Collaborative Research: Searching for the Expelled Envelope of Stripped-Envelope Supernovae

合作研究：寻找剥离包层超新星的驱逐包层

• 批准号: 1813825
• 负责人: John Wheeler
• 金额: $ 46.37万
• 依托单位: University of Texas at Austin
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2018
• 资助国家: 美国
• 起止时间: 2018-09-01 至 2024-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1813825&HistoricalAwards=false
• 关键词: Collaborative; Research; Searching; Expelled; Envelope

Astronomers study supernovae because the maximum luminosity of a stellar catastrophe can equal that of a billion suns, which is an awesome spectacle to see. By studying which stars become supernovae, we gain new insights into the course of the stellar life cycle. The explosion causes the star to expand and thin out, and this allows us to see ever deeper into the exploding matter. Matter is thrown into space at a few percent of the speed of light. When this happens, astronomers can read the signals from the outer layers of the stars and probe the nature of the star both before and after it exploded. Through these observations, we gain new insight into the formation of compact objects, such as neutron stars and black holes. The ejected matter is enriched in new elements, and thus, Supernovae are principal drivers of the nuclear evolution of the Universe. Supernovae are also an important factor in the physical structure and composition of galaxies. The energy released by supernovae may stimulate or inhibit the formation of stars. Supernovae may also eject matter from galaxies in supernova-heated galactic winds. Additionally, Supernovae serve as exquisite indicators of extragalactic distances. Through the study of Supernovae, we can determine the history of the cosmic expansion.A major issue in supernova research is determining how stars shed mass prior to explosion. The investigators will study the interaction of the exploding star, when the explosion collides with matter that was expelled before the explosion. Deeper understanding of these issues will expand our knowledge of how and when stars eject matter. The investigators seek to determine whether stars have multiple episodes of mass loss. They also want to know how the loss of mass alters the distribution of matter around the star. To better understand these questions, the investigators will study select stars that contain no hydrogen by the time they explode as supernovae because this means either the stars have expelled all their hydrogen-rich material into space or a companion star has accreted it. The investigators will also determine how the strength of the collision varies in time because the collision properties are related to the nature of the underlying supernova.This research project will help further our understanding of our place in the Universe. It will serve to train young scientists in the STEM fields. It will promote deeper understanding of science in the public. It will be accompanied by broad outreach in appropriate venues for writing and speaking.The investigators use the 2.7m Harlan J. Smith telescope at McDonald Observatory, in Texas, to search for the collision of supernovae. Narrow-band filters permit a rapid search for emission of hydrogen features that signify the presence of the collision of the supernova with previously-expelled hydrogen-rich material. The narrow-band filter observations also indicate variations in the strength of the hydrogen emission, which is a further clue to the nature of the interaction. The investigators will continue studies of collisions with the Hobby-Eberly Telescope to confirm that the hydrogen emission is from shocked material and not from ambient concentrations of hydrogen in the interstellar medium. They perform observations at other wavelengths, including the use of the NSF's Very Large Array radio observatory, to further constrain the properties - temperature and density - of the shocked material.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.

