Evidence of a Thermonuclear Runaway and Proton-Capture Material on a White Dwarf in a Dwarf Nova

Details Evidence of a Thermonuclear Runaway and Proton-Capture Material on a White Dwarf in a Dwarf Nova Evidence of a Thermonuclear Runaway and Proton-Capture Material on a White Dwarf in a Dwarf Nova

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...480l..17s&link_type=abstract

Astrophysical Journal Letters v.480, p.L17

Astronomy and Astrophysics

Astronomy

41

Stars: Novae, Cataclysmic Variables, Stars: Individual Constellation Name: Vw Hydri, Stars: White Dwarfs

Scientific paper

We present Hubble Space Telescope Goddard High-Resolution Spectrograph G160M spectra of the white dwarf in VW Hydri, exposed during quiescence, 1 month after the end of a normal dwarf nova outburst. Our spectra, covering the wavelength interval 1236--1272 A, were obtained at orbital phase 0.06--1.60; they reveal strong photospheric Si II lambda lambda 1260, 1265 absorption features and a previously unidentified broad feature centered around 1250 A. This feature is due to a blend of phosphorus lines. From line-shift measurements we determine a gravitational redshift of 58 +/- 33 km s-1, yielding a white dwarf mass Mwd = 0.86 ^{+0.18}_{-0.32} Msolar (this is only the second gravitational redshift determined for a cataclysmic variable white dwarf), white dwarf radius Rwd = 6.5 ^{+3.1}_{-1.5} x 108 cm, and gravity log g = 8.43 ^{+0.31}_{-0.54} . Our best-fitting synthetic spectra yield white dwarf effective temperature Twd = 22,000 K and a rotational velocity Vrot = 400 km s-1. The chemical abundances, in number relative to solar, are, for C, 0.5; N, 5.0; O, 2.0; Fe, 0.5; Si, 0.1; P, 900; and all other metals, 0.3. The abundance of phosphorus being 900 solar, coupled with the elevated aluminum abundance reported by Sion and coworkers, suggest nucleosynthetic production of these odd-numbered nuclei from proton capture on the even-numbered nuclei during a CNO thermonuclear runaway (TNR) on the white dwarf. It is clear that the white dwarf has undergone a runaway sometime in the past, the first such evidence of a TNR in a dwarf nova. A TNR on a slowly accreting 0.86 Msolar white dwarf should produce a classical nova explosion. If our interpretation is correct, then we have found the first direct spectroscopic link between a dwarf nova and a classical nova by using the white dwarf surface chemical abundance. This is also the first direct evidence of proton capture--processed material in the atmosphere of a white dwarf. Nova explosions on more numerous, lower mass C-O white dwarfs may therefore account for some fraction of the short-lived radionuclide 26Al in the Galaxy. This nuclide is observed from its Galactic gamma-ray line emission and is postulated to have an important role in the heating of small bodies in the solar system.

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