Single magnetic white dwarfs with Balmer emission lines: a small class with consistent physical characteristics as possible signposts for close-in planetary companions. Issue 2 (29th September 2020)

• Record Type: Journal Article
• Authors: Gänsicke, Boris T; Rodríguez-Gil, Pablo; Gentile Fusillo, Nicola P; Inight, Keith; Schreiber, Matthias R; Pala, Anna F; Tremblay, Pier-Emmanuel
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 499:Issue 2(2020)
• Page Start: 2564
• Page End: 2574
• Publication Date: 2020-09-29
• Subjects: stars: abundances -- stars: individual: SDSS J121929.45+471522.8 -- planet-star interactions -- white dwarfs; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa2969
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We report the identification of SDSS J121929.45+471522.8 as the third apparently isolated magnetic ( B ≃ 18.5 ± 1.0 MG) white dwarf exhibiting Zeeman-split Balmer emission lines. The star shows coherent variability at optical wavelengths with an amplitude of ≃0.03 mag and a period of 15.26 h, which we interpret as the spin period of the white dwarf. Modelling the spectral energy distribution and Gaia parallax, we derive a white dwarf temperature of 7500 ± 148 K, a mass of 0.649 ± 0.022 M⊙, and a cooling age of 1.5 ± 0.1 Gyr, as well as an upper limit on the temperature of a sub-stellar or giant planet companion of ≃250 K. The physical properties of this white dwarf match very closely those of the other two magnetic white dwarfs showing Balmer emission lines: GD356 and SDSS J125230.93−023417.7. We argue that, considering the growing evidence for planets and planetesimals on close orbits around white dwarfs, the unipolar inductor model provides a plausible scenario to explain the characteristics of this small class of stars. The tight clustering of the three stars in cooling age suggests a common mechanism switching the unipolar inductor on and off. Whereas Lorentz drift naturally limits the lifetime of the inductor phase, the relatively late onset of the line emission along the white dwarf cooling sequence remains unexplained.