天文学家研究超新星是因为恒星灾难的最大亮度可以相当于10亿个太阳，这是一个令人敬畏的奇观。通过研究哪些恒星会成为超新星，我们对恒星生命周期的过程有了新的认识。爆炸导致恒星膨胀和变薄，这使我们能够更深入地观察爆炸的物质。物质以光速的百分之几被抛入太空。当这种情况发生时，天文学家可以读取来自恒星外层的信号，并探测恒星爆炸前后的性质。通过这些观测，我们对致密物体的形成有了新的认识，比如中子星和黑洞。喷出的物质富含新元素，因此，超新星是宇宙核演化的主要驱动力。超新星也是星系物理结构和组成的重要因素。超新星释放的能量可能刺激或抑制恒星的形成。超新星也可能在超新星加热的星系风中从星系中喷射出物质。此外，超新星是银河系外距离的精确指示器。通过对超新星的研究，我们可以确定宇宙膨胀的历史。超新星研究的一个主要问题是确定恒星在爆炸前是如何脱落质量的。研究人员将研究爆炸恒星与爆炸前排出的物质发生碰撞时的相互作用。对这些问题的深入了解将扩大我们对恒星如何以及何时喷射物质的认识。研究人员试图确定恒星是否有多次质量损失。他们还想知道质量的损失是如何改变恒星周围物质分布的。为了更好地理解这些问题，研究人员将研究那些在超新星爆炸时不含氢的恒星，因为这意味着要么这些恒星将所有富含氢的物质驱逐到太空中，要么是一颗伴星吸积了这些物质。研究人员还将确定碰撞强度如何随时间变化，因为碰撞特性与潜在超新星的性质有关。这个研究项目将有助于我们进一步了解我们在宇宙中的位置。它将用于培养STEM领域的年轻科学家。它将促进公众对科学更深层次的理解。与此同时，还将在适当的场所广泛开展写作和演讲活动。研究人员使用位于德克萨斯州麦克唐纳天文台的2.7米哈兰·j·史密斯望远镜来寻找超新星碰撞。窄带滤光片允许快速搜索氢发射的特征，这些特征表明超新星与先前释放的富氢物质碰撞的存在。窄带滤光器的观测也表明了氢发射强度的变化，这是进一步揭示相互作用本质的线索。研究人员将继续用霍比-埃伯利望远镜对碰撞进行研究，以确认氢发射来自受冲击的物质，而不是来自星际介质中氢的环境浓度。他们在其他波长进行观测，包括使用美国国家科学基金会的甚大阵列射电天文台，以进一步限制受冲击物质的性质——温度和密度。该奖项反映了美国国家科学基金会的法定使命，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

Interaction of SN Ib 2004dk with a Previously Expelled Envelope

SN Ib 2004dk 与先前排出的信封的相互作用

• DOI: 10.3847/1538-4357/ab3e36
• 发表时间: 2019
• 期刊: The Astrophysical Journal
• 作者: Pooley, David;Wheeler, J. Craig;Vinkó, Jozsef;Dwarkadas, Vikram V.;Szalai, Tamas;Silverman, Jeffrey M.;Griesel, Madelaine;McCullough, Molly;Marion, G. H.;MacQueen, Phillip
• 通讯作者: MacQueen, Phillip

The Betelgeuse Project. III. Merger Characteristics

参宿四计划。

• DOI: 10.3847/1538-4357/abc3c9
• 发表时间: 2020
• 期刊: The Astrophysical Journal
• 作者: Sullivan, J. M.;Nance, S.;Wheeler, J. Craig
• 通讯作者: Wheeler, J. Craig

The Early Light Curve of the Type Ia Supernova 2021hpr in NGC 3147: Progenitor Constraints with the Companion Interaction Model

• DOI: 10.3847/1538-4357/acc10c
• 发表时间: 2023-03
• 期刊: The Astrophysical Journal
• 作者: G. Lim;M. Im;G. S. Paek;Sung-Chul Yoon;Changsu Choi;Sophia Kim;J. Wheeler;B. Thomas;J. Vinkó;Dohyeong Kim;Jinguk Seo;W. Kang;Taewoo Kim;H. Sung;Yonggi Kim;J.-N. Yoon;Hae-Yeon Kim;Jeong-Gyu Kim;Hana Bae;S. Ehgamberdiev;O. Burhonov;D. Mirzaqulov

High Angular Resolution ALMA Images of Dust and Molecules in the SN 1987A Ejecta

• DOI: 10.3847/1538-4357/ab4b46
• 发表时间: 2019-10
• 期刊: The Astrophysical Journal
• 作者: P. Cigan;M. Matsuura;H. Gomez;R. Indebetouw;F. Abellán;M. Gabler;A. Richards;D. Alp;T. Davis;H. Janka;J. Spyromilio;M. Barlow;D. Burrows;E. Dwek;C. Fransson;B. Gaensler;J. Larsson;P. Bouchet;P. Lundqvist;J. Marcaide;C. Ng;Sangwook Park;P. Roche;J. V. van Loon;J. Wheeler;G. Zanardo

Polarimetry of hydrogen-poor superluminous supernovae

贫氢超发光超新星的偏振测量

• DOI: 10.1051/0004-6361/202345945
• 发表时间: 2023
• 期刊: Astronomy & Astrophysics
• 影响因子: 6.5
• 作者: Pursiainen, M.;Leloudas, G.;Cikota, A.;Bulla, M.;Inserra, C.;Patat, F.;Wheeler, J. C.;Aamer, A.;Gal-Yam, A.;Maund, J.
• 通讯作者: Maund, J.