Thermal Evolution of Neo-neutron Stars. I. Envelopes, Eddington Luminosity Phase, and Implications for GW170817
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Thermal Evolution of Neo-neutron Stars. I. Envelopes, Eddington Luminosity Phase, and Implications for GW170817. / Beznogov, Mikhail V.; Page, Dany; Ramirez-Ruiz, Enrico.
In: Astrophysical Journal, Vol. 888, No. 2, 97, 10.01.2020.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - Thermal Evolution of Neo-neutron Stars. I. Envelopes, Eddington Luminosity Phase, and Implications for GW170817
AU - Beznogov, Mikhail V.
AU - Page, Dany
AU - Ramirez-Ruiz, Enrico
PY - 2020/1/10
Y1 - 2020/1/10
N2 - A neo-neutron star is a hot neutron star that has just become transparent to neutrinos. In a core-collapse supernova or accretion-induced collapse of a white dwarf, the neo-neutron star phase directly follows the proto-neutron star phase, about 30-60 s after the initial collapse. It will also be present in a binary neutron star merger in the case where the "born-again" hot massive compact star does not immediately collapse into a black hole. Eddington or even super-Eddington luminosities are present for some time. A neo-neutron star produced in a core-collapse supernova is not directly observable, but the one produced by a binary merger, likely associated with an off-axis short gamma-ray burst, may be observable for some time as well as when produced in the accretion-induced collapse of a white dwarf. We present a first step in the study of this neo-neutron star phase in a spherically symmetric configuration, thus ignoring fast rotation and also ignoring the effect of strong magnetic fields. We put particular emphasis on determining how long the star can sustain a near-Eddington luminosity and also show the importance of positrons and contraction energy during the neo-neutron star phase. We finally discuss the observational prospects for neutron star mergers triggered by LIGO and for accretion-induced collapse transients.
AB - A neo-neutron star is a hot neutron star that has just become transparent to neutrinos. In a core-collapse supernova or accretion-induced collapse of a white dwarf, the neo-neutron star phase directly follows the proto-neutron star phase, about 30-60 s after the initial collapse. It will also be present in a binary neutron star merger in the case where the "born-again" hot massive compact star does not immediately collapse into a black hole. Eddington or even super-Eddington luminosities are present for some time. A neo-neutron star produced in a core-collapse supernova is not directly observable, but the one produced by a binary merger, likely associated with an off-axis short gamma-ray burst, may be observable for some time as well as when produced in the accretion-induced collapse of a white dwarf. We present a first step in the study of this neo-neutron star phase in a spherically symmetric configuration, thus ignoring fast rotation and also ignoring the effect of strong magnetic fields. We put particular emphasis on determining how long the star can sustain a near-Eddington luminosity and also show the importance of positrons and contraction energy during the neo-neutron star phase. We finally discuss the observational prospects for neutron star mergers triggered by LIGO and for accretion-induced collapse transients.
KW - Neutron stars
KW - Type II supernovae
KW - Gamma-ray bursts
KW - X-ray point sources
KW - ACCRETION-INDUCED COLLAPSE
KW - EQUATION-OF-STATE
KW - HIGH-RESOLUTION CALCULATIONS
KW - COMPACT CENTRAL SOURCES
KW - NICKEL-RICH OUTFLOWS
KW - X-RAY SEARCH
KW - WHITE-DWARFS
KW - TEMPERATURE DISTRIBUTION
KW - SURFACE-TEMPERATURE
KW - SUPERNOVA-REMNANTS
U2 - 10.3847/1538-4357/ab5fd6
DO - 10.3847/1538-4357/ab5fd6
M3 - Journal article
VL - 888
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 97
ER -
ID: 247444492