RE J0317 - 853: the hottest known highly magnetic DA white dwarf

Barstow, M. A.; Jordan, S.; O’Donoghue, D.; Burleigh, M. R.; Napiwotzki, R.; Harrop-Allin, M. K.

doi:10.1093/mnras/277.3.971

Cited by 143 publications

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“…Although the FGS photometry shows a peak-to-peak amplitude variation between V = 14.60 and V = 14.84 (with 0.01 accuracy estimated using LB 9802 as a reference) consistent with the result from Barstow et al (1995), the sampling was not good enough to confirm the 725 s photometric variability quantitatively by means of a Fourier analysis of this sparse data set.…”

Section: Analysis Of the Fgs Datamentioning

confidence: 67%

“…The optical spectrum together with UV observations taken with the IUE satellite and the Hubble Space Telescope (HST) indicated that RE J 0317-853 possesses a very high effective temperatures in the range from 30 000 to 55 000 K; Barstow et al (1995) achieved their best fit for about 49 000 K. A careful analysis of the EUVE spectrum using the interstellar medium Lyman lines to account for the interstellar extreme ultraviolet absorption implied an effective temperature of 33 800 K (Vennes et al 2003). Within these constraints, RE J 0317-853 is one of the hottest known magnetic white dwarf (MWD); in any case, it has Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.…”

Section: Introductionmentioning

confidence: 97%

“…the highest known temperature of all MWDs with a field strength above 20 MG (Kawka et al 2007;Külebi et al 2009). Barstow et al (1995) performed high-speed photometry demonstrating that the optical brightness of RE J 0317-853 varies almost sinusoidally with a period of 725.4 ± 0.9 s and an amplitude of more than 0. m 1; these results were confirmed by Vennes et al (2003), who inferred a period of 725.727 ± 0.001 s from the variation in the circular polarisation. The only reasonable explanation of these results is rotation, implying that RE J 0317-853 rotates more rapidly than any other known white dwarf that is not a member of a close binary.…”

Section: Introductionmentioning

confidence: 99%

“…This object was analysed initially by Barstow et al (1995), then later by Kawka et al (2007) (for fit parameters see Table 1). Barstow et al (1995) derived a distance in the range 33−37 pc with these parameters using the evolutionary models of Wood (1992). The physical companionship of LB 9802 and RE J 0317-853 has recently been confirmed by Spitzer IRAC observations (Farihi et al 2008) that demonstrated the common proper motion nature of the system.…”

Section: Introductionmentioning

confidence: 99%

“…With an effective temperature of 50 000 K and assuming a distance of 36 pc Barstow et al (1995) concluded that the radius of RE J 0317-853 is about 0.0035 R with a corresponding extreme mass of 1.35 M (log g = 9.5). Later Vennes & Kawka (2008) derived a mass of 1.32 ± 0.03 M using T eff = 33 800 K, log g = 9.4 and 27 pc for the distance.…”

Section: Introductionmentioning

confidence: 99%

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Constraints on the origin of the massive, hot, and rapidly rotating magnetic white dwarf RE J 0317-853 from an HST parallax measurement

Külebi

Jordan

Nelan

et al. 2010

A&A

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Aims. We use the parallax measurements of RE J 0317-853 to determine its mass, radius, and cooling age and thereby constrain its evolutionary origins. Methods. We observed RE J 0317-853 with the Hubble Space Telescope's Fine Guidance Sensor to measure the parallax of RE J 0317-853 and its binary companion, the non-magnetic white dwarf LB 9802. In addition, we acquired spectra of comparison stars with the Boller & Chivens spectrograph of the SMARTS telescope to correct the parallax zero point. For the corrected parallax, we determine the radius, mass, and the cooling age with the help of evolutionary models from the literature. Results. The properties of RE J 0317-853 are constrained using the parallax information. We discuss the different cases of the core composition and the uncertain effective temperature. We confirm that RE J 0317-853 is close to the Chandrasekhar's mass limit in all cases and almost as old as its companion LB 9802.Conclusions. The precise evolutionary history of RE J 0317-853 depends on our knowledge of its effective temperature. It is possible that it had a single star progenitor possible if we assume that the effective temperature is at the cooler end of the possible range from 30 000 to 50 000 K; if T eff is instead at the hotter end, a binary-merger scenario for RE J 0317-853 becomes more plausible.

