Population synthesis for double white dwarfs

Nelemans, G.; Zwart, Simon F. Portegies; Verbunt, F.; Yungelson, L. R.

doi:10.1051/0004-6361:20010049

Cited by 289 publications

(521 citation statements)

References 49 publications

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“…Kulkarni & Narayan 1988;Naylor & Podsiadlowski 1993;Deloye 2008, and references therein), or ultracompact binaries (e.g. Nelemans et al 2001;Belczynski et al 2002).…”

Section: A Simple Model Of the Lmxb Luminosity Functionmentioning

confidence: 99%

On the nature of the break in the X-ray luminosity function of low-mass X-ray binaries

Revnivtsev

Постнов

Куранов

et al. 2011

A&A

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We analyze a flux-limited sample of persistent and bright (with 2-10 keV fluxes exceeding 1.4 × 10 −10 erg s −1 cm −2 ) low-mass X-ray binaries (LMXBs) in our Galaxy. It is demonstrated that the majority of binary systems with X-ray luminosities below log L(erg/s) ∼ 37.3 have unevolved secondary companions (except for those with white dwarf donors), while systems with higher X-ray luminosity harbor predominantly giant donors. Mass transfer in binary systems with giants significantly shortens their lifetime thus steepening the X-ray luminosity function of LMXBs at high luminosity. We argue that this is why the LMXB luminosity function constructed from observations of sources in our and distant galaxies demonstrates a break at log L(erg/s) ∼ 37.3.

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“…Kulkarni & Narayan 1988;Naylor & Podsiadlowski 1993;Deloye 2008, and references therein), or ultracompact binaries (e.g. Nelemans et al 2001;Belczynski et al 2002).…”

Section: A Simple Model Of the Lmxb Luminosity Functionmentioning

confidence: 99%

On the nature of the break in the X-ray luminosity function of low-mass X-ray binaries

Revnivtsev

Постнов

Куранов

et al. 2011

A&A

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“…Most of them could be consistent with either a cold (ZS) white-dwarf secondary or a larger SKH86/ TF89 secondary. ES Cet seems to be consistent only with a ZS secondary, but that error bar (only) does not include distance uncertainty, which is considerable, since the star is arguably 7 See Paczynski (1967) and Nelemans et al (2001) for a fuller discussion. The key point is that scales as at a fixed period, so the large spread…”

Section: ϫ5mentioning

confidence: 99%

The Helium‐rich Cataclysmic Variable ES Ceti

Espaillat

Patterson

Warner

et al. 2005

PUBL ASTRON SOC PAC

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ABSTRACT. We report photometry of the helium-rich cataclysmic variable ES Ceti during [2001][2002][2003][2004]. The star is roughly stable at and has a light curve dominated by a single period of 620 s, which remains measurably V ∼ 17.0 constant over the 3 yr baseline. The weight of evidence suggests that this is the true orbital period of the underlying binary, not a "superhump" as initially assumed. We report GALEX ultraviolet magnitudes that establish a very blue flux distribution and therefore a large bolometric correction. Other evidence (the very strong He ii l4686emission and a ROSAT detection in soft X-rays) also indicates a strong EUV source, and comparison to helium atmosphere models suggests a temperature of kK. For a distance of 350 pc, we estimate a luminosity of 130 ‫ע‬ 10 ergs s Ϫ1 , yielding a mass accretion rate of M , yr Ϫ1 onto an assumed 0.7 M , white 34 Ϫ9(0.8-1.7) # 10 (2-4) # 10 dwarf. This appears to be about as expected for white dwarfs orbiting each other in a 10 minute binary, assuming that mass transfer is powered by gravitational radiation losses. We estimate mean accretion rates for other heliumrich cataclysmic variables and find that they also follow the expected relation. There is some evidence Ϫ5M ∼ P o (the lack of superhumps and the small apparent size of the luminous region) that the mass-transfer stream in ES Cet directly strikes the white dwarf, rather than circularizing to form an accretion disk.

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“…AM CVn systems are discussed to contribute significantly to the Type Ia supernova production rate (Nelemans et al 2001;Solheim & Yungelson 2005). Furthermore, they are sources of low-frequency gravitational wave radiation, which will be detectable with the future Laser Interferometer Space Antenna LISA (e.g., Hils & Bender 2000).…”

Section: Introductionmentioning

confidence: 99%

A new grid of NLTE accretion-disc models for AM CVn systems: application to CE 315

Nagel¹,

Rauch²,

Werner³

2009

A&A

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Context. AM CVn stars are very compact interacting binary systems with helium-dominated spectra. The nature of the donor star remains unclear, but the accretion disc represents the chemical composition of the donor's atmosphere. Analysing the disc will therefore help us to understand the donor star and the formation of these systems. Aims. We investigate the influence of primary mass, mass-accretion rate, chemical abundances, irradiation by the primary, and inclination on the spectrum of the accretion disc to determine the extent to which it is possible to deduce these system properties by comparison with observed spectra. Methods. We compute a grid of metal-line blanketed NLTE accretion-disc spectra for an extensive parameter space by solving selfconsistently the radiative-transfer equations and the equations describing the vertical structure using our accretion disc code AcDc. Results. We detect emission-line spectra for low and absorption-line spectra for high mass-accretion rates. Irradiation of the accretion disc by the primary has almost no influence on the spectrum. The spectroscopic detection of the primary is achievable most easily in the UV. Comparing an observed spectrum of CE 315 with our accretion-disc models, we find the qualitatively closest match for a 0.8 M primary and a mass-accretion rate of 10 −11 M /yr. Furthermore, the disc of CE 315 exhibits a strong silicon underabundance confirming the hypothesis that it is a Pop. II object.

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Population synthesis for double white dwarfs

Cited by 289 publications

References 49 publications

On the nature of the break in the X-ray luminosity function of low-mass X-ray binaries

On the nature of the break in the X-ray luminosity function of low-mass X-ray binaries

The Helium‐rich Cataclysmic Variable ES Ceti

A new grid of NLTE accretion-disc models for AM CVn systems: application to CE 315

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