scholarly journals The influence of mass loss on the evolution of binaries

1981 ◽  
Vol 59 ◽  
pp. 405-430 ◽  
Author(s):  
C. de Loore
Keyword(s):  
Neutron Star ◽  
Mass Loss ◽  
Massive Stars ◽  
Compact Object ◽  
Supernova Explosion ◽  
Sequence Evolution ◽  
Chemical Abundances ◽  
Low Mass Stars ◽  
Object A ◽  
The Masses

Mass loss can affect the evolution of binaries in various ways, during different stages of the evolution.1. For massive stars stellar wind mass loss will change the masses of the components during their main sequence evolution.2. During the Roche lobe overflow phase (or tidal interaction phase) matter can leave the system.3. For low mass stars matter can leave the system during the mass exchange phase and can be stored in envelopes, disks or rings.4. Sufficiently massive stars(>8-15M0) undergo at the end of their life a supernova explosion, where most of the matter is blown away and a compact object, a neutron star or a black hole can be left.5. For intermediate stars one of the components can evolve into a degenerate He or CO dwarf; a reverse mass transfer can dump matter on this degenerate dwarf. If the conditions are favorable the white dwarf can explode with loss of matter, and a neutron star can be the result.6. The chemical abundances in the outer layers change.

scholarly journals The O-type spectroscopic binary system HD 93206

1979 ◽  
Vol 83 ◽  
pp. 277-280 ◽  
Author(s):  
Nancy D. Morrison ◽  
Peter S. Conti
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Mass Loss ◽  
Massive Stars ◽  
Radial Velocities ◽  
Mass Determination ◽  
Spectroscopic Binary ◽  
The Masses

The star HD 93206 (=QZ Carinae) is a double-lined (Conti et al. 1977), eclipsing (Moffat and Seggewiss 1972) binary with a period of 6 d. Walborn (1973) classified it 09.7Ib:(n). Since the star is probably a member of the cluster Collander 228 (which is near η Carinae), its distance can be assumed to be 2600 pc. In principle, one can determine the masses of the components of HD 93206 from observations of the radial velocities and the light curve, and a spectroscopic orbit is the object of this investigation. A mass determination for an evolved star such as this one is especially important for checking recently computed evolutionary tracks with mass loss for massive stars (de Loore et al. 1977, Chiosi et al. 1978, Dearborn et al. 1978).

Forming the Progenitors of Explosive Stellar Transients

2017 ◽  
Vol 14 (S339) ◽  
pp. 33-38
Author(s):  
S. Justham
Keyword(s):  
Neutron Star ◽  
Massive Stars ◽  
Deep Understanding ◽  
Compact Object ◽  
Core Collapse ◽  
Synoptic View

AbstractExplosive stellar transients arise from diverse situations, including deaths of massive stars, a variety of thermonuclear outbursts, and compact-object mergers. Stellar interactions are heavily implicated in explaining the observed populations of events, and not only those where binarity is obviously involved. Relationships between these classes probably help to elucidate our understanding; for example; the production of double neutron-star mergers from field binaries is thought to be heavily biased towards routes involving stripped core-collapse supernovæ. As we gain an ever more synoptic view of the changing sky, theorists should be mindful of developing an ability to take robust quantitative advantage of the available population information to help constrain the physics. This is complementary to aiming for deep understanding of individual events.

scholarly journals Episodic Mass Loss and Pre-SN Circumstellar Envelopes

2007 ◽  
Vol 3 (S250) ◽  
pp. 193-200 ◽  
Author(s):  
Nathan Smith
Keyword(s):  
Mass Loss ◽  
Stellar Evolution ◽  
Massive Stars ◽  
Supernova Explosion ◽  
Circumstellar Envelopes ◽  
Observational Fact ◽  
Solar Metallicity ◽  
The 19Th Century ◽  
Very High ◽  
Circumstellar Environment

AbstractI discuss observational clues concerning episodic mass-loss properties of massive stars in the time before the final supernova explosion. In particular, I will focus on the mounting evidence that LBVs and related stars are candidates for supernova progenitors, even though current paradigms place them at the end of core-H burning. Namely, conditions in the immediate circumstellar environment within a few 102 AU of Type IIn supernovae require very high progenitor mass-loss rates. Those rates are so high that the only known stars that come close are LBVs during rare giant eruptions. I will highlight evidence from observations of some recent extraordinary supernovae suggesting that explosive or episodic mass loss (a.k.a. LBV eruptions like the 19th century eruption of Eta Car) occur in the 5-10 years immediately preceding the SN. Finally, I will discuss some implications for stellar evolution from these SNe, the most important of which is the observational fact that the most massive stars can indeed make it to the ends of their lives with substantial H envelopes intact, even at Solar metallicity.

