Pre-Main-Sequence Evolution of Close Binaries with Mass Transfer

1981 ◽  
pp. 111-111
Author(s):  
Kwan-Yu Chen
Keyword(s):  
Mass Transfer ◽  
Main Sequence ◽  
Close Binaries ◽  
Sequence Evolution

scholarly journals The Evolution of Pre-Main Sequence Close Binaries

1980 ◽  
Vol 88 ◽  
pp. 149-153 ◽  
Author(s):  
Jon K. West ◽  
Kwan-Yu Chen
Keyword(s):  
Mass Transfer ◽  
Binary System ◽  
Total Mass ◽  
Main Sequence ◽  
Binary Star ◽  
Computer Models ◽  
Close Binary ◽  
Close Binaries ◽  
Close Binary Star ◽  
Conventional Computer

Conventional computer models of close binary star systems usually start with at least one component on the main sequence. Models of premain sequence binaries have been computed to study mass transfer (Yamasaki 1971). However no pre-main sequence computations have been published that follow the evolutionary tracks of a binary system onto the main sequence, even though some observed systems appear to be premain sequence (Field 1969). The main purpose of this investigation is the evaluation of individual close binaries with a pre-main sequence model. The evaluation will be accomplished by comparing the positions of the observed binary on the Hertzsprung-Russell diagram with the evolutionary tracks generated by the pre-main sequence model. If both components appear to have the same age and fall near the tracks of the model, then the system is possibly pre-main sequence. Eleven semidetached binaries were considered, each with a total mass between 2.5 and 6 solar masses and with a period between 0.9 and 3.4 days.

scholarly journals Massive donors in interacting binaries: effect of metallicity

2020 ◽  
Vol 638 ◽  
pp. A55 ◽  
Author(s):  
Jakub Klencki ◽  
Gijs Nelemans ◽  
Alina G. Istrate ◽  
Onno Pols
Keyword(s):  
Mass Transfer ◽  
Parameter Space ◽  
Binary Systems ◽  
Main Sequence ◽  
Massive Stars ◽  
First Episode ◽  
Sequence Evolution ◽  
Radial Expansion ◽  
Solar Metallicity ◽  
Order Of Magnitude

Metallicity is known to significantly affect the radial expansion of a massive star: the lower the metallicity, the more compact the star, especially during its post-main sequence evolution. Our goal is to study this effect in the context of binary evolution. Using the stellar-evolution code MESA, we computed evolutionary tracks of massive stars at six different metallicities between 1.0 Z⊙ and 0.01 Z⊙. We explored variations of factors known to affect the radial expansion of massive stars (e.g., semiconvection, overshooting, or rotation). Using observational constraints, we find support for an evolution in which already at a metallicity Z ≈ 0.2 Z⊙ massive stars remain relatively compact (∼100 R⊙) during the Hertzprung-gap (HG) phase and most of their expansion occurs during core-helium burning (CHeB). Consequently, we show that metallicity has a strong influence on the type of mass transfer evolution in binary systems. At solar metallicity, a case-B mass transfer is initiated shortly after the end of the main sequence, and a giant donor is almost always a rapidly expanding HG star. However, at lower metallicity, the parameter space for mass transfer from a more evolved, slowly expanding CHeB star increases dramatically. This means that envelope stripping and formation of helium stars in low-metallicity environments occurs later in the evolution of the donor, implying a shorter duration of the Wolf-Rayet phase (even by an order of magnitude) and higher final core masses. This metallicity effect is independent of the effect of metallicity-dependent stellar winds. At metallicities Z ≤ 0.04 Z⊙, a significant fraction of massive stars in binaries with periods longer than 100 days engages in the first episode of mass transfer very late into their evolution, when they already have a well-developed CO core. The remaining lifetime (≲104 yr) is unlikely to be long enough to strip the entire H-rich envelope. Cases of unstable mass transfer leading to a merger would produce CO cores that spin fast at the moment of collapse. We find that the parameter space for mass transfer from massive donors (> 40 M⊙) with outer convective envelopes is extremely small or even nonexistent. We briefly discuss this finding in the context of the formation of binary black hole mergers.

