Forming a clumpy circumstellar material in energetic pre-supernova activity
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| Format: | Preprint |
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2025
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| _version_ | 1866908328030896128 |
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| author | Hillel, Shlomi Schreier, Ron Soker, Noam |
| author_facet | Hillel, Shlomi Schreier, Ron Soker, Noam |
| contents | We demonstrate by three-dimensional hydrodynamical simulations of energy deposition into the envelope of a red supergiant (RSG) model the inflation of a Rayleigh-Taylor unstable envelope that forms a compact clumpy circumstellar material (CSM). Our simulations mimic vigorous core activity years to months before a core-collapse supernova (CCSN) explosion that deposits energy to the outer envelope. The fierce core nuclear activity in the pre-CCSN explosion phase might excite waves that propagate to the envelope. The wave energy is dissipated where envelope convection cannot carry the energy. We deposit this energy into a shell in the outer envelope with a power of L(wave)=2.6e6Lo or L(wave)=5.2e5Lo for 0.32 year. The energy-deposition shell expands while its pressure is higher than its surroundings, but its density is lower. Therefore, this expansion is Rayleigh-Taylor unstable and develops instability fingers. Most of the inflated envelope does not reach the escape velocity in the year of simulation but forms a compact and clumpy CSM. The high density of the inflated envelope implies that if a companion is present in that zone, it will accrete mass at a very high rate and power a pre-explosion outburst. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2503_14438 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Forming a clumpy circumstellar material in energetic pre-supernova activity Hillel, Shlomi Schreier, Ron Soker, Noam High Energy Astrophysical Phenomena We demonstrate by three-dimensional hydrodynamical simulations of energy deposition into the envelope of a red supergiant (RSG) model the inflation of a Rayleigh-Taylor unstable envelope that forms a compact clumpy circumstellar material (CSM). Our simulations mimic vigorous core activity years to months before a core-collapse supernova (CCSN) explosion that deposits energy to the outer envelope. The fierce core nuclear activity in the pre-CCSN explosion phase might excite waves that propagate to the envelope. The wave energy is dissipated where envelope convection cannot carry the energy. We deposit this energy into a shell in the outer envelope with a power of L(wave)=2.6e6Lo or L(wave)=5.2e5Lo for 0.32 year. The energy-deposition shell expands while its pressure is higher than its surroundings, but its density is lower. Therefore, this expansion is Rayleigh-Taylor unstable and develops instability fingers. Most of the inflated envelope does not reach the escape velocity in the year of simulation but forms a compact and clumpy CSM. The high density of the inflated envelope implies that if a companion is present in that zone, it will accrete mass at a very high rate and power a pre-explosion outburst. |
| title | Forming a clumpy circumstellar material in energetic pre-supernova activity |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2503.14438 |