A hidden population of massive white dwarfs: two spotted K + WD binaries
Article
Rowan, Dominick M, Jayasinghe, Tharindu, Tucker, Michael A., Lam, Casey Y., Thompson, Todd A., Kochanek, Christopher S., Abrams, Natasha S., Fulton, Benjamin J., Ilyin, Ilya, Isaacson, Howard, Lu, Jessica R., Martin, David V. and Nicholson, Belinda. 2024. "A hidden population of massive white dwarfs: two spotted K + WD binaries." Monthly Notices of the Royal Astronomical Society. 529, pp. 587-603. https://doi.org/10.1093/mnras/stae517
Article Title | A hidden population of massive white dwarfs: two spotted K + WD binaries |
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ERA Journal ID | 1074 |
Article Category | Article |
Authors | Rowan, Dominick M, Jayasinghe, Tharindu, Tucker, Michael A., Lam, Casey Y., Thompson, Todd A., Kochanek, Christopher S., Abrams, Natasha S., Fulton, Benjamin J., Ilyin, Ilya, Isaacson, Howard, Lu, Jessica R., Martin, David V. and Nicholson, Belinda |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 529, pp. 587-603 |
Number of Pages | 17 |
Year | 2024 |
Publisher | Oxford University Press |
Place of Publication | United States |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1093/mnras/stae517 |
Web Address (URL) | https://academic.oup.com/mnras/article/529/1/587/7610916 |
Abstract | The identification and characterization of massive (≳ 0.8 M⊙) white dwarfs is challenging in part due to their low luminosity. Here, we present two candidate single-lined spectroscopic binaries, Gaia DR3 4014708864481651840 and 5811237403155163520, with K-dwarf primaries and optically dark companions. Both have orbital periods of P ∼ 0.45 d and show rotational variability, ellipsoidal modulations, and high-amplitude radial velocity variations. Using light curves from the Transiting Exoplanet Survey Satellite (TESS), radial velocities from ground-based spectrographs, and spectral energy distributions, we characterize these binaries to describe the nature of the unseen companion. We find that both systems are consistent with a massive white dwarf companion. Unlike simple ellipsoidal variables, star-spots cause the light-curve morphology to change between TESS sectors. We attempt to constrain the orbital inclination using PHOEBE binary light-curve models, but degeneracies in the light curves of spotted stars prevent a precise determination. Finally, we search for similar objects using Gaia DR3 and TESS, and comment on these systems in the context of recently claimed compact object binaries. |
Keywords | binaries: spectroscopic; white dwarfs; Astrophysics - Solar and |
Contains Sensitive Content | Does not contain sensitive content |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
Public Notes | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2024 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
Byline Affiliations | Ohio State University, United States |
University of California Berkeley, United States | |
NASA Exoplanet Science Institute, United States | |
Leibniz Institute for Astrophysics Potsdam, Germany | |
Centre for Astrophysics | |
University of Oxford, United Kingdom |
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