MAGICS II. Seed black holes stripped of their surrounding stars do not sink
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| Autores principales: | , , , , , , , , , |
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| Formato: | Preprint |
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2024
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| _version_ | 1866929525387952128 |
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| author | Zhou, Yihao Mukherjee, Diptajyoti Chen, Nianyi Di Matteo, Tiziana Johansson, Peter H. Rantala, Antti Partmann, Christian Carlo, Ugo NiccolDi Bird, Simeon Ni, Yueying |
| author_facet | Zhou, Yihao Mukherjee, Diptajyoti Chen, Nianyi Di Matteo, Tiziana Johansson, Peter H. Rantala, Antti Partmann, Christian Carlo, Ugo NiccolDi Bird, Simeon Ni, Yueying |
| contents | MBH seed mergers are expected to be among the loudest sources of gravitational waves detected by the Laser Interferometer Space Antenna (LISA), providing a unique window into the birth and early growth of SMBH. We present the MAGICS-II simulation suite, consisting of 6 galaxy mergers that result in MBH seeds mergers identified in the cosmological simulation ASTRID. With the enhanced resolution (mass resolution: 500 $\mathrm{M}_{\odot}$; softening length: $5$ pc), improved subgrid models for the MBH dynamics and accretion, and the accurate regularized gravity integrator included in KETJU, we trace MBH seeds dynamics down to 0.1 pc. After evolving all the systems for $\approx$ 1.2 Gyr in three stages (MAGICS-2000, MAGICS-500, and MAGICS-K), we find in 4 of the 6 systems the MBHs stall at separations $ Δr \gtrsim 200$ pc. Only in 2 systems, the MBHs manage to sink further, and only in one of them a bound binary forms. In the sinking systems, the MBH retains a population of bound stars. The final separation between the MBH is related to the surrounding unstripped stellar (and/or dark matter) mass: if more than 90\% of the surrounding stellar system is stripped away, the MBHs stall. Besides the unstripped stars from the original host galaxy, we find that newly formed stars bound to the MBH significantly contribute to its sinking. Resolving the stellar system around MBH seeds, and its induced tidal interactions and dynamical friction is key for accurately capturing MBH dynamics. For this, high resolution simulations are required. In a companion paper (MAGICS-III), we resimulate the central regions of these systems with increased resolution to model directly the effects of actual star clusters around MBHs. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2409_19914 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | MAGICS II. Seed black holes stripped of their surrounding stars do not sink Zhou, Yihao Mukherjee, Diptajyoti Chen, Nianyi Di Matteo, Tiziana Johansson, Peter H. Rantala, Antti Partmann, Christian Carlo, Ugo NiccolDi Bird, Simeon Ni, Yueying Astrophysics of Galaxies MBH seed mergers are expected to be among the loudest sources of gravitational waves detected by the Laser Interferometer Space Antenna (LISA), providing a unique window into the birth and early growth of SMBH. We present the MAGICS-II simulation suite, consisting of 6 galaxy mergers that result in MBH seeds mergers identified in the cosmological simulation ASTRID. With the enhanced resolution (mass resolution: 500 $\mathrm{M}_{\odot}$; softening length: $5$ pc), improved subgrid models for the MBH dynamics and accretion, and the accurate regularized gravity integrator included in KETJU, we trace MBH seeds dynamics down to 0.1 pc. After evolving all the systems for $\approx$ 1.2 Gyr in three stages (MAGICS-2000, MAGICS-500, and MAGICS-K), we find in 4 of the 6 systems the MBHs stall at separations $ Δr \gtrsim 200$ pc. Only in 2 systems, the MBHs manage to sink further, and only in one of them a bound binary forms. In the sinking systems, the MBH retains a population of bound stars. The final separation between the MBH is related to the surrounding unstripped stellar (and/or dark matter) mass: if more than 90\% of the surrounding stellar system is stripped away, the MBHs stall. Besides the unstripped stars from the original host galaxy, we find that newly formed stars bound to the MBH significantly contribute to its sinking. Resolving the stellar system around MBH seeds, and its induced tidal interactions and dynamical friction is key for accurately capturing MBH dynamics. For this, high resolution simulations are required. In a companion paper (MAGICS-III), we resimulate the central regions of these systems with increased resolution to model directly the effects of actual star clusters around MBHs. |
| title | MAGICS II. Seed black holes stripped of their surrounding stars do not sink |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2409.19914 |