RE1016 - 05: a white dwarf binary discovered with the ROSAT Wide Field Camera

Jomaron, C. M.; Branduardi‐Raymont, G.; Bromage, G. E.; Hassall, B. J. M.; Hodgkin, S. T.; Mason, K. O.; Naylor, T.; Watson, M. G.

doi:10.1093/mnras/264.1.219

Cited by 8 publications

(6 citation statements)

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“…Our Hamilton echelle spectrum corroborates the estimated spectral type, since the spectrum of EUVE J1016[053C appears very similar in overall appearance to that of Gliese 526, which Boeshaar classiÐed as M1.5. Jomaron et al (1993) estimate a dK8ÈdM1 classiÐcation, just consistent with our value.…”

Section: A Note On the Companion Of Euv E J1016[053supporting

confidence: 91%

“…Finder charts are available in Vennes & Thorstensen (1994b), Jomaron et al (1993), and Thorstensen et al (1994). The three new systems are more distant and fainter both in the optical and FUV spectral ranges.…”

Section: Fuv and Optical Spectroscopymentioning

confidence: 99%

“…The parentheses enclose formal 1 p uncertainties in the last digits quoted. EUV E J1016[053.ÈOur data now extend to 1998 June, and the total span of all available data (including that of Jomaron et al 1993) is 2167 days. The updated ephemeris for EUVE J1016[053 is…”

Section: Improved Orbital Periods and Ephemeridesmentioning

confidence: 99%

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Stellar Masses, Kinematics, and White Dwarf Composition for Three Close DA+dMe Binaries

Vennes

Thorstensen

Polomski

1999

ApJ

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We determine the mass functions and mass ratios for three close white dwarf plus red dwarf binaries (EUVE J0720[317, 1016[053, and 2013]400). Hubble Space T elescope Goddard High-Resolution Spectrograph spectra of the He II j1640 and C IV j1550 spectral lines trace the white dwarf orbital motion, and Hamilton Spectrograph echelle spectra (Lick Observatory) and lower dispersion spectra trace the red dwarf orbital motion. The data sets allow us to measure orbital periods and velocities, as well as the white dwarf gravitational redshifts. The red dwarf and white dwarf mass estimates obtained from a combination of independent mass measurements for the white dwarf stars and our new orbital elements help constrain probable evolutionary outcomes. We Ðnd that EUVE J0720[317 will probably come into contact within a Hubble time and that the mass transfer will be unstable on a dynamical time. We also conclude that the much lower secondary masses in EUVE J1016[053 and EUVE J2013]400 exclude the possibility of signiÐcant interaction in these systems. We also present new helium and carbon photospheric abundance measurements in the three white dwarfs. The white dwarf atmospheric composition may show the e †ects of accretion of red dwarf mass-loss material onto its surface. Finally, we study the kinematics of the systems, and we also show that the white dwarf in EUVE J1016[053 is part of a quadruple system.

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Section: A Note On the Companion Of Euv E J1016[053supporting

confidence: 91%

Section: Fuv and Optical Spectroscopymentioning

confidence: 99%

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Stellar Masses, Kinematics, and White Dwarf Composition for Three Close DA+dMe Binaries

Vennes

Thorstensen

Polomski

1999

ApJ

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“…RE 1016-053: Discovered as bright EUV source during the ROSAT Wide Field Camera all-sky survey and listed as a WD by Pounds et al (1993), classified as DA+dM by Jomaron et al (1993), orbital period (spectroscopic) measured by Tweedy et al (1993).…”

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confidence: 99%

The age, life expectancy, and space density of Post Common Envelope Binaries

Schreiber

Gänsicke

2003

A&A

182

242

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Abstract. We present a sample of 30 well observed Post Common Envelope Binaries (PCEBs). Deriving the cooling age of the white dwarfs, we show that the PCEB population is dominated by young systems. Having calculated the orbital evolution of the systems under the assumption of two different prescriptions for the angular momentum loss, we find that most of the systems have not yet completed a significant fraction of their PCEB life time. We therefore predict the existence of a large population of old PCEBs containing cold white dwarfs (T eff < ∼ 15 000 K). Our calculations show that nearly half of the PCEBs in our sample will evolve into a semi-detached configuration and start mass transfer in less than the Hubble-time. These systems are thus representative for progenitors of the current CV population. Only one of them (V471 Tau) will evolve into a long-period (P orb > ∼ 4 h) CV, and a significant fraction of the systems will start mass transfer in the period gap. Having estimated the distances of the PCEBs in the sample, we derive a space density of ρ PCEB ∼ 6−30 × 10 −6 pc −3 , depending on the assumed angular momentum loss prescription. Taking into account the evolutionary time scales we compute a lower limit for the CV space density, predicted by the currently known PCEB population of ρ CV > ∼ 10 −5 pc −3 . Finally, we discuss possible observational selection effects and conclude that the observed PCEB population is probably highly incomplete.

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“…The pre-cataclysmic binary EUVE J1016Ϫ053 was first identified in the ROSAT Wide Field Camera sky survey (RE 1016Ϫ053; Jomaron et al 1993;Tweedy et al 1993) and subsequently in the Extreme Ultraviolet Explorer (EUVE) allsky survey (Bowyer et al 1994). Thorstensen, Vennes, & Bowyer (1996) measured an orbital period of 0.78929 days.…”

Section: Introductionmentioning

confidence: 99%

The Accreting White Dwarf in the Close Binary EUVE J1016−053

Vennes

Dupuis

Bowyer

et al. 1997

The Astrophysical Journal

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The hot white dwarf in the close binary EUVE J1016Ϫ053 (ϭRE 1016Ϫ053) has been classified as a DAO white dwarf; its mixed H͞He composition has been attributed to steady accretion from the close red dwarf companion. We have obtained extreme-ultraviolet (EUV) photometric and spectroscopic observations of EUVE J1016Ϫ053 with the Extreme Ultraviolet Explorer (EUVE). We report the discovery of a 230% EUV flux variation over a period of 57.3 minutes, which we attribute to surface abundance inhomogeneities modulated over the stellar rotation period, P rot . The EUVE spectrum shows the effect of heavy-element opacities on the white dwarf EUV energy distribution. Spectral synthesis including trace opacities of helium and a group of heavy elements (C, N, O, Si, S, Fe) in the otherwise hydrogen-rich atmosphere constrains abundances to Y͞Y J ϭ Z͞Z J ϭ 2 ϫ 10 Ϫ3 , in support of a simple accretion model. The low surface-averaged helium abundance measured in the white dwarf atmosphere limits the accretion rate to between 10 Ϫ19 and 10 Ϫ18 M J yr Ϫ1 , i.e., much lower than the Bondi-Hoyle accretion rate, which is of the same order as the red dwarf mass-loss rate (Ն10 Ϫ14 M J yr Ϫ1 ), therefore invalidating a simple wind-accretion model. We speculate that weak mass loss from the white dwarf or interaction with a magnetosphere may inhibit accretion onto the white dwarf. Accretion of heavy elements may also be restricted to smaller areas, possibly correlating to magnetic poles.

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RE1016 - 05: a white dwarf binary discovered with the ROSAT Wide Field Camera

Cited by 8 publications

References 0 publications

Stellar Masses, Kinematics, and White Dwarf Composition for Three Close DA+dMe Binaries

Stellar Masses, Kinematics, and White Dwarf Composition for Three Close DA+dMe Binaries

The age, life expectancy, and space density of Post Common Envelope Binaries

The Accreting White Dwarf in the Close Binary EUVE J1016−053

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