The Effect of Donor Star Rejuvenation on Common Envelope Evolution
In close binary star systems, common envelope evolution (CEE) may occur after a previous phase of mass transfer. Some isolated formation channels for double neutron star binaries suggest that the donor of CEE was the accretor of a previous phase of stable mass transfer. Accretion should substantiall...
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2025-01-01
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| author | C. Landri P. M. Ricker M. Renzo S. Rau A. Vigna-Gómez |
| author_facet | C. Landri P. M. Ricker M. Renzo S. Rau A. Vigna-Gómez |
| author_sort | C. Landri |
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| description | In close binary star systems, common envelope evolution (CEE) may occur after a previous phase of mass transfer. Some isolated formation channels for double neutron star binaries suggest that the donor of CEE was the accretor of a previous phase of stable mass transfer. Accretion should substantially alter the structure of the donor, particularly by steepening the density gradient at the core-envelope interface and rejuvenating the star. We study the CEE of a donor that was the accretor of a previous phase of stable mass transfer and has a rejuvenated structure. We perform 3D hydrodynamics simulations of the CEE of an 18 M _⊙ supergiant with a 1.4 M _⊙ companion using rejuvenated and non-rejuvenated 1D stellar models for the donor. We compare the two simulations to characterize the effect of the rejuvenation on the outcome of the common envelope phase and the shape of the ejecta. We find that accounting for a previous phase of mass transfer reduces the duration of the inspiral phase by a factor of two, likely due to the different structures in the outer layers of the donor. In the rejuvenated case, the simulations show more equatorially concentrated and asymmetric ejecta, though both cases display evidence for the formation of a pressure-supported thick circumbinary disk. During the dynamical inspiral phase, the impact of rejuvenation on the unbinding of the envelope is unclear; we find that rejuvenation decreases the amount of unbound mass by 20%–40% depending on the energy criterion used. |
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| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-9c28a066d3c84c3687c66be1eea8de022025-01-17T15:56:58ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0197915710.3847/1538-4357/ad9d3cThe Effect of Donor Star Rejuvenation on Common Envelope EvolutionC. Landri0https://orcid.org/0000-0001-8078-0905P. M. Ricker1https://orcid.org/0000-0002-5294-0630M. Renzo2https://orcid.org/0000-0002-6718-9472S. Rau3https://orcid.org/0000-0003-4692-5941A. Vigna-Gómez4https://orcid.org/0000-0003-1817-3586Institute of Theoretical Physics, Faculty of Mathematics and Physics, Charles University , V Holešovickách 2, CZ-180 00 Praha 8, Czech Republic ; camille.landri@utf.mff.cuni.czDepartment of Astronomy and Illinois Center for Advanced Studies of the Universe, University of Illinois , 1002 W. Green St., Urbana, IL 61801, USASteward Observatory, University of Arizona , 933 N. Cherry Ave., Tucson, AZ 85721, USADepartment of Astronomy, University of Illinois , 1002 W. Green St., Urbana, IL 61801, USAMax-Planck-Institut für Astrophysik , Karl-Schwarzschild-Str. 1, D-85748 Garching, GermanyIn close binary star systems, common envelope evolution (CEE) may occur after a previous phase of mass transfer. Some isolated formation channels for double neutron star binaries suggest that the donor of CEE was the accretor of a previous phase of stable mass transfer. Accretion should substantially alter the structure of the donor, particularly by steepening the density gradient at the core-envelope interface and rejuvenating the star. We study the CEE of a donor that was the accretor of a previous phase of stable mass transfer and has a rejuvenated structure. We perform 3D hydrodynamics simulations of the CEE of an 18 M _⊙ supergiant with a 1.4 M _⊙ companion using rejuvenated and non-rejuvenated 1D stellar models for the donor. We compare the two simulations to characterize the effect of the rejuvenation on the outcome of the common envelope phase and the shape of the ejecta. We find that accounting for a previous phase of mass transfer reduces the duration of the inspiral phase by a factor of two, likely due to the different structures in the outer layers of the donor. In the rejuvenated case, the simulations show more equatorially concentrated and asymmetric ejecta, though both cases display evidence for the formation of a pressure-supported thick circumbinary disk. During the dynamical inspiral phase, the impact of rejuvenation on the unbinding of the envelope is unclear; we find that rejuvenation decreases the amount of unbound mass by 20%–40% depending on the energy criterion used.https://doi.org/10.3847/1538-4357/ad9d3cCommon envelope binary starsInteracting binary starsCommon envelope evolutionHydrodynamicsHydrodynamical simulations |
| spellingShingle | C. Landri P. M. Ricker M. Renzo S. Rau A. Vigna-Gómez The Effect of Donor Star Rejuvenation on Common Envelope Evolution The Astrophysical Journal Common envelope binary stars Interacting binary stars Common envelope evolution Hydrodynamics Hydrodynamical simulations |
| title | The Effect of Donor Star Rejuvenation on Common Envelope Evolution |
| title_full | The Effect of Donor Star Rejuvenation on Common Envelope Evolution |
| title_fullStr | The Effect of Donor Star Rejuvenation on Common Envelope Evolution |
| title_full_unstemmed | The Effect of Donor Star Rejuvenation on Common Envelope Evolution |
| title_short | The Effect of Donor Star Rejuvenation on Common Envelope Evolution |
| title_sort | effect of donor star rejuvenation on common envelope evolution |
| topic | Common envelope binary stars Interacting binary stars Common envelope evolution Hydrodynamics Hydrodynamical simulations |
| url | https://doi.org/10.3847/1538-4357/ad9d3c |
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