Binary Stars among Cataclysmic Variables. II. Nova WZ Sagittae: a Possible Radiator of Gravitational Waves.

Kraft, Robert P.; Mathews, Jon; Greenstein, Jesse L.

doi:10.1086/147381

Cited by 149 publications

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“…Roche lobe filling can be achieved in consequence of the radius increase brought about by the nuclear evolution of a potential donor (e.g., Webbink et al, 1983;Taam, 1983a), or in consequence of orbital angular momentum loss due to gravitational wave radiation (GWR) (Kraft et al, 1962;Paczyń ski, 1967;Faulkner, 1971), or due to a magnetic stellar wind (MSW) (e.g., Verbunt and Zwaan, 1981;Taam, 1983b). In order for GWR to be important, A must be less than 2-3 R ᭪ (depending on component masses).…”

Section: Modes Of Mass Transfer and Of Orbital Angular Momentum Lossmentioning

confidence: 99%

“…For this reason, their consideration of hydrogen burning stopped at Na. The years following the publication of B 2 FH have seen (a) the discovery of the 22 Ne isotopic anomaly in meteorites (Black, 1972;Lewis et al, 1979;Eberhardt et al, 1979), (b) observations of anticorrelations of Na and Al with O in globular clusters (reviewed by Kraft, 1994 andKraft et al, 1997), and (c) observations of Na enhancements in red giant atmospheres (Takeda and Takada-Hidai, 1994). All of these effects are thought to arise from some form of a NeNa cycle, and so it has remained a topic of interest (additional details concerning Na and Al in globular clusters can be found in Sec.…”

Section: H Burning In the Nesi Region: Laboratory Studies A Intmentioning

confidence: 99%

“…Within the past few years proton captures by various isotopes from oxygen through magnesium have been invoked to explain the low oxygen combined with excess Na and Al in globular cluster red giants (Kraft, 1994;Kraft et al, 1997 and references therein). At the time of the writing of B 2 FH no member of a globular cluster had been analyzed in detail for its chemical composition.…”

Section: B O Depletion and The Enhancement Of Na And Almentioning

confidence: 99%

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Synthesis of the elements in stars: forty years of progress

et al. 1997

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Forty years ago Burbidge, Burbidge, Fowler, and Hoyle combined what we would now call fragmentary evidence from nuclear physics, stellar evolution and the abundances of elements and isotopes in the solar system as well as a few stars into a synthesis of remarkable ingenuity. Their review provided a foundation for forty years of research in all of the aspects of low energy nuclear experiments and theory, stellar modeling over a wide range of mass and composition, and abundance studies of many hundreds of stars, many of which have shown distinct evidence of the processes suggested by B 2 FH. In this review we summarize progress in each of these fields with emphasis on the most recent developments. [S0034-6861(97)

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Section: Modes Of Mass Transfer and Of Orbital Angular Momentum Lossmentioning

confidence: 99%

Section: H Burning In the Nesi Region: Laboratory Studies A Intmentioning

confidence: 99%

Section: B O Depletion and The Enhancement Of Na And Almentioning

confidence: 99%

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Synthesis of the elements in stars: forty years of progress

et al. 1997

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“…We assume that this mode takes place when the corresponding timescale τ J is shorter than the timescales at which the other three modes of mass transfer take place. Angular momentum loss can happen due to gravitational wave radiationJ gr (Kraft et al 1962) and magnetic brakingJ mb (Schatzman 1962;Huang 1966;Skumanich 1972;Verbunt & Zwaan 1981). Mass transfer proceeds on the time scale on which these processes occur: (A.20) where J b is the angular momentum of the circularized binary given by Eq.…”

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Supernova Type Ia progenitors from merging double white dwarfs

Toonen

Nelemans

Zwart

2012

A&A

305

386

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Context. The study of Type Ia supernovae (SNIa) has lead to greatly improved insights into many fields in astrophysics, e.g. cosmology, and also into the metal enrichment of the universe. Although a theoretical explanation of the origin of these events is still lacking, there is a general consensus that SNIa are caused by the thermonuclear explosions of carbon/oxygen white dwarfs with masses near the Chandrasekhar mass. Aims. We investigate the potential contribution to the supernova Type Ia rate from the population of merging double carbon-oxygen white dwarfs. We aim to develop a model that fits the observed SNIa progenitors as well as the observed close double white dwarf population. We differentiate between two scenarios for the common envelope (CE) evolution; the α-formalism based on the energy equation and the γ-formalism that is based on the angular momentum equation. In one model we apply the α-formalism throughout. In the second model the γ-formalism is applied, unless the binary contains a compact object or the CE is triggered by a tidal instability for which the α-formalism is used. Methods. The binary population synthesis code SeBa was used to evolve binary systems from the zero-age main sequence to the formation of double white dwarfs and subsequent mergers. SeBa has been thoroughly updated since the last publication of the content of the code.Results. The limited sample of observed double white dwarfs is better represented by the simulated population using the γ-formalism for the first CE phase than the α-formalism. For both CE formalisms, we find that although the morphology of the simulated delay time distribution matches that of the observations within the errors, the normalisation and time-integrated rate per stellar mass are a factor ∼7−12 lower than observed. Furthermore, the characteristics of the simulated populations of merging double carbon-oxygen white dwarfs are discussed and put in the context of alternative SNIa models for merging double white dwarfs.

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“…Jesse knew about this, said it was in Landau and Lifshitz and that I ought to talk to Jon Mathews of the Caltech physics department. Thus was born in 1962 [15] what I think is the first paper on gravitational radiation in the ordinary astronomical literature, when the three of us suggested [14] that WZ Sge might radiate gravitational waves on an interesting cosmic timescale. In 1966, I took this up again in a paper [15] in which I argued that gravitational-wave "grinding" might be a means of solving the mass-loss problem, since most of the late-type components in these systems seemed to be too faint for evolutionary expansion to be the dominant driving mechanism.…”

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confidence: 99%

Cataclysmic Variables as Binary Stars: Then and Now

Kraft

1990

International Astronomical Union Colloquium

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A brief history is given of the clues that led to the establishment, in the period c. 1950 to 1965, of a universal binary model for novae and related cataclysmic variables. The observational facts, established early in this period by A. H. Joy and R. F. Sanford (selected binary orbits), J. L. Greenstein (spectroscopy) and M. Walker (photometry) are reviewed, as are the theoretical ideas that formed the basis for the early models, viz

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Binary Stars among Cataclysmic Variables. II. Nova WZ Sagittae: a Possible Radiator of Gravitational Waves.

Cited by 149 publications

References 0 publications

Synthesis of the elements in stars: forty years of progress

Synthesis of the elements in stars: forty years of progress

Supernova Type Ia progenitors from merging double white dwarfs

Cataclysmic Variables as Binary Stars: Then and Now

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