Supernova Shock Wave and Radiative Interactions

超新星冲击波和辐射相互作用

• 批准号: 1814910
• 负责人: Roger Chevalier
• 金额: $ 35.97万
• 依托单位: University of Virginia Main Campus
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2018
• 资助国家: 美国
• 起止时间: 2018-08-15 至 2023-07-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1814910&HistoricalAwards=false
• 关键词: Supernova; Shock; Wave; Radiative; Interactions

Supernovae (SNe) are explosions that end the lives of massive stars. They are important to study since supernovae seed the galaxy with atomic elements made in the star and in the explosion, and they help astronomers to understand how stars evolve and die. One of the ways astronomers study supernovae is by observing how the matter ejected in the SNe interacts with the gaseous material surrounding the star, producing a shock wave. In order to help to interpret such observations, a research team at the University of Virginia will carry out a program to investigate the interaction of a supernova with a dense circumstellar medium. Their study will include hydrodynamic computer simulations, modeling of energy transfer in the form of electromagnetic radiation, and calculations of physical conditions in the shock. By better defining the nature of the circumstellar media involved in these events, this research seeks to fill gaps in stellar evolution theory. The principal investigator will give annual public lectures at the McCormick Observatory, near the university, as well as talks for elderly persons given at accessible sites. A graduate student and an undergraduate student will be involved in the research and will learn techniques used in theoretical astrophysics, as well as ways of approaching open questions. The goal of the project is to investigate the interaction of a supernova with a dense, possibly optically thick, circumstellar medium. The physical conditions are more extreme than ordinarily encountered in supernova interactions and the structure of the mass loss region is probably complex. The researchers will develop diagnostics for the conditions in and structure of the interaction. Specific topics that will be addressed include the shock wave structure and hydrodynamic instabilities when cooling is important, consistent models for X-ray and ultraviolet/optical shock emission, pre-shock ionization and emission, nonthermal particles and radio emission and absorption, and infrared emission from the radiative heating of dust. The models will be compared to multiwavelength observations, from radio to X-rays. The research will relate the findings for observed interacting supernovae to plausible mechanisms for driving the pre-supernova mass loss. Supernovae that have narrow line characteristics are inferred to have a dense, slow moving circumstellar medium. These characteristics are observed over a broad range of supernova types, including those with and without hydrogen lines, superluminous supernovae, supernovae with Type Ia characteristics, and possible low energy supernovae. For these events, neither the mechanism driving the mass loss nor the timing with the supernova is understood, although narrow line supernovae make up about 9% of Type II supernovae. By better defining the nature of the circumstellar media involved in these events, this research seeks to fill gaps in stellar evolution theory. In addition, aspects of the physical processes in dense media should be more broadly applicable, for example to the dense media in active galactic nuclei.This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.

超新星（SNe）是终结大质量恒星生命的爆炸。 它们是重要的研究，因为超新星种子星系与原子元素在星星和爆炸，他们帮助天文学家了解恒星如何演变和死亡。 天文学家研究超新星的方法之一是观察SNe中喷出的物质如何与星星周围的气体物质相互作用，产生冲击波。 为了帮助解释这些观测结果，弗吉尼亚大学的一个研究小组将开展一项计划，调查超新星与致密的星周介质的相互作用。 他们的研究将包括流体动力学计算机模拟，电磁辐射形式的能量转移建模，以及冲击中物理条件的计算。 通过更好地定义这些事件中所涉及的星周介质的性质，这项研究旨在填补恒星演化理论的空白。首席研究员将在大学附近的麦考密克天文台举行年度公开讲座，并在无障碍场所为老年人举行讲座。一名研究生和一名本科生将参与研究，并将学习理论天体物理学中使用的技术，以及解决开放性问题的方法。该项目的目标是研究超新星与致密的、可能是光学厚的星周介质的相互作用。物理条件比通常在超新星相互作用中遇到的更极端，质量损失区域的结构可能很复杂。研究人员将开发诊断的条件和结构的相互作用。具体的主题，将被解决包括冲击波结构和流体动力学不稳定性时，冷却是重要的，一致的模型，X射线和紫外线/光学冲击发射，预冲击电离和发射，非热粒子和无线电发射和吸收，以及红外辐射加热的尘埃发射。这些模型将与从无线电到X射线的多波长观测进行比较。 这项研究将把观察到的相互作用的超新星的发现与驱动超新星前质量损失的合理机制联系起来。具有窄谱线特征的超新星被推断为具有致密、缓慢移动的星周介质。这些特征在广泛的超新星类型中被观察到，包括那些有和没有氢线的超新星，超亮超新星，具有Ia型特征的超新星，以及可能的低能量超新星。对于这些事件，无论是驱动质量损失的机制还是超新星的时间都不清楚，尽管窄线超新星占II型超新星的9%。通过更好地定义这些事件中所涉及的星周介质的性质，这项研究旨在填补恒星演化理论的空白。此外，稠密介质中的物理过程的各个方面应该更广泛地适用，例如活动星系核中的稠密介质。该奖项反映了NSF的法定使命，并通过使用基金会的知识价值和更广泛的影响审查标准进行评估，被认为值得支持。

项目成果

Supernova Interaction with a Dense Detached Shell in SN 2001em

• DOI: 10.3847/1538-4357/abb460
• 发表时间: 2020-08
• 期刊: The Astrophysical Journal
• 作者: P. Chandra;R. Chevalier;N. Chugai;D. Milisavljevic;C. Fransson

Evidence for a Pulsar Wind Nebula in the Type Ib Peculiar Supernova SN 2012au

• DOI: 10.3847/2041-8213/aadd4e
• 发表时间: 2018-09
• 期刊: The Astrophysical Journal Letters
• 作者: D. Milisavljevic;D. Patnaude;R. Chevalier;J. Raymond;R. Fesen;R. Margutti;Brody Conner;J. Banovetz

The Matter Beyond the Ring: The Recent Evolution of SN 1987A Observed by the Hubble Space Telescope

• DOI: 10.3847/1538-4357/ab4ff2
• 发表时间: 2019-10
• 期刊: The Astrophysical Journal
• 作者: J. Larsson;C. Fransson;D. Alp;P. Challis;R. Chevalier;R. Kirshner;R. Kirshner;Stephen S. Lawrence;B. Leibundgut;P. Lundqvist;S. Mattila;K. Migotto;J. Sollerman;G. Sonneborn;J. Spyromilio;N. Suntzeff;J. Wheeler

The luminous type IIn supernova SN 2017hcc: Infrared bright, X-ray, and radio faint

发光型 IIn 超新星 SN 2017hcc：红外亮光、X 射线和射电微弱

• DOI: 10.1093/mnras/stac2915
• 发表时间: 2022
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Chandra, Poonam;Chevalier, Roger A.;James, Nicholas J. H.;Fox, Ori D.
• 通讯作者: Fox, Ori D.

Detection of the Red Supergiant Wind from the Progenitor of Cassiopeia A

仙后座 A 前身红超巨星风的探测

• DOI: 10.3847/1538-4357/ab76bf
• 发表时间: 2020
• 期刊: The Astrophysical Journal
• 作者: Weil, Kathryn E.;Fesen, Robert A.;Patnaude, Daniel J.;Raymond, John C.;Chevalier, Roger A.;Milisavljevic, Dan;Gerardy, Christopher L.
• 通讯作者: Gerardy, Christopher L.