论文标题
SN 2018GK重新访问：光球，中央引擎和推定的灰尘
SN 2018gk Revisited: the Photosphere, the Central Engine, And the Putative Dust
论文作者
论文摘要
在本文中，我们对SN 2018GK的物理特性进行了全面研究，该研究是发光的IIB型超新星（SN）。我们发现，早期光电速度从较大的值到光球到达温度地面之前的值不等。我们概括了光球模量，并适合SN 2018GK的多频光曲线（LCS）。我们发现$^{56} $ ni质量模型需要$ \ sim0.90 $ m $ m $ _ \ odot $ of $^{56} $ ni，该$比派生的exjecta smos（$ \ sim0.10 $ m $ _ $ _ \ odot $）大。另外，我们使用Magnetar Plus $^{56} $ Ni和后备和$^{56} $ NI型号来适合SN 2018GK的LCS，发现这两种型号可以适合LCS。由于参数相当合理（$ m _ {\ rm ej} = 1.65 $ m $ _ \ odot $，$ m _ {\ rm ni} = 0.05 $ m $ m $ _ \ odot $ y比ys $ syn的$ ni，$ ni是$ ni，我们偏爱磁铁和$^{56} $ ni。由中微子驱动的核心崩溃Sne $ b = 6.52 \ times10^{14} $ g可与文献中研究的发光和超弱的sne相当，而$ p_0 = 10.42 $ ms，可与发光的sne相当），而shallback plus $^{56 $ ni $ ni $ ni $ ni $ ni $ ni $ ni的有效性相当。因此，我们建议SN 2018GK可能是主要由中央发动机提供动力的SN IIB。最后，我们在某些时期确认了SN 2018GK的光谱能量分布（SED）的NIR过量，并使用黑体加上灰尘发射模型来限制假定灰尘的物理特性。
In this paper, we perform a comprehensive study for the physical properties of SN 2018gk which is a luminous type IIb supernova (SN). We find that the early-time photospheric velocity vary from a larger value to a smaller value before the photosphere reach a temperature floor. We generalize the photosphere modulus and fit the multi-band light curves (LCs) of SN 2018gk. We find that the $^{56}$Ni mass model require $\sim0.90$ M$_\odot$ of $^{56}$Ni which is larger than the derived ejecta mass ($\sim0.10$ M$_\odot$). Alternatively, we use the magnetar plus $^{56}$Ni and the fallback plus $^{56}$Ni models to fit the LCs of SN 2018gk, finding that the two models can fit the LCs. We favor the magnetar plus $^{56}$Ni since the parameters are rather reasonable ($M_{\rm ej} =1.65$ M$_\odot$, $M_{\rm Ni}=0.05$ M$_\odot$ which is smaller than the upper limit of the value of the $^{56}$Ni mass can by synthesized by the neutrino-powered core collapse SNe $B=6.52\times10^{14}$ G which is comparable to those of luminous and superluminous SNe studied in the literature, and $P_0=10.42$ ms which is comparable to those of luminous SNe), while the validity of the fallback plus $^{56}$Ni model depends on the accretion efficiency ($η$). Therefore, we suggest that SN 2018gk might be a SN IIb mainly powered by a central engine. Finally, we confirm the NIR excesses of the spectral energy distributions (SEDs) of SN 2018gk at some epochs and constrain the physical properties of the putative dust using the blackbody plus dust emission model.
