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由非球对称星周物质相互作用供能的明亮长寿命II型超新星SN 2021irp（I）：利用测光与光谱揭示能量来源

The bright long-lived Type II SN 2021irp powered by aspherical circumstellar material interaction (I): Revealing the energy source with photometry and spectroscopy

T. M. Reynolds, T. Nagao, R. Gottumukkala, C. P. Gutiérrez, T. Kangas, T. Kravtsov, H. Kuncarayakti, K. Maeda, N. Elias-Rosa, M. Fraser, R. Kotak, S. Mattila, A… 展开作者

T. M. Reynolds, T. Nagao, R. Gottumukkala, C. P. Gutiérrez, T. Kangas, T. Kravtsov, H. Kuncarayakti, K. Maeda, N. Elias-Rosa, M. Fraser, R. Kotak, S. Mattila, A. Pastorello, P. J. Pessi, Y. -Z. Cai, J. P. U. Fynbo, M. Kawabata, P. Lundqvist, K. Matilainen, S. Moran, A. Reguitti, K. Taguchi, M. Yamanaka

备注：
23 pages, 16 figures, submitted to A&A
发表信息：
A&A 702, A212 (2025)
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AI总结：

本研究通过测光与光谱观测发现明亮长寿命II型超新星SN 2021irp的能量来自与非对称大质量星周物质的相互作用，同时分析了相关尘埃的特性。

摘要：

部分核坍缩超新星（CCSNe）亮度过高且总辐射能量过大，无法仅靠抛射物的热能释放以及合成的$^{56}$Ni/$^{56}$Co的放射性衰变能量供能。额外能量的一个来源是超新星（SN）抛射物与大质量星周物质（CSM）之间的相互作用。这是IIn型超新星的重要供能机制，这类超新星会呈现由未受激波冲击的CSM产生的窄谱线，但并非所有存在相互作用的超新星都有这类窄线。我们展示了富氢超新星SN 2021irp的测光与光谱观测结果，该超新星亮度极高，$M_{o} < -19.4$星等，且寿命很长，亮度保持在$M_{o} = -18$星等以上的时长约为250天。我们证明这类超新星需要额外能量源供能，并确定了该能量源的性质。我们还研究了与该超新星相关的原有尘埃和新形成尘埃的特性。测光观测显示，该超新星的光度比典型II型超新星高一个数量级，且持续时间长得多。我们探测到归因于尘埃发射的红外超。光谱显示多成分谱线轮廓、Fe II假连续谱，且缺乏吸收线，这些都是IIn型超新星的典型特征。我们探测到与未受激波冲击的CSM相关的窄（< 85 km s$^{-1}$）P-Cygni轮廓。发射线轮廓的不对称性表明尘埃形成发生在250-300天期间。对超新星黑体半径演化的分析表明，发射区域的形状存在不对称性。我们确定SN 2021irp的主要能量来源是与大质量CSM的广泛相互作用，且该CSM在前身星周围呈非对称分布。红外超可以用新形成尘埃的发射来解释，不过也有一些证据表明早期存在来自原有尘埃的红外回波。

英文摘要：

Some core-collapse supernovae (CCSNe) are too luminous and radiate too much total energy to be powered by the release of thermal energy from the ejecta and radioactive-decay energy from the synthesised $^{56}$Ni/$^{56}$Co. A source of additional power is the interaction between the supernova (SN) ejecta and a massive circumstellar material (CSM). This is an important power source in Type IIn SNe, which show narrow spectral lines arising from the unshocked CSM, but not all interacting SNe show such narrow lines. We present photometric and spectroscopic observations of the hydrogen-rich SN 2021irp, which is both luminous, with $M_{o} < -19.4$ mag, and long-lived, remaining brighter than $M_{o} = -18$ mag for $\sim$ 250 d. We show that an additional energy source is required to power such a SN, and determine the nature of the source. We also investigate the properties of the pre-existing and newly formed dust associated with the SN. Photometric observations show that the luminosity of the SN is an order of magnitude higher than typical Type II SNe and persists for much longer. We detect a infrared excess attributed to dust emission. Spectra show multi-component line profiles, an Fe II pseudo-continuum, and a lack of absorption lines, all typical features of Type IIn SNe. We detect a narrow (< 85 kms$^{-1}$) P-Cygni profile associated with the unshocked CSM. An asymmetry in emission line profiles indicates dust formation occurring from 250-300 d. Analysis of the SN blackbody radius evolution indicates asymmetry in the shape of the emitting region. We identify the main power source of SN 2021irp as extensive interaction with a massive CSM, and that this CSM is distributed asymmetrically around the progenitor star. The infrared excess is explained with emission from newly formed dust although there is also some evidence of an IR echo from pre-existing dust at early times.

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