SN 2018hna: 1987A-like Supernova with a Signature of Shock Breakout
SN 2018hna: 1987A-like Supernova with a Signature of Shock Breakout
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DOI：
10.3847/2041-8213/ab3d44
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发表时间：
2019-08
期刊：
影响因子：
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通讯作者：
Anuradha Singh;D. Sahu;G. Anupama;B. Kumar;H. Kumar;M. Yamanaka;P. Baklanov;N. Tominaga;S. Blinn
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文献类型：
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作者：
Anuradha Singh;D. Sahu;G. Anupama;B. Kumar;H. Kumar;M. Yamanaka;P. Baklanov;N. Tominaga;S. Blinn
本文给出了特殊的II型超新星2018hna的高频率紫外、光学和近红外光度和低分辨率光谱观测结果。早期的多波段光曲线显示了从爆炸爆发到∼14d的绝热冷却包络发射。SN 2018hna在V波段的上升时间为∼88天，与SN 1987A相似。从SN 2018hna的测辐射热学LC推断其56Ni质量为∼0.087±0.004 M⊙。冷却相的流体动力学模拟表明，它是一个半径为∼50R⊙，质量为∼14-20M⊙，爆炸能量为∼1.72.9x1051erg的前驱粒子。前驱星体的半径比标准的红超巨星要小，这表明它是SN2018hna的蓝超巨星前体。在类1987A事件的低金属丰度环境下，推测了宿主星系UGc 07534的亚太阳金属丰度(∼0.3Z⊙)。
High-cadence ultraviolet, optical, and near-infrared photometric and low-resolution spectroscopic observations of the peculiar Type II supernova (SN) 2018hna are presented. The early-phase multiband light curves (LCs) exhibit the adiabatic cooling envelope emission following the shock breakout up to ∼ 14 days from the explosion. SN 2018hna has a rise time of ∼ 88 days in the V band, similar to SN 1987A. A 56Ni mass of ∼0.087 ± 0.004 M⊙ is inferred for SN 2018hna from its bolometric LC. Hydrodynamical modeling of the cooling phase suggests a progenitor with a radius ∼50 R⊙, a mass of ∼14–20 M⊙, and an explosion energy of ∼1.7–2.9 × 1051 erg. The smaller inferred radius of the progenitor than a standard red supergiant is indicative of a blue supergiant progenitor of SN 2018hna. A subsolar metallicity (∼0.3 Z⊙) is inferred for the host galaxy UGC 07534, concurrent with the low-metallicity environments of 1987A-like events.