Mass Transfer in a Short Wetted-Wall Column. 2. Binary Systems

AbstractWe present preliminary work on the formation scenario of blue straggler stars by mass transfer in binary systems. More precisely, using Smoothed Particle Hydrodynamics (SPH), we want to model only the outer parts of the stars in order to get a much greater spatial resolution of the mass transfer flow itself. The inner boundary conditions are achieved using the so-called ghost particles and by replacing the inner mass by a central point mass. Stability of this central point mass is crucial, and it is shown that we get reasonable results. These simulations should give us indications on which layers of the donor star are actually transferred to the other star as well as how mass is transferred and how it settles on the accretor. This work is aimed at getting distinct observational signatures which would help identifying the dominant formation mechanism of blue straggler stars.

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Constraining Progenitors of Observed Low-mass X-ray Binaries Using Convection and Rotation-Boosted Magnetic Braking

The Astrophysical Journal ◽

10.3847/1538-4357/ac236c ◽

2021 ◽

Vol 922 (2) ◽

pp. 174

Author(s):

Kenny X. Van ◽

Natalia Ivanova

Keyword(s):

Mass Transfer ◽

Binary Systems ◽

Formation Rate ◽

Mass Transfer Rate ◽

Population Synthesis ◽

X Ray ◽

Synthesis Technique ◽

Low Mass ◽

Magnetic Braking ◽

X Ray Binaries

Abstract We present a new method for constraining the mass transfer evolution of low-mass X-ray binaries (LMXBs)—a reverse population synthesis technique. This is done using the detailed 1D stellar evolution code MESA (Modules for Experiments in Stellar Astrophysics) to evolve a high-resolution grid of binary systems spanning a comprehensive range of initial donor masses and orbital periods. We use the recently developed convection and rotation-boosted (CARB) magnetic braking scheme. The CARB magnetic braking scheme is the only magnetic braking prescription capable of reproducing an entire sample of well-studied persistent LMXBs—those with mass ratios, periods, and mass transfer rates that have been observationally determined. Using the reverse population synthesis technique, where we follow any simulated system that successfully reproduces an observed LMXB backward, we have constrained possible progenitors for each observed well-studied persistent LMXB. We also determined that the minimum number of LMXB formations in the Milky Way is 1500 per Gyr if we exclude Cyg X-2. For Cyg X-2, the most likely formation rate is 9000 LMXB Gyr−1. The technique we describe can be applied to any observed LMXB with well-constrained mass ratio, period, and mass transfer rate. With the upcoming GAIA DR3 containing information on binary systems, this technique can be applied to the data release to search for progenitors of observed persistent LMXBs.

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Mass Transfer and Accretion Disc Flow in Close Binary Systems

10.1007/978-94-010-1217-1_3 ◽

1977 ◽

pp. 35-40

Author(s):

D. N. C. Lin ◽

J. E. Pringle

Keyword(s):

Mass Transfer ◽

Binary Systems ◽

Accretion Disc ◽

Close Binary ◽

Close Binary Systems

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The Formation of Compact Objects in Binary Systems

Symposium - International Astronomical Union ◽

10.1017/s0074180900073848 ◽

1981 ◽

Vol 93 ◽

pp. 155-175 ◽

Cited By ~ 1

Author(s):

E.P.J. van den Heuvel

Keyword(s):

Mass Transfer ◽

Binary Systems ◽

Compact Star ◽

Compact Objects ◽

Binary Interaction ◽

X Ray ◽

Tidal Forces ◽

Short Period ◽

Wide Range ◽

X Ray Binaries

The various ways in which compact objects (neutron stars and black holes) can be formed in interacting binary systems are qualitatively outlined on the basis of the three major modes of binary interaction identified by Webbink (1980). Massive interacting binary systems (M1 ≳ 10–12 M⊙) are, after the first phase of mass transfer expected to leave as remnants:(i) compact stars in massive binary systems (mass ≳ 10 M⊙) with a wide range of orbital periods, as remnants of quasi-conservative mass transfer; these systems later evolve into massive X-ray binaries.(ii) short-period compact star binaries (P ~ 1–2 days) in which the companion may be more massive or less massive than the compact object; these systems have high runaway velocities (≳ 100 km/sec) and start out with highly eccentric orbits, which are rapidly circularized by tidal forces; they may later evolve into low-mass X-ray binaries;(iii) single runaway compact objects with space velocities of ~ 102 to 4.102 km/sec; these are expected to be the most numerous compact remnants.Compact star binaries may also form from Cataclysmic binaries or wide binaries in which an O-Ne-Mg white dwarf is driven over the Chandrasekhar limit by accretion.

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IUE Observations of the Two Peculiar Binary Systems Beta Lyrae and Upsilon Sagittarii

Symposium - International Astronomical Union ◽

10.1017/s0074180900065001 ◽

1980 ◽

Vol 88 ◽

pp. 271-286 ◽

Cited By ~ 2

Author(s):

Margherita Hack ◽

Umberto Flora ◽

Paolo Santin

Keyword(s):

Mass Transfer ◽

Mass Loss ◽

Radial Velocity ◽

Effective Temperature ◽

Binary Systems ◽

Close Binaries ◽

Infrared Excess ◽

Show Evidence ◽

The Common ◽

Ultraviolet Observations

The common peculiarities of these two systems are: a) the companion is a massive object (probably m2≥10) whose spectrum is not observable; b) both systems show evidence, though in different degrees, of mass-transfer and mass-loss; c) both present, in different degrees, hydrogen deficiency; d) ultraviolet observations have shown, in both cases, the presence of lines of highly ionized elements like N V, C IV, Si IV, probably formed in an extended envelope because they do not show orbital radial velocity shifts, and cannot be explained by the effective temperature of the star whose spectrum we observe. The latter property seems to be common to several close binaries, as shown by the ultraviolet observations with IUE by Plavec and Koch (1979); e) both systems present infrared excess, suggesting the presence of an extended envelope (Gehrz et al. 1974; Lee and Nariai, 1967; Humphreys and Ney, 1974; Treffers et al. 1976).

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Forced-Convection Mass Transfer From Wetted Grooves

Journal of Basic Engineering ◽

10.1115/1.3425532 ◽

1972 ◽

Vol 94 (4) ◽

pp. 715-719

Author(s):

R. G. Bressler

Keyword(s):

Mass Transfer ◽

Forced Convection ◽

Test Facility ◽

Reynolds Analogy ◽

Flow Rates ◽

Capillary Action ◽

Air Stream ◽

Partial Pressures ◽

Evaporative Heat Transfer ◽

Wetted Wall Column

A wetted-wall column was used to measure liquid flow rates in capillary grooves on vertical surfaces. The test facility contained interchangeable grooved surfaces (2-in. OD) which contacted a liquid reservoir in such a way that the test surfaces were partially wetted by capillary action. The wetted portion was exposed to a forced-convection air stream, so that surface evaporation took place because of the different partial pressures of the vapor at the liquid-vapor interface and at the center of the air stream. All data were obtained in steady-state and nearly isothermal conditions. Experimental results with carbon tetrachloride on brass surfaces were in agreement with approximate predictions, which were computed for evaporative heat transfer and then related to mass transfer by using Reynolds analogy for pipe flow.

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