Detection of a White Dwarf Companion to the White Dwarf SDSSJ125733.63+542850.5

Marsh, T. R.; Gänsicke, B. T.; Steeghs, D.; Southworth, J.; Koester, D.; Harris, Vandra; Merry, L.

doi:10.1088/0004-637x/736/2/95

Cited by 47 publications

(57 citation statements)

References 34 publications

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“…The temperature for the cool white dwarf is T1 = 6400 ± 37 ± 50 K, while its surface gravity is constrained to log g1 ∼ 6.0 -6.5 by the radius ratio (in turn constrained by the relative flux contributions of the two white dwarfs), yielding a best mass estimate of 0.24 M⊙, in agreement with Marsh et al (2011). Using evolutionary models we find that the age must be > 3 Gyrs, significantly longer than the 1.1 Gyr age of the hot white dwarf.…”

Section: Discussionsupporting

confidence: 59%

“…These deep, radialvelocity variable Balmer lines in fact originate in a cool, ELM white dwarf, which we hereafter refer to as the primary (because it dominates the flux at visual wavelengths, and following van Kerkwijk 2010 andMarsh et al 2011). The secondary is another white dwarf, which is hotter and significantly more massive, causing it to have very broad absorption lines.…”

Section: Introduction To Sdss J1257+5428mentioning

confidence: 99%

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A double white dwarf with a paradoxical origin?

Bours¹,

Marsh²,

Gänsicke³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present Hubble Space Telescope UV spectra of the 4.6 h period double white dwarf SDSS J125733.63+542850.5. Combined with Sloan Digital Sky Survey optical data, these reveal that the massive white dwarf (secondary) has an effective temperature T 2 = 13030 ± 70 ± 150 K and a surface gravity log g 2 = 8.73 ± 0.05 ± 0.05 (statistical and systematic uncertainties respectively), leading to a mass of M 2 = 1.06 M ⊙ . The temperature of the extremely low-mass white dwarf (primary) is substantially lower at T 1 = 6400 ± 37 ± 50 K, while its surface gravity is poorly constrained by the data. The relative flux contribution of the two white dwarfs across the spectrum provides a radius ratio of R 1 /R 2 ≃ 4.2, which, together with evolutionary models, allows us to calculate the cooling ages. The secondary massive white dwarf has a cooling age of ∼ 1 Gyr, while that of the primary low-mass white dwarf is likely to be much longer, possibly 5 Gyrs, depending on its mass and the strength of chemical diffusion. These results unexpectedly suggest that the low-mass white dwarf formed long before the massive white dwarf, a puzzling discovery which poses a paradox for binary evolution.

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Section: Discussionsupporting

confidence: 59%

Section: Introduction To Sdss J1257+5428mentioning

confidence: 99%

A double white dwarf with a paradoxical origin?

Bours¹,

Marsh²,

Gänsicke³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…Observed binary white dwarfs are overplotted with filled circles. Thick points taken are from Marsh et al (2011), thinner points from Tovmassian et al (2004); Napiwotzki et al (2005); Kulkarni & van Kerkwijk (2010); Brown et al (2010Brown et al ( , 2011Marsh et al (2011);Kilic et al (2011a,c,b), see Sect. 2.1 for a discussion.…”

Section: Seba -A Fast Stellar and Binary Evolution Codementioning

confidence: 99%

Supernova Type Ia progenitors from merging double white dwarfs

Toonen

Nelemans

Zwart

2012

A&A

316

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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“…Another mechanism is a common envelope induced by binary interactions (Iben & Livio 1993;Marsh et al 1995), making extremely low mass (ELM) He WDs (M He < 0.20 M or so) when the interaction occurs at the base of the RGB (see van Kerkwijk et al 1996). These ELM He WDs were first seen as companions to millisecond pulsars (e.g., Bassa et al 2006) or in high proper motion catalogs (Kawka et al 2006;Kawka & Vennes 2009), but the advent of the Sloan Digital Sky Survey (Eisenstein et al 2006) and other surveys revealed many additional ELM WDs (Kilic et al 2007b(Kilic et al , 2010b(Kilic et al , 2011c(Kilic et al , 2012Badenes et al 2009;Mullally et al 2009;Marsh et al 2011;Steinfadt et al 2010b;Parsons et al 2011;Marsh 2011;Brown et al 2011b;Vennes et al 2011, and Figure 1). ELM WDs were predicted to possess stably burning H envelopes (M env ∼ 10 −3 -10 −2 M ) that keep them bright for Gyr (Serenelli et al 2002;Panei et al 2007), and this has certainly aided the recent detections Brown et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Orbital Evolution of Compact White Dwarf Binaries

Kaplan

Bildsten

Steinfadt

2012

ApJ

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The newfound prevalence of extremely low mass (ELM, M He < 0.2 M ) helium white dwarfs (WDs) in tight binaries with more massive WDs has raised our interest in understanding the nature of their mass transfer. Possessing small (M env ∼ 10 −3 M ) but thick hydrogen envelopes, these objects have larger radii than cold WDs and so initiate mass transfer of H-rich material at orbital periods of 6-10 minutes. Building on the original work of D'Antona et al., we confirm the 10 6 yr period of continued inspiral with mass transfer of H-rich matter and highlight the fact that the inspiraling direct-impact double WD binary HM Cancri likely has an ELM WD donor. The ELM WDs have less of a radius expansion under mass loss, thus enabling a larger range of donor masses that can stably transfer matter and become a He mass transferring AM CVn binary. Even once in the long-lived AM CVn mass transferring stage, these He WDs have larger radii due to their higher entropy from the prolonged H-burning stage.

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Detection of a White Dwarf Companion to the White Dwarf SDSSJ125733.63+542850.5

Cited by 47 publications

References 34 publications

A double white dwarf with a paradoxical origin?

A double white dwarf with a paradoxical origin?

Supernova Type Ia progenitors from merging double white dwarfs

Orbital Evolution of Compact White Dwarf Binaries

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