scholarly journals Evolution of Intermediate Mass Close Binaries

1980 ◽  
Vol 88 ◽  
pp. 109-114
Author(s):  
Th.J. Van Der Linden
Keyword(s):  
Mass Transfer ◽  
Binary Systems ◽  
Main Sequence ◽  
Mass Transfer Rate ◽  
Primary Component ◽  
Close Binary ◽  
Close Binaries ◽  
Transfer Phase ◽  
Helium Burning ◽  
Helium Star

Numerical simulations of close binary evolution were performed for five binary systems, using a newly developed evolutionary program. The systems have masses 3+2, 4+3.2, 6+4, 9+6, 12+8 M⊙ and periods 2d, 1d78, 3d, 4d, 5d respectively. The primary component was followed from the zero-age main sequence through the mass transfer phase to core-helium burning. Special care was given to the self-consistent determination of the mass transfer rate and the detailed treatment of composition changes. After the mass transfer phase the resulting systems consist of a main sequence star with a helium star companion of mass 0.36, 0.46, 0.82, 1.48, 2.30 M⊙ for the five systems respectively. Interesting “thermal pulses” were found in the 3+2 M⊙ system at the onset of helium burning.

scholarly journals Pre-Main-Sequence Evolution of Close Binaries with Mass Transfer

1981 ◽  
Vol 93 ◽  
pp. 111-111 ◽  
Author(s):  
Kwan-Yu Chen
Keyword(s):  
Mass Transfer ◽  
Angular Momentum ◽  
Virial Theorem ◽  
Angular Speed ◽  
Close Binaries ◽  
Time Interval ◽  
Sequence Evolution ◽  
Time Step ◽  
Orbital Revolution ◽  
Approximate Expressions

The scenario begins with two spherical masses of Roche radii, as given by Paczynski (1971), at a separation of centers, A. The mass flows from the initially more massive star a in rapid rotation to its companion b. The separation changes in accordance with the conservation of orbital angular momentum. The corresponding Roche radius of b is considered to be its radius. The luminosities of the stars are given in the approximate expressions following Schatzman (1963) for convective or radiative equilibrium. The luminosity of b determines the time for a given mass transfer with the use of the virial theorem. This time step and the virial theorem, then, determine the change of the radius of a. The angular speed of a is maintained such that the centrifugal and gravitational accelerations are equal at the equator. If the total angular momentum of the system is conserved, the angular momentum of b can be computed. Initially, b is considered to rotate in synchronism with the orbital revolution. The mass transfer stops when the centrifugal and gravitational accelerations become equal at the equator of b, or when the change in potential energy becomes zero. In the table, Sf is the ratio of final rotational and orbital angular speeds; t is the time interval in 103y; initial Ma is 3 solar masses; Mbi = 0.7 for part 1, and Ai = 32.2 solar radii for part 2.

ON THE THEORY OF GAMMA RAY BURSTS AND HYPERNOVAE: THE BLACK HOLE SOFT X-RAY TRANSIENT SOURCES

2003 ◽  
Vol 18 (04) ◽  
pp. 527-576 ◽  
Author(s):  
CHANG-HWAN LEE ◽  
GERALD E. BROWN
Keyword(s):  
Mass Transfer ◽  
Black Hole ◽  
Mass Loss ◽  
Evolutionary History ◽  
Main Sequence ◽  
Gamma Ray ◽  
Supernova Explosion ◽  
Sequence Evolution ◽  
X Ray ◽  
Black Hole Binaries

We show that a common evolutionary history can produce the black hole binaries in the Galaxy in which the black holes have masses of ~ 5 - 10M⊙. In the black hole binaries with low-mass, ≲ 2.5M⊙ ZAMS (zero age main sequence) companions, the latter remain in main sequence during the active stage of soft X-ray transients (SXT's), most of them being of K or M classification. In two intermediate cases, IL Lupi and Nova Scorpii with ZAMS ~ 2.5M⊙ companions the orbits are greatly widened because of large mass loss in the explosion forming the black hole, and whereas these companions are in late main sequence evolution, they are close to evolving. Binaries with companion ZAMS masses ≳ 3M⊙ are initially "silent" until the companion begins evolving across the Herzsprung gap. We provide evidence that the narrower, shorter period binaries, with companions now in main sequence, are fossil remnants of gamma ray bursters (GRB's). We also show that the GRB is generally accompanied by a hypernova explosion (a very energetic supernova explosion). We further show that the binaries with evolved companions are good models for some of the ultraluminous X-ray sources (ULX's) recently seen by Chandra in other galaxies. The great regularity in our evolutionary history, especially the fact that most of the companions of ZAMS mass ≲ 2.5M⊙ remain in main sequences as K or M stars can be explained by the mass loss in common envelope evolution to be Case C; i.e. to occur only after core He burning has finished. Since our argument for Case C mass transfer is not generally understood in the community, we add an appendix, showing that with certain assumptions which we outline we can reproduce the regularities in the evolution of black hole binaries by Case C mass transfer.

