SN2023fyq：一颗因双星相互作用而具有长期前身星活动的Ibn型超新星
SN2023fyq: A Type Ibn Supernova With Long-standing Precursor Activity Due to Binary Interaction
AI总结：
本文研究Ibn型超新星SN 2023fyq，发现其长期前身星活动源于双星质量转移，抛射物与赤道盘相互作用产生主峰，构成双星起源的独特超新星类别。
摘要：
我们展示了SN 2023fyq的光度和光谱观测，这是一颗位于邻近星系NGC 4388（距离D≃18 Mpc）中的Ibn型超新星。此外，我们利用DLT40、ATLAS、ZTF、ASAS-SN、Swift以及业余天文学家Koichi Itagaki的数据，追踪了SN 2023fyq位置处长期存在的前身星发射。前身星活动在超新星爆发前近三年内持续被观测到，并在最后100天内出现相对快速的上升。爆发后的双峰光变曲线达到约10^43 erg s^-1的光度。在SN 2023fyq的星云光谱中观测到的强中间宽度He线表明，相互作用在晚期阶段仍然活跃。我们发现，SN 2023fyq的前身星活动最好解释为包含一颗低质量He星和一颗致密伴星的双星系统中的质量转移。这一过程可能形成了一个赤道盘（约0.6 M_sun），而超新星抛射物与该盘的相互作用为超新星的主峰提供了能量。早期超新星光变曲线揭示了在爆发前数周抛射的致密延展物质（约0.3 M_sun）存在于约3000 R_sun处，这可能是由于核心硅燃烧的最后阶段或因双星轨道收缩导致的失控质量转移，从而在爆发前约30天内引起快速上升的前身星发射。最终的爆发可能是由He星的核心坍缩或He星与致密天体的并合触发。SN 2023fyq与SN 2018gjx和SN 2015G一起，构成了Ibn型超新星中的一个独特类别，它们起源于双星系统，并可能表现出可探测的、持续时间长的爆发前喷发，其星等范围从-10到-13。
英文摘要：
We present photometric and spectroscopic observations of SN 2023fyq, a type Ibn supernova in the nearby galaxy NGC 4388 (D$\simeq$18~Mpc). In addition, we trace long-standing precursor emission at the position of SN 2023fyq using data from DLT40, ATLAS, ZTF, ASAS-SN, Swift, and amateur astronomer Koichi Itagaki. Precursor activity is observed up to nearly three years before the supernova explosion, with a relatively rapid rise in the final 100 days. The double-peaked post-explosion light curve reaches a luminosity of $\sim10^{43}~\rm erg\,s^{-1}$. The strong intermediate-width He lines observed in the nebular spectrum of SN 2023fyq imply the interaction is still active at late phases. We found that the precursor activity in SN 2023fyq is best explained by the mass transfer in a binary system involving a low-mass He star and a compact companion. An equatorial disk is likely formed in this process ($\sim$0.6$\rm M_{\odot}$), and the interaction of SN ejecta with this disk powers the main peak of the supernova. The early SN light curve reveals the presence of dense extended material ($\sim$0.3$\rm M_{\odot}$) at $\sim$3000$\rm R_{\odot}$ ejected weeks before the SN explosion, likely due to final-stage core silicon burning or runaway mass transfer resulting from binary orbital shrinking, leading to rapid rising precursor emission within $\sim$30 days prior to explosion. The final explosion could be triggered either by the core-collapse of the He star or by the merger of the He star with a compact object. SN 2023fyq, along with SN 2018gjx and SN 2015G, forms a unique class of Type Ibn SNe which originate in binary systems and are likely to exhibit detectable long-lasting pre-explosion outbursts with magnitudes ranging from $-$10 to $-$13.
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