The closest extremely low-mass white dwarf to the Sun

Adela Kawka; Jeffrey D. Simpson; Stéphane Vennes; Michael S. Bessell; Gary S. da Costa; Anna F. Marino; Simon J. Murphy

doi:10.1093/MNRASL/SLAA068

The closest extremely low-mass white dwarf to the Sun

Adela Kawka^*, Jeffrey D. Simpson, Stéphane Vennes, Michael S. Bessell, Gary S. da Costa, Anna F. Marino, Simon J. Murphy

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

7 Citations (Scopus)

Abstract

We present the orbit and properties of 2MASS J050051.85−093054.9, establishing it as the closest (d ≈ 71 pc) extremely low-mass white dwarf to the Sun. We find that this star is hydrogen rich with T_eff ≈ 10 500 K, log g ≈ 5.9, and, following evolutionary models, has a mass of ≈0.17 M☉. Independent analysis of radial velocity and Transiting Exoplanet Survey Satellite (TESS) photometric time series reveals an orbital period of ≈9.5 h. Its high velocity amplitude (K ≈ 144 km s⁻¹) produces a measurable Doppler beaming effect in the TESS light curve with an amplitude of 1 mmag. The unseen companion is most likely a faint white dwarf. J0500−0930 belongs to a class of post-common envelope systems that will most likely merge through unstable mass transfer and in specific circumstances lead to Type Ia supernova explosions.

Original language	English
Pages (from-to)	L129-L134
Journal	Monthly Notices of the Royal Astronomical Society: Letters
Volume	495
Issue number	1
DOIs	https://doi.org/10.1093/MNRASL/SLAA068
Publication status	Published - 2020

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10.1093/MNRASL/SLAA068

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title = "The closest extremely low-mass white dwarf to the Sun",

abstract = "We present the orbit and properties of 2MASS J050051.85−093054.9, establishing it as the closest (d ≈ 71 pc) extremely low-mass white dwarf to the Sun. We find that this star is hydrogen rich with Teff ≈ 10 500 K, log g ≈ 5.9, and, following evolutionary models, has a mass of ≈0.17 M☉. Independent analysis of radial velocity and Transiting Exoplanet Survey Satellite (TESS) photometric time series reveals an orbital period of ≈9.5 h. Its high velocity amplitude (K ≈ 144 km s−1) produces a measurable Doppler beaming effect in the TESS light curve with an amplitude of 1 mmag. The unseen companion is most likely a faint white dwarf. J0500−0930 belongs to a class of post-common envelope systems that will most likely merge through unstable mass transfer and in specific circumstances lead to Type Ia supernova explosions.",

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author = "Adela Kawka and Simpson, {Jeffrey D.} and St{\'e}phane Vennes and Bessell, {Michael S.} and {da Costa}, {Gary S.} and Marino, {Anna F.} and Murphy, {Simon J.}",

note = "Publisher Copyright: {\textcopyright} 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society",

year = "2020",

doi = "10.1093/MNRASL/SLAA068",

language = "English",

volume = "495",

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T1 - The closest extremely low-mass white dwarf to the Sun

AU - Kawka, Adela

AU - Simpson, Jeffrey D.

AU - Vennes, Stéphane

AU - Bessell, Michael S.

AU - da Costa, Gary S.

AU - Marino, Anna F.

AU - Murphy, Simon J.

PY - 2020

Y1 - 2020

N2 - We present the orbit and properties of 2MASS J050051.85−093054.9, establishing it as the closest (d ≈ 71 pc) extremely low-mass white dwarf to the Sun. We find that this star is hydrogen rich with Teff ≈ 10 500 K, log g ≈ 5.9, and, following evolutionary models, has a mass of ≈0.17 M☉. Independent analysis of radial velocity and Transiting Exoplanet Survey Satellite (TESS) photometric time series reveals an orbital period of ≈9.5 h. Its high velocity amplitude (K ≈ 144 km s−1) produces a measurable Doppler beaming effect in the TESS light curve with an amplitude of 1 mmag. The unseen companion is most likely a faint white dwarf. J0500−0930 belongs to a class of post-common envelope systems that will most likely merge through unstable mass transfer and in specific circumstances lead to Type Ia supernova explosions.

AB - We present the orbit and properties of 2MASS J050051.85−093054.9, establishing it as the closest (d ≈ 71 pc) extremely low-mass white dwarf to the Sun. We find that this star is hydrogen rich with Teff ≈ 10 500 K, log g ≈ 5.9, and, following evolutionary models, has a mass of ≈0.17 M☉. Independent analysis of radial velocity and Transiting Exoplanet Survey Satellite (TESS) photometric time series reveals an orbital period of ≈9.5 h. Its high velocity amplitude (K ≈ 144 km s−1) produces a measurable Doppler beaming effect in the TESS light curve with an amplitude of 1 mmag. The unseen companion is most likely a faint white dwarf. J0500−0930 belongs to a class of post-common envelope systems that will most likely merge through unstable mass transfer and in specific circumstances lead to Type Ia supernova explosions.

KW - Binaries: close

KW - Stars: individual: 2MASS J050051.85−093054.9

KW - White dwarfs

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DO - 10.1093/MNRASL/SLAA068

M3 - Article

SN - 1745-3925

VL - 495

SP - L129-L134

JO - Monthly Notices of the Royal Astronomical Society: Letters

JF - Monthly Notices of the Royal Astronomical Society: Letters

IS - 1

ER -

The closest extremely low-mass white dwarf to the Sun

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