V1460 Her: A fast spinning white dwarf accreting from an evolved donor star
| Autor: | Matthew R. Burleigh, Odette Toloza, Richard Ashley, Elmé Breedt, John R. Thorstensen, Paul Chote, A. F. Pala, T. R. Marsh, Boris T. Gänsicke |
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| Rok vydání: | 2020 |
| Předmět: |
Astrophysics::High Energy Astrophysical Phenomena
Cataclysmic variable star FOS: Physical sciences Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics 7. Clean energy 01 natural sciences Spectral line Orbital inclination Photometry (optics) 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Emission spectrum 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics Solar and Stellar Astrophysics (astro-ph.SR) QB Physics 010308 nuclear & particles physics White dwarf Astronomy and Astrophysics Orbital period Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science Astrophysics::Earth and Planetary Astrophysics Main sequence |
| ISSN: | 1745-3933 |
| DOI: | 10.48550/arxiv.2008.13242 |
| Popis: | We present time-resolved optical and ultraviolet (UV) spectroscopy and photometry of V1460 Her, an eclipsing cataclysmic variable with a 4.99-h orbital period and an overluminous K5-type donor star. The optical spectra show emission lines from an accretion disc along with absorption lines from the donor. We use these to measure radial velocities, which, together with constraints upon the orbital inclination from photometry, imply masses of $M_1=0.869\pm 0.006\, \mathrm{M}_\odot$ and $M_2=0.295\pm 0.004\, \mathrm{M}_\odot$ for the white dwarf and the donor. The radius of the donor, $R_2=0.43\pm 0.002\, \mathrm{\it R}_\odot$, is ≈50 per cent larger than expected given its mass, while its spectral type is much earlier than the M3.5 type that would be expected from a main-sequence star with a similar mass. Hubble Space Telescope (HST) spectra show strong N v 1240-Å emission but no C iv 1550-Å emission, evidence for CNO-processed material. The donor is therefore a bloated, overluminous remnant of a thermal time-scale stage of high mass transfer and has yet to reestablish thermal equilibrium. Remarkably, the HST UV data also show a strong 30 per cent peak-to-peak, $38.9\,$s pulsation that we explain as being due to the spin of the white dwarf, potentially putting V1460 Her in a similar category to the propeller system AE Aqr in terms of its spin frequency and evolutionary path. AE Aqr also features a post-thermal time-scale mass donor, and V1460 Her may therefore be its weak magnetic field analogue since the accretion disc is still present, with the white dwarf spin-up a result of a recent high accretion rate. |
| Databáze: | OpenAIRE |
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