CI Aql: a Type Ia supernova progenitor?

• Published in: Monthly notices of the Royal Astronomical Society 2013-08, Vol.433 (2), p.1588-1598
• Main Authors: Sahman, D. I., Dhillon, V. S., Marsh, T. R., Moll, S., Thoroughgood, T. D., Watson, C. A., Littlefair, S. P.
• Format: Article
• Language: English
• Subjects: Astrophysics; Measurement techniques; Spectrum analysis; Supernovae; White dwarfs; X-ray astronomy
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stt830

If recurrent novae are progenitors of Type Ia supernovae, their white dwarfs must have masses close to the Chandrasekhar limit. The most reliable means of determining white dwarf masses in recurrent novae is dynamically, via radial-velocity and rotational-broadening measurements of the companion star. Such measurements require the system to be both eclipsing and to show absorption features from the secondary star. Prior to the work reported here, the only dynamical mass estimate of a recurrent nova was for U Sco, which has a white dwarf mass of 1.55 ± 0.24 M. We present new time-resolved, intermediate-resolution spectroscopy of the eclipsing recurrent nova CI Aquilae (CI Aql) during quiescence. We find the mass of the white dwarf to be 1.00 ± 0.14 M and the mass of the secondary star to be 2.32 ± 0.19 M. We estimate the radius of the secondary to be 2.07 ± 0.06 R, implying that it is a slightly evolved early A-type star. The high mass ratio of q = 2.35 ± 0.24 and the high secondary-star mass implies that the mass transfer occurs on a thermal time-scale. We suggest that CI Aql is rapidly evolving into a supersoft X-ray source, and ultimately may explode as a Type Ia supernova within 10 Myr.