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arXiv 2102.08121astro-ph.SRastro-ph.HE
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SN 2017 hpa：一颗富碳Ia型超新星

SN 2017hpa: A carbon-rich type Ia supernova

Anirban Dutta, Avinash Singh, G. C. Anupama, D. K. Sahu, Brajesh Kumar

备注：
15 pages, 13 figures, Accepted for publication in MNRAS
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摘要：

本文介绍了Ia型超新星SN 2017 hpa的光学（UBVRI）和紫外（Swift-UVOT）测光以及光谱学。我们研究了从$B$ -带的最大光起，从$-13.8$到$+108$ ~d的宽波段紫外光变曲线和低分辨光谱。光度分析表明SN 2017 hpa是一个正常的Ia型超新星，具有$Δm_{B}(15) = 0.98\pm0.16$等和$M_{B}=-19.45\pm0.15$等，距离模数为$μ= 34.08\pm0.09$等。$(uvw1-uvv)$的颜色演变表明SN 2017 hpa属于NUV-蓝群。$(B-V)$的最大颜色比正常的Ia型超新星更蓝。光谱分析表明，Si II 6355的吸收功能迅速演变的速度梯度，$\dot{v}=128\pm 7$ km s $^{-1}$ d $^{-1}$。最大前相位谱显示出明显的C Ⅱ 6580吸收特征。从观测到的光谱中测得的C II 6580的线速度低于Si II 6355的线速度，这可能是由于视线效应。合成光谱拟合到使用syn++的前最大光谱表明除了光球分量之外，在Si II吸收中存在高速分量。用光谱合成程序TARDIS对观测光谱进行拟合，估算出喷出物中未燃碳的质量为$\sim 0.019$ ~ $M_{\odot}$。峰值辐射热光度为$L^{bol}_{peak} = 1.43\times10^{43}$ erg s $^{-1}$。辐射扩散模型拟合的测热光变曲线表明，在爆炸过程中生成了$^{56}$ Ni的$0.61\pm0.02$ $M_\odot$。

英文摘要：

We present the optical (UBVRI) and ultraviolet (Swift-UVOT) photometry, and optical spectroscopy of Type Ia supernova SN 2017hpa. We study broadband UV+optical light curves and low resolution spectroscopy spanning from $-13.8$ to $+108$~d from the maximum light in $B$-band. The photometric analysis indicates that SN 2017hpa is a normal type Ia with $Δm_{B}(15) = 0.98\pm0.16$ mag and $M_{B}=-19.45\pm0.15$ mag at a distance modulus of $μ= 34.08\pm0.09$ mag. The $(uvw1-uvv)$ colour evolution shows that SN 2017hpa falls in the NUV-blue group. The $(B-V)$ colour at maximum is bluer in comparison to normal type Ia supernovae. Spectroscopic analysis shows that the Si II 6355 absorption feature evolves rapidly with a velocity gradient, $\dot{v}=128\pm 7$ km s$^{-1}$ d$^{-1}$. The pre-maximum phase spectra show prominent C II 6580 Å absorption feature. The C II 6580 Å line velocity measured from the observed spectra is lower than the velocity of Si II 6355 Å, which could be due to a line of sight effect. The synthetic spectral fits to the pre-maximum spectra using syn++ indicate the presence of a high velocity component in the Si II absorption, in addition to a photospheric component. Fitting the observed spectrum with the spectral synthesis code TARDIS, the mass of unburned C in the ejecta is estimated to be $\sim 0.019$~$M_{\odot}$. The peak bolometric luminosity is $L^{bol}_{peak} = 1.43\times10^{43}$ erg s$^{-1}$. The radiation diffusion model fit to the bolometric light curve indicates $0.61\pm0.02$ $M_\odot$ of $^{56}$Ni is synthesized in the explosion.

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