Fate of the Remnant in Tidal Stripping Event: Repeating and Nonrepeating
Tidal disruption events (TDE) occur when a star ventures too close to a massive black hole. In a partial TDE (pTDE), the star only grazes the tidal radius, causing the outer envelope of the star to be stripped away while the stellar core survives. Previous research has shown that a star, once tidall...
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2024-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ad8b24 |
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| author | Jin-Hong Chen Lixin Dai Shang-Fei Liu Jian-Wen Ou |
| author_facet | Jin-Hong Chen Lixin Dai Shang-Fei Liu Jian-Wen Ou |
| author_sort | Jin-Hong Chen |
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| description | Tidal disruption events (TDE) occur when a star ventures too close to a massive black hole. In a partial TDE (pTDE), the star only grazes the tidal radius, causing the outer envelope of the star to be stripped away while the stellar core survives. Previous research has shown that a star, once tidally stripped in a parabolic orbit, can acquire enough orbital energy for its remnant to become a high-velocity star potentially capable of escaping the galaxy. Conversely, some studies have reported that the remnant may lose orbital energy and undergo re-disruption, leading to a recurring pTDE. This study aims to uncover the physical mechanisms and determine the conditions that lead to these divergent outcomes. We find that the orbital energy change only depends on the impact factor and the stellar structure, and barely depends on the mass of the black hole or the exact mass or orbital eccentricity of the star. For a γ = 5/3 (or γ = 4/3) polytropic star, after a pTDE its remnant gains orbital energy when the impact factor β ≳ 0.62 (or ≳1.1) or loses energy and vice versa. Additionally, we verify an analytical equation for orbital energy change that is applicable across various systems. Through hydrodynamic simulations, we also explore the structure of the stellar remnant post-tidal stripping. Our findings provide critical insights for interpreting observed pTDEs and advancing knowledge on the orbital evolution and event rate of these events. |
| format | Article |
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| institution | Kabale University |
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| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-b59427a5eccb4b0fa018e7b2ecc9e4972024-12-04T12:16:18ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-0197718010.3847/1538-4357/ad8b24Fate of the Remnant in Tidal Stripping Event: Repeating and NonrepeatingJin-Hong Chen0https://orcid.org/0000-0002-3525-791XLixin Dai1https://orcid.org/0000-0002-9589-5235Shang-Fei Liu2https://orcid.org/0000-0002-9442-137XJian-Wen Ou3https://orcid.org/0000-0002-6176-7745Department of Physics, University of Hong Kong , Pokfulam Road, Hong Kong, People’s Republic of China ; chenjh2@hku.hk, lixindai@hku.hkDepartment of Physics, University of Hong Kong , Pokfulam Road, Hong Kong, People’s Republic of China ; chenjh2@hku.hk, lixindai@hku.hkSchool of Physics and Astronomy, Sun Yat-sen University , Zhuhai 519082, People's Republic of China; CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area, Sun Yat-sen University , Zhuhai 519082, People's Republic of ChinaSchool of Intelligent Engineering, Shaoguan University , Shaoguan 512005, People's Republic of ChinaTidal disruption events (TDE) occur when a star ventures too close to a massive black hole. In a partial TDE (pTDE), the star only grazes the tidal radius, causing the outer envelope of the star to be stripped away while the stellar core survives. Previous research has shown that a star, once tidally stripped in a parabolic orbit, can acquire enough orbital energy for its remnant to become a high-velocity star potentially capable of escaping the galaxy. Conversely, some studies have reported that the remnant may lose orbital energy and undergo re-disruption, leading to a recurring pTDE. This study aims to uncover the physical mechanisms and determine the conditions that lead to these divergent outcomes. We find that the orbital energy change only depends on the impact factor and the stellar structure, and barely depends on the mass of the black hole or the exact mass or orbital eccentricity of the star. For a γ = 5/3 (or γ = 4/3) polytropic star, after a pTDE its remnant gains orbital energy when the impact factor β ≳ 0.62 (or ≳1.1) or loses energy and vice versa. Additionally, we verify an analytical equation for orbital energy change that is applicable across various systems. Through hydrodynamic simulations, we also explore the structure of the stellar remnant post-tidal stripping. Our findings provide critical insights for interpreting observed pTDEs and advancing knowledge on the orbital evolution and event rate of these events.https://doi.org/10.3847/1538-4357/ad8b24Hydrodynamical simulationsTidal disruptionIntermediate-mass black holesRoche lobe overflowBlack hole physicsGalaxies |
| spellingShingle | Jin-Hong Chen Lixin Dai Shang-Fei Liu Jian-Wen Ou Fate of the Remnant in Tidal Stripping Event: Repeating and Nonrepeating The Astrophysical Journal Hydrodynamical simulations Tidal disruption Intermediate-mass black holes Roche lobe overflow Black hole physics Galaxies |
| title | Fate of the Remnant in Tidal Stripping Event: Repeating and Nonrepeating |
| title_full | Fate of the Remnant in Tidal Stripping Event: Repeating and Nonrepeating |
| title_fullStr | Fate of the Remnant in Tidal Stripping Event: Repeating and Nonrepeating |
| title_full_unstemmed | Fate of the Remnant in Tidal Stripping Event: Repeating and Nonrepeating |
| title_short | Fate of the Remnant in Tidal Stripping Event: Repeating and Nonrepeating |
| title_sort | fate of the remnant in tidal stripping event repeating and nonrepeating |
| topic | Hydrodynamical simulations Tidal disruption Intermediate-mass black holes Roche lobe overflow Black hole physics Galaxies |
| url | https://doi.org/10.3847/1538-4357/ad8b24 |
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