power-law ∼t 2 evolution. The early light curve evolves from blue to red to blue during the first week. To explain this, we fitted the early part of the BVRI-band light curves with a two-component model consisting of ejecta–companion interaction and a simple power-law model. The early excess and its color can be explained by shock-cooling emission due to a companion star having a radius of 8.84 ± 0.58 R ⊙. We also examined Hubble Space Telescope preexplosion images, finding no detection of a progenitor candidate, consistent with the above result. However, we could not detect signs of a significant amount of stripped mass from a nondegenerate companion star (≲0.003 M ⊙ for Hα emission). The early excess light in the multiband light curve supports a nondegenerate companion in the progenitor system of SN 2021hpr. At the same time, the nondetection of emission lines opens the door for other methods to explain this event.