Endurance of SN 2005ip after a decade: X-rays, radio, and H-alpha like SN 1988Z require long-lived pre-supernova mass loss
Nathan Smith, Charles D. Kilpatrick, Jon C. Mauerhan, Jennifer E. Andrews, Raffaella Margutti, Wen-Fai Fong, Melissa L. Graham, WeiKang Zheng, Patrick L. Kelly,… 展开作者
Nathan Smith, Charles D. Kilpatrick, Jon C. Mauerhan, Jennifer E. Andrews, Raffaella Margutti, Wen-Fai Fong, Melissa L. Graham, WeiKang Zheng, Patrick L. Kelly, Alexei V. Filippenko, Ori D. Fox
SN2005ip was a TypeIIn event notable for its sustained strong interaction with circumstellar material (CSM), coronal emission lines, and IR excess, interpreted as shock interaction with the very dense and clumpy wind of an extreme red supergiant. We present a series of late-time spectra of SN2005ip and a first radio detection of this SN, plus late-time X-rays, all of which indicate that its CSM interaction is still strong a decade post-explosion. We also present and discuss new spectra of geriatric SNe with continued CSM interaction: SN1988Z, SN1993J, and SN1998S. From 3-10 yr post-explosion, SN2005ip's H-alpha luminosity and other observed characteristics were nearly identical to those of the radio-luminous SN1988Z, and much more luminous than SNe1993J and 1998S. At 10 yr after explosion, SN2005ip showed a drop in H$α$ luminosity, followed by a quick resurgence over several months. We interpret this variability as ejecta crashing into a dense shell located at around 0.05 pc from the star, which may be the same shell that caused the IR echo at earlier epochs. The extreme H-alpha luminosities in SN2005ip and SN1988Z are still dominated by the forward shock at 10 yr post-explosion, whereas SN1993J and SN1998S are dominated by the reverse shock at a similar age. Continuous strong CSM interaction in SNe~2005ip and 1988Z is indicative of enhanced mass loss for about 1e3 yr before core collapse, longer than Ne, O, or Si burning phases. Instead, the episodic mass loss must extend back through C burning and perhaps even part of He burning.
SN 2024dy: Dust formation in a long-lived Type IIn supernova and constraints on the dust mass
Kagoshima University（鹿儿岛大学）；Hiroshima University（广岛大学）；Tohoku University（东北大学）；Stockholm University（斯德哥尔摩大学）；Indian Institute of Astrophysics（印度天体物理研究所）
Nucleosynthesis of an $11.8\,M_\odot$ Supernova with 3D Simulation of the Inner Ejecta: Overall Yields and Implications for Short-Lived Radionuclides in the Early Solar System
SN 2019vxm: A luminous and long-lived Type IIn supernova with early flash-ionisation features
Tsinghua University（清华大学）；Yunnan Observatories, Chinese Academy of Sciences (CAS)（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）；National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台，国立自然科学研究院）；Graduate Institute for Advanced Studies, SOKENDAI（综合研究大学院大学（SOKENDAI））；School of Physics and Astronomy, Monash University（蒙纳士大学物理与天文学院）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；Department of Astronomy, University of California, Berkeley（加州大学伯克利分校天文学系）
SN 2019vxm是一颗峰值亮度高、演化缓慢的IIn型超新星，早期光谱显示闪光电离特征，后期红外超表明新尘埃形成，其光变曲线与SN 2010jl相似。
DES16C3cje: A low-luminosity, long-lived supernova
本文介绍了暗能量巡天（DES）观测到的一颗低光度、长寿命的II型超新星（SN II），红移为0.0618。DES16C3cje是唯一的SN。光谱的特征是极窄的光球线对应于非常低的膨胀速度$\lesssim1500$ km s $^{-1}$，并且光变曲线显示了在50天后衰减的初始峰值，然后在另外的100天内缓慢地重新变亮，以达到M $_r\sim -15.5$ mag的绝对亮度。时间光变曲线则慢于由$^{56}$ Co的放射性衰变供电所预期的时间光变曲线，但与由吸积功率所预期的时间光变曲线相当。通过比较测辐射热光变曲线和流体动力学模型，我们发现DES16C3cje可以用以下两种解释：i）低爆炸能量（0.11 foe）和相对较大的$^{56}$ Ni生产0.075 M $_{\odot}$，来自其他SNe II典型的$\sim15$ M $_{\odot}$红超巨星祖先，或ii）相对紧凑的$\sim40$ M $_{\odot}$恒星，爆炸能量为1 foe，和0.08 M $_{\odot}$的$^{56}$ Ni。这两种情况都需要额外的能量输入来解释后期光变曲线，这与以$\sim0.5\times{10^{-8}}$ M $_{\odot}$ s $^{-1}$的速率的回退吸积一致。
Signatures of Circumstellar Interaction in the Type IIL Supernova ASASSN-15oz
富氢、核心坍缩的超新星通常分为四类：IIP、IIL、IIn和IIb。一般来说，与星周物质的相互作用只被认为是IIn型超新星。然而，最近对IIP和IIL超新星的流体动力学建模需要星周物质来重现它们早期的光变曲线。在这种情况下，IIL超新星在爆炸前经历了大量的质量损失。我们在ASASSN-15 oz上测试了这一假设，这是一颗IIL型超新星。随着X射线、紫外线、光学、红外线和无线电的广泛跟踪，我们提出了我们对相互作用迹象的搜索，以及由它们的检测所指示的质量损失历史。我们发现的证据表明，短暂的激烈的质量损失之前，爆炸的光变曲线建模，相当于在1.5 M $_{\odot}$的材料在1800 R $_{\odot}$的祖先。我们还检测到超新星的无线电，表明质量损失率$10^{-6}-10^{-7}$ M $_{\odot}$年$^{-1}$之前的极端质量损失期。我们未能在X射线中探测到这颗超新星，在紫外线、可见光和近红外线中也没有窄的发射谱线，这些都与这幅图并不矛盾，并在$<10^{-4}$ M $_{\odot}$ yr $^{-1}$的极端周期之外设定了质量损失率的上限。本文强调了收集更多II型超新星的全面数据的重要性，以便详细建模的祖星和超新星，可以阐明他们的质量损失历史和包络结构，从而告知恒星演化模型。
A steadily declining dispersion measure for the repeating fast radio burst FRB 20220529A: Evidence for an FRB engine embedded in an expanding supernova remnant
McGill University（麦吉尔大学）；University of Toronto（多伦多大学）；Northwestern University（西北大学）；Massachusetts Institute of Technology（麻省理工学院）
Quantifying Element Importance for Mass Recovery from Population III Supernova Yield Fits
University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；NSF-Simons AI Institute for the Sky (SkAI)（美国国家科学基金会-西蒙斯天空人工智能研究所）；NSF NOIRLab（美国国家科学基金会NOIR天文台）；Oregon State University（俄勒冈州立大学）
The bright long-lived Type II SN 2021irp powered by aspherical circumstellar material interaction (I): Revealing the energy source with photometry and spectroscopy
