Constraining Type Ia Supernova Progenitors via their Environments

通过环境限制 Ia 型超新星祖细胞

• 批准号: 2107070
• 负责人: Laura Chomiuk
• 金额: $ 45.92万
• 依托单位: Michigan State University
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2021
• 资助国家: 美国
• 起止时间: 2021-09-01 至 2025-08-31
• 项目状态: 未结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=2107070&HistoricalAwards=false
• 关键词: Constraining; Type; Ia; Supernova; Progenitors

Supernovae (SNe), or stellar explosions, are important astronomical events for many reasons: they produce and distribute heavy atomic elements into the galaxy, and they can be used as indicators of distances to far-away galaxies, which is vital for studying cosmology. One of the major unsolved problems in supernova science is the nature of the progenitor of the explosion. A research group at Michigan State University (MSU) will attempt to better understand SNe by investigating the circumstellar medium (CSM) around supernovae. The CSM records the history of mass-loss in the millennia prior to explosion, and therefore is a key to determining SN progenitors. The investigators will focus on detecting atomic line emission at ultraviolet (UV) wavelengths associated with the interaction shock from SN ejecta impacting a CSM shell. They will use UV image archival databases and interpret derived fluxes in the context of published shell-interaction models. As part of the project, the researchers will work with the Charles Drew Science Scholars program at MSU and the National Astronomy Consortium to involve undergraduate students from diverse backgrounds in summer and academic year research in supernova science.For Type Ia SNe, the CSM can reveal the identity of the mass-donor companion, which reveals the physics of both the binary interaction and supernova explosion. The single-degenerate (main sequence/red giant companion) and double-degenerate (white dwarf companion) channels are two dominant progenitor hypotheses. In recent years, SNe Ia have been discovered with detached shells of CSM that the ejecta impact months or years after explosion (i.e., delayed interaction). The origin of this material is unknown, but there are two likely possibilities which can distinguish between progenitor channels. In the single-degenerate channel, a SN may be preceded by multiple nova eruptions, which can form sub-solar-mass shells—while in the double-degenerate channel, a common envelope is expelled before the SN, forming a few-solar-mass shell. The investigators will search for more examples of delayed-interaction SNe Ia and use an appropriate theoretical framework to determine the range of properties of detached CSM shells. They will interpret derived fluxes in the context of published shell-interaction models, and will calculate the UV and optical emission line signals from the models to produce a grid of light curves whose luminosity and duration depend on the CSM mass, radius, extent, and geometry. By comparing these simulated light curves to data, they will calculate the probability of SNe Ia hosting CSM shells across a range of CSM properties. This will provide the most stringent constraints on the presence and properties of CSM shells around SNe Ia to date, and provide a rigorous test of the hypothesis that SNe Ia can occur while the ejected common envelope is still in the system.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)或恒星爆炸是重要的天文事件，原因有很多：它们产生重原子元素并将其分配到星系中，它们可以用作到遥远星系的距离指示器，这对研究宇宙学至关重要。超新星科学中尚未解决的主要问题之一是爆炸的先驱的性质。密歇根州立大学(MSU)的一个研究小组将试图通过研究超新星周围的星周介质(CSM)来更好地理解SNE。CSM记录了爆炸前数千年的质量损失历史，因此是确定SN前体的关键。调查人员将专注于探测与锡喷出物撞击CSM壳的相互作用激波相关的紫外线(UV)波长的原子线发射。他们将使用紫外线图像档案数据库，并在已发表的贝壳相互作用模型的背景下解释导出的通量。作为该项目的一部分，研究人员将与密歇根州立大学的查尔斯·德鲁科学学者计划和国家天文学联合会合作，让来自不同背景的本科生参加夏季和学年的超新星科学研究。对于Ia型SNE，CSM可以揭示质量捐赠者的身份，这揭示了双星相互作用和超新星爆炸的物理学。单简并(主序/红巨星伴生)和双简并(白矮星伴生)通道是两种主要的前身假说。近年来，在分离的CSM弹壳中发现了SneIa，它们在爆炸数月或数年后撞击(即延迟相互作用)。这种物质的来源尚不清楚，但有两种可能的可能性可以区分祖细胞通道。在单简并通道中，SN之前可能有多次新星爆发，形成亚太阳质量的壳层，而在双简并通道中，公共包层在SN之前被逐出，形成几个太阳质量的壳层。研究人员将寻找更多延迟相互作用SNE Ia的例子，并使用适当的理论框架来确定分离的CSM炮弹的性质范围。他们将在已发表的壳层相互作用模型的背景下解释推导出的通量，并将计算模型中的UV和光学发射线信号，以产生其光度和持续时间取决于CSM质量、半径、范围和几何形状的灯光曲线网格。通过将这些模拟的光曲线与数据进行比较，他们将计算SNE Ia托管一系列CSM属性的CSM壳的概率。这将对SNE Ia周围CSM炮弹的存在和性能提供迄今为止最严格的限制，并对SNE Ia可能在被弹出的公共信封仍在系统中时发生的假设进行严格测试。该奖项反映了NSF的法定使命，并通过使用基金会的智力优势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

The fastest stars in the Galaxy

• DOI: 10.21105/astro.2306.03914
• 发表时间: 2023-06
• 期刊: The Open Journal of Astrophysics
• 作者: K. El-Badry;K. Shen;V. Chandra;E. Bauer;J. Fuller;J. Strader;L. Chomiuk;R. Naidu;I. Caiazzo;Antonio C. Rodriguez;Pranav Nagarajan-;Natsuko Yamaguchi;Z. Vanderbosch;B. Roulston;J. Roestel;B. Gansicke;Jiwon Jesse Han;K. Burdge;A. Filippenko;T. Brink;W. Zheng

Synchrotron emission from double-peaked radio light curves of the symbiotic recurrent nova V3890 Sagitarii

共生循环新星 V3890 Sagitarii 双峰射电光变曲线的同步辐射

• DOI: 10.1093/mnras/stad1534
• 发表时间: 2023
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Nyamai, Miriam M.;Linford, Justin D.;Allison, James R.;Chomiuk, Laura;Woudt, Patrick A.;Ribeiro, Valério A. R. M.;Sarbadhicary, Sumit K.
• 通讯作者: Sarbadhicary, Sumit K.

Radio Observations of Six Young Type Ia Supernovae

• DOI: 10.3847/1538-4357/acd84f
• 发表时间: 2023-05
• 期刊: The Astrophysical Journal
• 作者: C. Harris;S. Sarbadhicary;L. Chomiuk;A. Piro;D. Sand;S. Valenti

Catching a nova X-ray/UV flash in the visible? Early spectroscopy of the very slow Nova Velorum 2022 (Gaia22alz)

在可见光中捕捉到新星 X 射线/紫外线闪光？

• DOI: 10.1093/mnras/stad1914
• 发表时间: 2023
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Aydi, E.;Chomiuk, L.;Mikołajewska, J.;Brink, J.;Metzger, B. D.;Strader, J.;Buckley, D. A. H.;Harvey, E. J.;Holoien, T. W. -S;Izzo, L.
• 通讯作者: Izzo, L.