The evolutionary history of GD 1400AB, a white dwarf–brown dwarf binary

ABSTRACT GD1400AB was one of the first known white dwarf $+$ brown dwarf binaries and is the only one of these systems where the white dwarf is a ZZ Ceti pulsator. Here, we present both radial velocity measurements and time-series photometry, analysing both the white dwarf pulsations and the effects of irradiation on the brown dwarf. We find that the brightness temperatures of 1760 $\pm $ 10 K for the nightside and 1860 $\pm$ 10 K for the dayside indicate that the brown dwarf is hotter than spectra have previously suggested, although brightness temperatures calculated using a larger radius for the brown dwarf are consistent with previously determined spectral types. We also discuss the likely evolutionary pathway of this binary and put its common envelope phase into context with the other known systems.

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Publication Details

Journal
Monthly Notices of the Royal Astronomical Society
Published
2024-10-07
DOI
https://doi.org/10.1093/mnras/stae2301
Citations
6
Primary Topic
Stellar, planetary, and galactic studies
Type
article
Field-Weighted Citation Impact
1.99

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article

The evolutionary history of GD 1400AB, a white dwarf–brown dwarf binary

M. R. Burleigh, J. J. Hermes, S. L. Casewell, P. Bergeron et al.
6 citations
Monthly Notices of the Royal Astronomical Society
Stellar, planetary, and galactic studies
1.99
article

The evolutionary history of GD 1400AB, a white dwarf–brown dwarf binary

M. R. Burleigh, J. J. Hermes, S. L. Casewell, P. Bergeron, M. Zorotovic, Jenni R French, F. Faedi, R. Napiwotzki, K L Lawrie
article en
6 citations

Abstract

ABSTRACT GD1400AB was one of the first known white dwarf $+$ brown dwarf binaries and is the only one of these systems where the white dwarf is a ZZ Ceti pulsator. Here, we present both radial velocity measurements and time-series photometry, analysing both the white dwarf pulsations and the effects of irradiation on the brown dwarf. We find that the brightness temperatures of 1760 $\pm $ 10 K for the nightside and 1860 $\pm$ 10 K for the dayside indicate that the brown dwarf is hotter than spectra have previously suggested, although brightness temperatures calculated using a larger radius for the brown dwarf are consistent with previously determined spectral types. We also discuss the likely evolutionary pathway of this binary and put its common envelope phase into context with the other known systems.

Monthly Notices of the Royal Astronomical SocietyVol. 535(1)
Boston University (US), University of Hertfordshire (GB), University of Leicester (GB), Université de Montréal (CA), University of Valparaíso (CL)
National Aeronautics and Space Administration, University of California, California Institute of Technology, Jet Propulsion Laboratory, Natural Sciences and Engineering Research Council of Canada, Science and Technology Facilities Council
Openalex Percentile: Top 14%
Stellar, planetary, and galactic studies
1.99
DOIOpen Access PDFOpenAlex
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