On rapid binary mass transfer - I. Physical model
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On rapid binary mass transfer - I. Physical model. / Lu, Wenbin; Fuller, Jim; Quataert, Eliot; Bonnerot, Clement.
In: Monthly Notices of the Royal Astronomical Society, Vol. 519, No. 1, 16.12.2022, p. 1409-1424.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - On rapid binary mass transfer - I. Physical model
AU - Lu, Wenbin
AU - Fuller, Jim
AU - Quataert, Eliot
AU - Bonnerot, Clement
PY - 2022/12/16
Y1 - 2022/12/16
N2 - In some semidetached binary systems, the donor star may transfer mass to the companion at a very high rate. We propose that, at sufficiently high mass-transfer rates such that the accretion disc around the companion becomes geometrically thick (or advection-dominated) near the disc outer radius, a large fraction of the transferred mass may be lost through the outer Lagrangian (L2) point, as a result of the excessive energy generated by viscous heating that cannot be efficiently radiated away. A physical model is constructed where the L2 mass-loss fraction is given by the requirement that the remaining material in the disc has Bernoulli number equal to the L2 potential energy. Our model predicts significant L2 mass-loss at mass transfer rates exceeding a few 10(-4) M-circle dot yr(-1). An equatorial circumbinary outflow (CBO) is formed in these systems. Implications for the orbital evolution and the observational appearance of the system are discussed. In particular, (1) rapid angular momentum loss from the system tends to shrink the orbit, and hence may increase the formation rate of mergers and gravitational-wave sources; and (2) photons from the hot disc wind are reprocessed by the CBO into longer wavelength emission in the infrared bands, consistent with Spitzer observations of some ultra-luminous X-ray sources.
AB - In some semidetached binary systems, the donor star may transfer mass to the companion at a very high rate. We propose that, at sufficiently high mass-transfer rates such that the accretion disc around the companion becomes geometrically thick (or advection-dominated) near the disc outer radius, a large fraction of the transferred mass may be lost through the outer Lagrangian (L2) point, as a result of the excessive energy generated by viscous heating that cannot be efficiently radiated away. A physical model is constructed where the L2 mass-loss fraction is given by the requirement that the remaining material in the disc has Bernoulli number equal to the L2 potential energy. Our model predicts significant L2 mass-loss at mass transfer rates exceeding a few 10(-4) M-circle dot yr(-1). An equatorial circumbinary outflow (CBO) is formed in these systems. Implications for the orbital evolution and the observational appearance of the system are discussed. In particular, (1) rapid angular momentum loss from the system tends to shrink the orbit, and hence may increase the formation rate of mergers and gravitational-wave sources; and (2) photons from the hot disc wind are reprocessed by the CBO into longer wavelength emission in the infrared bands, consistent with Spitzer observations of some ultra-luminous X-ray sources.
KW - binaries: general
KW - gravitational waves
KW - stars: mass-loss
KW - ADVECTION-DOMINATED ACCRETION
KW - X-RAY SOURCE
KW - COMMON-ENVELOPE EVOLUTION
KW - BLACK-HOLE
KW - PRESUPERNOVA EVOLUTION
KW - NUMERICAL-SIMULATION
KW - WHITE-DWARF
KW - XMM-NEWTON
KW - FLOWS
KW - STARS
U2 - 10.1093/mnras/stac3621
DO - 10.1093/mnras/stac3621
M3 - Journal article
VL - 519
SP - 1409
EP - 1424
JO - Royal Astronomical Society. Monthly Notices
JF - Royal Astronomical Society. Monthly Notices
SN - 0035-8711
IS - 1
ER -
ID: 338784930