Inferring a Dense Confined Circumstellar Medium around Supernova Progenitors via Long-term Hydrodynamical Evolution
Circumstellar interaction of supernova (SN) ejecta is an essential process in its evolution, and observations of SNe have found the signature of circumstellar interaction in both the early and late evolutionary phases of SNe. In this Letter, we show that if the SN forward shock plunges into a tenuou...
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2025-01-01
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| author | Tomoki Matsuoka Keiichi Maeda Ke-Jung Chen |
| author_facet | Tomoki Matsuoka Keiichi Maeda Ke-Jung Chen |
| author_sort | Tomoki Matsuoka |
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| description | Circumstellar interaction of supernova (SN) ejecta is an essential process in its evolution, and observations of SNe have found the signature of circumstellar interaction in both the early and late evolutionary phases of SNe. In this Letter, we show that if the SN forward shock plunges into a tenuous stellar wind from a dense circumstellar medium (CSM) in the vicinity of the progenitor (i.e., confined CSM), the subsequent time evolutions of the SN–CSM interaction system deviate from the prediction of a self-similar solution. In this case, after all of the confined CSM is swept up by the SN forward shock (roughly 10 days after the explosion), the propagation of the shocked shell will be driven by the freely expanding ram pressure of the confined CSM component, instead of the SN ejecta. Meanwhile, the forward shock decelerates faster than the prediction of thin-shell approximation once the confined CSM component reaches homologous expansion. This lasts until the reverse shock in the confined CSM component reaches the head of the SN ejecta, leading to the restoration of the system into the evolutionary model without confined CSM, where the SN ejecta drives the expansion of the system. We also show that this peculiar evolution will be reflected in observational signatures originating from SN–CSM interaction, taking rapid decline and rebrightening of radio emission as examples. Our results shed light on the importance of taking into account the effect of initial SN–CSM interaction even when we focus on observational properties of SNe a few years after the explosion. |
| format | Article |
| id | doaj-art-5542e71ad66b4ad7b8ff17f381a44910 |
| institution | Kabale University |
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| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-5542e71ad66b4ad7b8ff17f381a449102025-08-20T03:56:41ZengIOP PublishingThe Astrophysical Journal Letters2041-82052025-01-019882L5310.3847/2041-8213/adef08Inferring a Dense Confined Circumstellar Medium around Supernova Progenitors via Long-term Hydrodynamical EvolutionTomoki Matsuoka0https://orcid.org/0000-0002-6916-3559Keiichi Maeda1https://orcid.org/0000-0003-2611-7269Ke-Jung Chen2https://orcid.org/0000-0002-4848-5508Institute of Astronomy and Astrophysics , Academia Sinica, No. 1, Sec. 4, Roosevelt Road, Taipei 106216, Taiwan ; tmatsuoka@asiaa.sinica.edu.twDepartment of Astronomy, Kyoto University , Kitashirakawa-oiwakecho, Sakyo-ku, Kyoto 606-8502, JapanInstitute of Astronomy and Astrophysics , Academia Sinica, No. 1, Sec. 4, Roosevelt Road, Taipei 106216, Taiwan ; tmatsuoka@asiaa.sinica.edu.tw; Heidelberg Institute for Theoretical Studies , Schloss-Wolfsbrunnenweg 35, Heidelberg 69118, GermanyCircumstellar interaction of supernova (SN) ejecta is an essential process in its evolution, and observations of SNe have found the signature of circumstellar interaction in both the early and late evolutionary phases of SNe. In this Letter, we show that if the SN forward shock plunges into a tenuous stellar wind from a dense circumstellar medium (CSM) in the vicinity of the progenitor (i.e., confined CSM), the subsequent time evolutions of the SN–CSM interaction system deviate from the prediction of a self-similar solution. In this case, after all of the confined CSM is swept up by the SN forward shock (roughly 10 days after the explosion), the propagation of the shocked shell will be driven by the freely expanding ram pressure of the confined CSM component, instead of the SN ejecta. Meanwhile, the forward shock decelerates faster than the prediction of thin-shell approximation once the confined CSM component reaches homologous expansion. This lasts until the reverse shock in the confined CSM component reaches the head of the SN ejecta, leading to the restoration of the system into the evolutionary model without confined CSM, where the SN ejecta drives the expansion of the system. We also show that this peculiar evolution will be reflected in observational signatures originating from SN–CSM interaction, taking rapid decline and rebrightening of radio emission as examples. Our results shed light on the importance of taking into account the effect of initial SN–CSM interaction even when we focus on observational properties of SNe a few years after the explosion.https://doi.org/10.3847/2041-8213/adef08SupernovaeSupernova dynamicsCircumstellar matterHydrodynamics |
| spellingShingle | Tomoki Matsuoka Keiichi Maeda Ke-Jung Chen Inferring a Dense Confined Circumstellar Medium around Supernova Progenitors via Long-term Hydrodynamical Evolution The Astrophysical Journal Letters Supernovae Supernova dynamics Circumstellar matter Hydrodynamics |
| title | Inferring a Dense Confined Circumstellar Medium around Supernova Progenitors via Long-term Hydrodynamical Evolution |
| title_full | Inferring a Dense Confined Circumstellar Medium around Supernova Progenitors via Long-term Hydrodynamical Evolution |
| title_fullStr | Inferring a Dense Confined Circumstellar Medium around Supernova Progenitors via Long-term Hydrodynamical Evolution |
| title_full_unstemmed | Inferring a Dense Confined Circumstellar Medium around Supernova Progenitors via Long-term Hydrodynamical Evolution |
| title_short | Inferring a Dense Confined Circumstellar Medium around Supernova Progenitors via Long-term Hydrodynamical Evolution |
| title_sort | inferring a dense confined circumstellar medium around supernova progenitors via long term hydrodynamical evolution |
| topic | Supernovae Supernova dynamics Circumstellar matter Hydrodynamics |
| url | https://doi.org/10.3847/2041-8213/adef08 |
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