SN 2025aedz：一颗具有快速峰值后下降的典型短平台IIP型超新星
SN 2025aedz: A typical short-plateau type IIP supernova with rapid post-peak decline
- Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）
- INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）
- Center for Astrophysics | Harvard & Smithsonian（哈佛史密森尼天体物理中心）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
本文报道了典型短平台IIP型超新星SN 2025aedz，其快速峰值后下降源于低质量氢包层前身星及星周相互作用，为红超巨星问题提供观测约束。
AI中文摘要：
IIP型超新星（SNe IIP）是观测中核坍缩超新星最常见的亚类。然而，具有数十天量级短平台的IIP型超新星很少被观测到。这类超新星的前身星有助于解决恒星演化中的红超巨星问题。在本文中，我们报告了SN 2025aedz的光学测光和光谱观测，这是一颗具有典型短平台的快速峰值后下降的IIP型超新星。它的峰值绝对星等为$M_r=-17.16\pm0.03$等。其$r$波段光变曲线显示出陡峭的早期峰值后下降，速率约为$\sim5\\,\mathrm{mag}\\,(100\\,\mathrm{d})^{-1}$，随后是一个相对较短的平台期，平台持续时间为$\sim50\pm3$天。整体光谱演化与正常IIP型超新星一致，在光球层阶段显示出具有显著巴耳末P-Cygni轮廓的蓝色连续谱，随后随着抛射物冷却，氢和金属谱线逐渐增强，尽管金属谱线仍然较弱且膨胀速度迅速下降。SN 2025aedz在整体演化上与短平台超新星SN 2018gj相似，而其显著的早期下降则类似于目前已知平台持续时间最短的SN 2023ufx。热核光变曲线的放射性尾部暗示合成的$^{56}$Ni质量约为$\sim0.03\pm0.01\\,M_\odot$。受陡峭早期下降的启发，我们通过探索不同的星周物质构型进行了辐射流体动力学模拟，以重现其早期热核光变曲线。这些模拟表明，SN 2025aedz起源于一个具有相对低质量氢包层的前身星，可能是通过增强的质量损失或双星相互作用产生的，而陡峭的早期下降则可能由星周相互作用的额外光度来解释。
英文摘要：
Type IIP supernovae (SNe IIP) are the most common subclass of core-collapse SNe in observations. However, SNe IIP with short plateaus of the order of tens of days are rarely observed. The progenitors for this kind of SN can help to address the red supergiant issue in stellar evolution. In this article, we report optical photometry and spectroscopy of SN\,2025aedz, a rapidly post-peak declining SN IIP with a typical short plateau. It exhibits a peak absolute magnitude of $M_r=-17.16\pm0.03$\,mag. The $r$-band light curve shows a steep early post-peak decline of $\sim5\,\mathrm{mag}\,(100\,\mathrm{d})^{-1}$ followed by a relatively short plateau, with a plateau duration of $\sim50\pm3$\,d. The overall spectral evolution is consistent with that of normal SNe~IIP, showing a blue continuum with prominent Balmer P-Cygni profiles during the photospheric phase, followed by the gradual strengthening of hydrogen and metal lines as the ejecta cools down, although the metal lines remain weak and the expansion velocities decline rapidly. SN\,2025aedz is similar to the short-plateau SN\,2018gj in its overall evolution, whereas its pronounced early decline resembles that of SN\,2023ufx, which has the shortest plateau duration known so far. The radioactive tail of the bolometric light curve implies a synthesized $^{56}$Ni mass of $\sim0.03\pm0.01\,M_\odot$. Motivated by the steep early decline, we performed radiation hydrodynamic simulations by exploring different circumstellar material configurations to reproduce its early bolometric light curve. These simulations indicate that SN\,2025aedz originated from a progenitor with a relatively low-mass hydrogen envelope, possibly produced through enhanced mass loss or binary interaction, while the steep early decline is likely explained by additional luminosity from circumstellar interaction.
