An Analytic Model for Mass Transfer in Binaries with Arbitrary Eccentricity, with Applications to Triple-star Systems

Hamers, Adrian S.; Dosopoulou, Fani

doi:10.3847/1538-4357/ab001d

Cited by 48 publications

(45 citation statements)

References 79 publications

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“…Hamers & Dosopoulou (2019) noted that evolution towards circularisation from Dosopoulou & Kalogera (2016b) could lead to (non-physical) negative eccentricity solutions. They proposed a revised analytic model for mass transfer in eccentric binaries.…”

Section: Discussionmentioning

confidence: 99%

Common envelope episodes that lead to double neutron star formation

Vigna-Gómez

MacLeod

Neijssel

et al. 2020

Publ. Astron. Soc. Aust.

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Close double neutron stars (DNSs) have been observed as Galactic radio pulsars, while their mergers have been detected as gamma-ray bursts and gravitational wave sources. They are believed to have experienced at least one common envelope episode (CEE) during their evolution prior to DNS formation. In the last decades, there have been numerous efforts to understand the details of the common envelope (CE) phase, but its computational modelling remains challenging. We present and discuss the properties of the donor and the binary at the onset of the Roche lobe overflow (RLOF) leading to these CEEs as predicted by rapid binary population synthesis models. These properties can be used as initial conditions for detailed simulations of the CE phase. There are three distinctive populations, classified by the evolutionary stage of the donor at the moment of the onset of the RLOF: giant donors with fully convective envelopes, cool donors with partially convective envelopes, and hot donors with radiative envelopes. We also estimate that, for standard assumptions, tides would not circularise a large fraction of these systems by the onset of RLOF. This makes the study and understanding of eccentric mass-transferring systems relevant for DNS populations.

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Section: Discussionmentioning

confidence: 99%

Common envelope episodes that lead to double neutron star formation

Vigna-Gómez

MacLeod

Neijssel

et al. 2020

Publ. Astron. Soc. Aust.

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“…We further note that the dynamics of these encounters are the high-mass ratio limit of the more-thoroughly considered scenario of Roche lobe overflow in eccentric stellar binaries (e.g. Matese and Whitmire 1983;Hamers and Dosopoulou 2019).…”

Section: Multiple Encountersmentioning

confidence: 85%

The Process of Stellar Tidal Disruption by Supermassive Black Holes

et al. 2021

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Tidal disruption events (TDEs) are among the brightest transients in the optical, ultraviolet, and X-ray sky. These flares are set into motion when a star is torn apart by the tidal field of a massive black hole, triggering a chain of events which is – so far – incompletely understood. However, the disruption process has been studied extensively for almost half a century, and unlike the later stages of a TDE, our understanding of the disruption itself is reasonably well converged. In this Chapter, we review both analytical and numerical models for stellar tidal disruption. Starting with relatively simple, order-of-magnitude physics, we review models of increasing sophistication, the semi-analytic “affine formalism,” hydrodynamic simulations of the disruption of polytropic stars, and the most recent hydrodynamic results concerning the disruption of realistic stellar models. Our review surveys the immediate aftermath of disruption in both typical and more unusual TDEs, exploring how the fate of the tidal debris changes if one considers non-main sequence stars, deeply penetrating tidal encounters, binary star systems, and sub-parabolic orbits. The stellar tidal disruption process provides the initial conditions needed to model the formation of accretion flows around quiescent massive black holes, and in some cases may also lead to directly observable emission, for example via shock breakout, gravitational waves or runaway nuclear fusion in deeply plunging TDEs.

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“…We note that on an eccentric orbit, _ M=M may vary smoothly along the orbit. For instance, it might be reasonable to assume that _ M has a local maximum and minimum at periapsis and apoapsis, respectively [13]. Detailed modeling of mass transfer in eccentric orbits is the subject of ongoing research that is beyond the scope of this paper.…”

Section: Donor Spin Evolution Due To Mass Transfermentioning

confidence: 99%

“…In turn, modeling the mass transfer rate on eccentric orbits in which the orbital separation oscillates is extremely difficult since mass transfer might occur partially within each orbit at a varying rate and does backreact on the orbital elements, changing the eccentricity and semimajor axis. Recently, several promising attempts have been made to solve these difficulties [13][14][15][16]. Secondly, the rotational angular momentum vectors (spins) of the binary stars are assumed to be aligned with the orbital axis.…”

Section: Introductionmentioning

confidence: 99%

Flipping spins in mass transferring binaries and origin of spin-orbit misalignment in binary black holes

Stegmann

Antonini

2021

Phys. Rev. D

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Close stellar binaries are prone to undergo a phase of stable mass transfer in which a star loses mass to its companion. Assuming that the donor star loses mass along the instantaneous interstellar axis, we derive the orbit-averaged equations of motion describing the evolution of the donor rotational angular momentum vector (spin) that accompanies the transfer of mass. We consider: (i) a model in which the mass transfer rate is constant within each orbit and (ii) a phase-dependent rate in which all mass per orbit is lost at periapsis. In both cases, we find that the ejection of ≳30 percent of the donor's initial mass causes its spin to nearly flip onto the orbital plane of the binary, independently of the initial spin-orbit alignment. Moreover, we show that the spin flip due to mass transfer can easily dominate over tidal synchronization in any giant stars and main-sequence stars with masses ∼1.5 to 5 M ⊙ . Finally, the general equations of motion, including tides, are used to evolve a realistic population of massive binary stars, leading to the formation of binary black holes. Assuming that the stellar core and envelope are fully coupled, the resulting tilt of the first-born black hole reduces its spin projection onto the orbit normal by a factor ∼Oð0.1Þ. This result supports previous studies in favor of an insignificant contribution to the effective spin projection, χ eff , in binary black holes formed from the evolution of field binaries.

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An Analytic Model for Mass Transfer in Binaries with Arbitrary Eccentricity, with Applications to Triple-star Systems

Cited by 48 publications

References 79 publications

Common envelope episodes that lead to double neutron star formation

Common envelope episodes that lead to double neutron star formation

The Process of Stellar Tidal Disruption by Supermassive Black Holes

Flipping spins in mass transferring binaries and origin of spin-orbit misalignment in binary black holes

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