scholarly journals Birth of the ELMs: a ZTF survey for evolved cataclysmic variables turning into extremely low-mass white dwarfs

2021 ◽  
Author(s):  
Kareem El-Badry ◽  
Hans-Walter Rix ◽  
Eliot Quataert ◽  
Thomas Kupfer ◽  
Ken J Shen
Keyword(s):  
Mass Transfer ◽  
White Dwarfs ◽  
Main Sequence ◽  
Cataclysmic Variables ◽  
Close Binaries ◽  
Convective Envelope ◽  
Compact Binary ◽  
Show Evidence ◽  
Low Mass ◽  
Hubble Time

Abstract We present a systematic survey for mass-transferring and recently-detached cataclysmic variables (CVs) with evolved secondaries, which are progenitors of extremely low mass white dwarfs (ELM WDs), AM CVn systems, and detached ultracompact binaries. We select targets below the main sequence in the Gaia colour-magnitude diagram with ZTF light curves showing large-amplitude ellipsoidal variability and orbital period Porb < 6 hr. This yields 51 candidates brighter than G = 18, of which we have obtained many-epoch spectra for 21. We confirm all 21 to be completely– or nearly–Roche lobe filling close binaries. 13 show evidence of ongoing mass transfer, which has likely just ceased in the other 8. Most of the secondaries are hotter than any previously known CV donors, with temperatures 4700 < Teff/K < 8000. Remarkably, all secondaries with $T_{\rm eff} \gtrsim 7000\, \rm K$ appear to be detached, while all cooler secondaries are still mass-transferring. This transition likely marks the temperature where magnetic braking becomes inefficient due to loss of the donor’s convective envelope. Most of the proto-WD secondaries have masses near 0.15 M⊙; their companions have masses near 0.8 M⊙. We infer a space density of $\sim 60\, \rm kpc^{-3}$, roughly 80 times lower than that of normal CVs and three times lower than that of ELM WDs. The implied Galactic birth rate, $\mathcal {R}\sim 60\, \rm Myr^{-1}$, is half that of AM CVn binaries. Most systems are well-described by MESA models for CVs in which mass transfer begins only as the donor leaves the main sequence. All are predicted to reach minimum periods 5 ≲ Porb/min ≲ 30 within a Hubble time, where they will become AM CVn binaries or merge. This sample triples the known evolved CV population and offers broad opportunities for improving understanding of the compact binary population.

scholarly journals Interacting young M-dwarfs in triple system – Par 1802 binary system case study

2019 ◽  
Vol 489 (2) ◽  
pp. 2298-2306 ◽  
Author(s):  
Shelley J Cheng ◽  
Alec M Vinson ◽  
Smadar Naoz
Keyword(s):  
Mass Transfer ◽  
Binary Systems ◽  
Main Sequence ◽  
Binary Star ◽  
Dynamical Evolution ◽  
Sequence Evolution ◽  
Proof Of Concept ◽  
Orion Nebula ◽  
Roche Limit ◽  
Tidal Heating

ABSTRACT The binary star Par 1802 in the Orion Nebula presents an interesting puzzle in the field of stellar dynamics and evolution. Binary systems such as Par 1802 are thought to form from the same natal material and thus the stellar members are expected to have very similar physical attributes. However, Par 1802’s stars have significantly different temperatures despite their identical (within $3\, {\rm per\, cent}$) masses of about 0.39 M⊙. The leading proof-of-concept idea is that a third companion gravitationally induced the two stars to orbit closer than their Roche limit, which facilitated heating through tidal effects. Here we expand on this idea and study the three-body dynamical evolution of such a system, including tidal and pre-main-sequence evolution. We also include tidal heating and mass transfer at the onset of Roche limit crossing. We show, as a proof-of-concept, that mass transfer combined with tidal heating can naturally explain the observed temperature discrepancy. We also predict the orbital configuration of the possible tertiary companion. Finally, we suggest that the dynamical evolution of such a system has pervasive consequences. We expect an abundance of systems to undergo mass transfer during their pre-main-sequence time, which can cause temperature differences.