scholarly journals Chemical Abundances of the Secondary Stars in the Black Hole Binary A0620-00 and the Neutron Star Binary Cen X-4

2004 ◽  
Vol 194 ◽  
pp. 204-204
Author(s):  
J. I. González-Hernández ◽  
R. Rebolo ◽  
G. Israelian ◽  
J. Casares
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
High Resolution ◽  
Compact Object ◽  
Accretion Disc ◽  
Accretion Discs ◽  
Chemical Abundances ◽  
X Ray ◽  
Black Hole Binary ◽  
Star Binary

We have determined abundances in the secondary stars of the black hole X-ray binary A0620-00 and the neutron star Binary Cen X-4. These are K type stars veiled by the emission produced by the respective accretion discs. We searched for evidence of nucleosynthetic products from the progenitor of the compact object that could have contaminated the secondary stars (as in Israelian et al., 1999).Using high resolution spectra obtained with VLT/UVES, we have derived in a consistent way stellar parameters and the veiling caused by the accretion disc.

scholarly journals Constraints on Stellar Evolution from Observations of Compact Object Binaries

2004 ◽  
Vol 194 ◽  
pp. 266-266
Author(s):  
T. Bulik ◽  
R. Moderski ◽  
K. Belczyński
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Gravitational Waves ◽  
Stellar Evolution ◽  
Compact Object ◽  
Selection Effects ◽  
Common Envelope ◽  
Mass Ratios ◽  
The Masses

The masses of compact object (black hole, neutron star) binaries depend strongly on the parameters describing stellar evolution. Such masses or their functions can be measured using gravitational waves or through microlensing searches. We analyze an example of the varying common envelope efficiency and show the dependence of distributions of the measured chirp masses in gravitational waves mass ratios through microlensing taking into account the relevant selection effects.

Non-conservative Evolution of Massive O-Type Close Binaries with Galactic and with Magellanic Cloud Chemical Abundances

1981 ◽  
Vol 93 ◽  
pp. 183-183
Author(s):  
D. Vanbeveren
Keyword(s):  
Mass Loss ◽  
Stellar Wind ◽  
Supernova Explosion ◽  
Large Mass ◽  
Close Binaries ◽  
Chemical Abundances ◽  
Average Mass ◽  
Evolutionary Pattern ◽  
Evolutionary Phase ◽  
The Difference

The general evolutionary pattern of massive O type close binaries evolving according to a case B mode of mass transfer, including mass loss by stellar wind prior to Roche lobe overflow (RLOF) at rates appropriate for O type stars, only marginally depends on the choice of the initial chemical composition whether the galactic or the MC abundances are used (the difference never exceeds 10%). The theoretical results are compared to the observations, O type binaries describing the evolutionary phase prior to RLOF, WR type binaries describing the helium burning phase after RLOF. The large mass loss by stellar wind in WR stars considerably affects the evolution during the latter phase. The comparison yields the following conclusions:a) from the ZAMS up to the WR stage, 50%-60% of the initial primary mass is leaving the system corresponding to at least 70%–80% of the total mass lost by the primary due to stellar wind and RLOF;b) during the WR phase the star is losing approximately half of its mass;c) the average mass ratio for binaries prior to the supernova explosion equals 3, i.e. the exploding star is 3 times less massive than its companion.

Effects of mass loss on the evolution of massive stars. I - Main-sequence evolution

1978 ◽  
Vol 223 ◽  
pp. 552 ◽  
Author(s):  
D. S. P. Dearborn ◽  
J. B. Blake ◽  
K. L. Hainebach ◽  
D. N. Schramm
Keyword(s):  
Mass Loss ◽  
Main Sequence ◽  
Massive Stars ◽  
Sequence Evolution

scholarly journals Analysis of Neutrino Burst from the Supernova in the Large Magellanic Cloud

1988 ◽  
Vol 108 ◽  
pp. 424-425
Author(s):  
Hideyuki Suzuki ◽  
Katsuhiko Sato
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Binding Energy ◽  
Massive Star ◽  
Compact Object ◽  
Supernova Explosion ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

A massive star has been believed to end his life with the collapsed driven supernova explosion and the formation of the compact object such as a neutron star or a black hole. When the compact object is formed, a large amount of energy corresponding to the binding energy of the object must be released. It has been considered that most of the energy is emitted by neutrinos because of their adequate coupling with the matter. The observation of the neutrino burst from SN1987A by Kamiokande and IMB offered us the first chance to test these scenarios of the collapse driven supernova explosion directly. We began to analyze the data just after their publication and got many important results which are presented below. In our analysis the distance of SN1987A is assumed to be 50kpc.

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.

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