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Section: Analysis Of the Fgs Datamentioning

confidence: 67%

Section: Introductionmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Constraints on the origin of the massive, hot, and rapidly rotating magnetic white dwarf RE J 0317-853 from an HST parallax measurement

Külebi

Jordan

Nelan

et al. 2010

A&A

Self Cite

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Magnetic deformation of the white dwarf surface structure

Fendt¹,

Dravins²

2000

Astron. Nachr.

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The influence of strong, large‐scale magnetic fields on the structure and temperature distribution in white dwarf atmospheres is investigated. Magnetic fields may provide an additional component of pressure support, thus possibly inflating the atmosphere compared to the non‐magnetic case. Since the magnetic forces are not isotropic, atmospheric properties may significantly deviate from spherical symmetry. In this paper the magnetohydrostatic equilibrium is calculated numerically in the radial direction for either for small deviations from different assumptions for the poloidal current distribution. We generally find indication that the scale height of the magnetic white dwarf atmosphere enlarges with magnetic field strength and/or poloidal current strength. This is in qualitative agreement with recent spectropolarimetric observations of Grw+10°8247. Quantitatively, we .nd for e.g. a mean surface poloidal field strength of 100 MG and a toroidal field strength of 2‐10 MG an increase of scale height by a factor of 10. This is indicating that already a small deviation from the initial force‐free dipolar magnetic field may lead to observable effects. We further propose the method of finite elements for the solution of the two‐dimensional magnetohydrostatic equilibrium including radiation transport in the diffusive approximation. We present and discuss preliminary solutions, again indicating on an expansion of the magnetized atmosphere.

show abstract

Magnetic deformation of the white dwarf surface structure

Fendt¹,

Dravins²

2000

Astron. Nachr.

View full text Add to dashboard Cite

The influence of strong, large-scale magnetic fields on the structure and temperature distribution in white dwarf atmospheres is investigated. Magnetic fields may provide an additional component of pressure support, thus possibly inflating the atmosphere compared to the non-magnetic case. Since the magnetic forces are not isotropic, atmospheric properties may significantly deviate from spherical symmetry. In this paper the magnetohydrostatic equilibrium is calculated numerically in the radial direction for either for small deviations from different assumptions for the poloidal current distribution. We generally find indication that the scale height of the magnetic white dwarf atmosphere enlarges with magnetic field strength and/or poloidal current strength. This is in qualitative agreement with recent spectropolarimetric observations of Grw+10 • 8247. Quantitatively, we find for e.g. a mean surface poloidal field strength of 100 MG and a toroidal field strength of 2-10 MG an increase of scale height by a factor of 10. This is indicating that already a small deviation from the initial force-free dipolar magnetic field may lead to observable effects. We further propose the method of finite elements for the solution of the two-dimensional magnetohydrostatic equilibrium including radiation transport in the diffusive approximation. We present and discuss preliminary solutions, again indicating on an expansion of the magnetized atmosphere.

show abstract

RE J0317 - 853: the hottest known highly magnetic DA white dwarf

Cited by 143 publications

References 0 publications

Constraints on the origin of the massive, hot, and rapidly rotating magnetic white dwarf RE J 0317-853 from an HST parallax measurement

Constraints on the origin of the massive, hot, and rapidly rotating magnetic white dwarf RE J 0317-853 from an HST parallax measurement

Magnetic deformation of the white dwarf surface structure

Magnetic deformation of the white dwarf surface structure

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