Hydrodynamics of Relativistic Superheated Bubbles
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arXiv
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| Main Authors: | , , , |
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| Format: | Preprint |
| Published: |
2024
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| _version_ | 1866917275983937536 |
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| author | Bea, Yago Casalderrey-Solana, Jorge Mateos, David Sanchez-Garitaonandia, Mikel |
| author_facet | Bea, Yago Casalderrey-Solana, Jorge Mateos, David Sanchez-Garitaonandia, Mikel |
| contents | Relativistic, charged, superheated bubbles may play an important role in neutron star mergers if first-order phase transitions are present in the phase diagram of Quantum Chromodynamics. We describe the properties of these bubbles in the hydrodynamic regime. We find two qualitative differences with supercooled bubbles. First, the pressure at the center of an expanding superheated bubble can be higher or lower than the pressure in the asymptotic, metastable phase. Second, some fluid flows develop metastable regions behind the bubble wall for any choice of the equation of state. We consider the possible role of a conserved charge akin to baryon number. The fluid flow profiles are unaffected by this charge if the speed of sound is constant in each phase, but they are modified for more general equations of state. We compute the efficiency factor relevant for gravitational wave production. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2406_14450 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Hydrodynamics of Relativistic Superheated Bubbles Bea, Yago Casalderrey-Solana, Jorge Mateos, David Sanchez-Garitaonandia, Mikel High Energy Physics - Theory High Energy Astrophysical Phenomena General Relativity and Quantum Cosmology Relativistic, charged, superheated bubbles may play an important role in neutron star mergers if first-order phase transitions are present in the phase diagram of Quantum Chromodynamics. We describe the properties of these bubbles in the hydrodynamic regime. We find two qualitative differences with supercooled bubbles. First, the pressure at the center of an expanding superheated bubble can be higher or lower than the pressure in the asymptotic, metastable phase. Second, some fluid flows develop metastable regions behind the bubble wall for any choice of the equation of state. We consider the possible role of a conserved charge akin to baryon number. The fluid flow profiles are unaffected by this charge if the speed of sound is constant in each phase, but they are modified for more general equations of state. We compute the efficiency factor relevant for gravitational wave production. |
| title | Hydrodynamics of Relativistic Superheated Bubbles |
| topic | High Energy Physics - Theory High Energy Astrophysical Phenomena General Relativity and Quantum Cosmology |
| url | https://arxiv.org/abs/2406.14450 |