scholarly journals The Evolution of Massive Close Binaries with Mass Loss and Overshooting. An Application to V729 Cyg (=BD+40 4220)

1986 ◽  
Vol 116 ◽  
pp. 399-400
Author(s):  
Christiaan H. B. Sybesma
Keyword(s):  
Mass Transfer ◽  
Mass Loss ◽  
Stellar Wind ◽  
Main Sequence ◽  
Classical Case ◽  
Type Systems ◽  
Close Binaries ◽  
Convective Core ◽  
Red Supergiants ◽  
V729 Cyg

The evolution of massive close binaries is altered if the effects of mass loss through a stellar wind and overshooting from the convective core are taken into account. The occurrence of mass transfer as well as the extent of the mass transfer itself differs from the classical case (Doom and De Greve 1983, Doom 1984). The main-sequence widening due to the enlargement of the convective core results in an enhancement of the frequency of case A of mass transfer. It occurs for initial periods much longer than in the classical case. A cosiderable number of early-type systems will therefore undergo this type of mass transfer (Sybesma, 1985b). Systems with primary masses larger than 35 M will most likely not undergo mass transfer at all as these stars do not form red supergiants if overshooting is coupled to the effects of mass loss through stellar wind. These systems will only be able to undergo case A of mass transfer, and then only for initial periods below 2–3 days.

scholarly journals Interaction Beyond the Main Sequence: One Recipe?

1992 ◽  
Vol 151 ◽  
pp. 41-50
Author(s):  
Jean-Pierre De Greve
Keyword(s):  
Mass Transfer ◽  
Phase Space ◽  
Main Sequence ◽  
Mass Range ◽  
Sequence Evolution ◽  
Helium Burning ◽  
The Core ◽  
Simple Concept ◽  
Homogeneous Set ◽  
Mass Ratios

We investigate the different aspects that govern the interaction of post-main-sequence evolution of binaries, using a new, homogeneous set of computations. The set describes the evolution of both components through the phase of mass transfer, till the end of the core helium burning of the primary. The mass range is 9 to 40 Mo, the mass ratios are 0.9 and 0.6 (and introducing 0.99 as a newcomer). Both for small and large masses we discuss the consequences of non-conservative mass transfer. Using a simple concept for the fraction β of transferred matter, we look to its value at the onset of mass transfer for various mass ratios and periods. Exploration of the phase space of interacting binaries reveals the influence of the various parameters on the dimensions of the resulting systems after mass transfer. Special attention is given to binaries with mass ratios very close to one. Their secondaries evolve directly into yellow supergiants such as observed in the LMC.

The Infancy of Solar-Type Stars and its Relevance for the Origin of Life

1997 ◽  
Vol 161 ◽  
pp. 267-282 ◽  
Author(s):  
Thierry Montmerle
Keyword(s):  
Main Sequence ◽  
Solar Nebula ◽  
Circumstellar Disks ◽  
T Tauri Stars ◽  
Necessary Condition ◽  
Sequence Evolution ◽  
T Tauri ◽  
Solar Type ◽  
Optical Domain ◽  
The Origin Of Life

AbstractFor life to develop, planets are a necessary condition. Likewise, for planets to form, stars must be surrounded by circumstellar disks, at least some time during their pre-main sequence evolution. Much progress has been made recently in the study of young solar-like stars. In the optical domain, these stars are known as «T Tauri stars». A significant number show IR excess, and other phenomena indirectly suggesting the presence of circumstellar disks. The current wisdom is that there is an evolutionary sequence from protostars to T Tauri stars. This sequence is characterized by the initial presence of disks, with lifetimes ~ 1-10 Myr after the intial collapse of a dense envelope having given birth to a star. While they are present, about 30% of the disks have masses larger than the minimum solar nebula. Their disappearance may correspond to the growth of dust grains, followed by planetesimal and planet formation, but this is not yet demonstrated.

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