Stellar response after stripping as a model for common-envelope outcomes
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Stellar response after stripping as a model for common-envelope outcomes. / Vigna-Gomez, Alejandro; Wassink, Michelle; Klencki, Jakub; Istrate, Alina; Nelemans, Gijs; Mandel, Ilya.
I: Monthly Notices of the Royal Astronomical Society, Bind 511, Nr. 2, 11.02.2022, s. 2326-2338.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Stellar response after stripping as a model for common-envelope outcomes
AU - Vigna-Gomez, Alejandro
AU - Wassink, Michelle
AU - Klencki, Jakub
AU - Istrate, Alina
AU - Nelemans, Gijs
AU - Mandel, Ilya
PY - 2022/2/11
Y1 - 2022/2/11
N2 - Binary neutron stars have been observed as millisecond pulsars, gravitational-wave sources, and as the progenitors of short gamma-ray bursts and kilonovae. Massive stellar binaries that evolve into merging double neutron stars are believed to experience a common-envelope episode. During this episode, the envelope of a giant star engulfs the whole binary. The energy transferred from the orbit to the envelope by drag forces or from other energy sources can eject the envelope from the binary system, leading to a stripped short-period binary. In this paper, we use one-dimensional single stellar evolution to explore the final stages of the common-envelope phase in progenitors of neutron star binaries. We consider an instantaneously stripped donor star as a proxy for the common-envelope phase and study the star's subsequent radial evolution. We determine a range of stripping boundaries that allow the star to avoid significant rapid re-expansion and that thus represent plausible boundaries for the termination of the common-envelope episode. We find that these boundaries lie above the maximum compression point, a commonly used location of the core/envelope boundary. We conclude that stars may retain fractions of a solar mass of hydrogen-rich material even after the common-envelope episode. If we consider orbital energy as the only energy source available, all of our models would overfill their Roche lobe after ejecting the envelope, whose binding energy includes gravitational, thermal, radiation, and recombination energy terms.
AB - Binary neutron stars have been observed as millisecond pulsars, gravitational-wave sources, and as the progenitors of short gamma-ray bursts and kilonovae. Massive stellar binaries that evolve into merging double neutron stars are believed to experience a common-envelope episode. During this episode, the envelope of a giant star engulfs the whole binary. The energy transferred from the orbit to the envelope by drag forces or from other energy sources can eject the envelope from the binary system, leading to a stripped short-period binary. In this paper, we use one-dimensional single stellar evolution to explore the final stages of the common-envelope phase in progenitors of neutron star binaries. We consider an instantaneously stripped donor star as a proxy for the common-envelope phase and study the star's subsequent radial evolution. We determine a range of stripping boundaries that allow the star to avoid significant rapid re-expansion and that thus represent plausible boundaries for the termination of the common-envelope episode. We find that these boundaries lie above the maximum compression point, a commonly used location of the core/envelope boundary. We conclude that stars may retain fractions of a solar mass of hydrogen-rich material even after the common-envelope episode. If we consider orbital energy as the only energy source available, all of our models would overfill their Roche lobe after ejecting the envelope, whose binding energy includes gravitational, thermal, radiation, and recombination energy terms.
KW - stars: binaries (including multiple): close
KW - stars: binaries: general
KW - stars: massive
KW - stars: neutron
KW - BINDING-ENERGY PARAMETER
KW - BLACK-HOLE
KW - NEUTRON-STAR
KW - CONVECTIVE BOUNDARIES
KW - BINARY
KW - EVOLUTION
KW - MODULES
KW - SYSTEM
KW - PROGENITORS
KW - DISCOVERY
U2 - 10.1093/mnras/stac237
DO - 10.1093/mnras/stac237
M3 - Journal article
VL - 511
SP - 2326
EP - 2338
JO - Royal Astronomical Society. Monthly Notices
JF - Royal Astronomical Society. Monthly Notices
SN - 0035-8711
IS - 2
ER -
ID: 303686152