We present a study of the orbital light curves of the recurrent nova IM Normae since its 2002 outburst. The broad “eclipses” recur with a 2.46 hr period, which increases on a timescale of 1.28(16) × 106yr. Under the assumption of conservative mass transfer, this suggests a rate near 10−7
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Abstract M ⊙yr−1, and this agrees with the estimatedaccretion rate of the postnova, based on our estimate of luminosity. IM Nor appears to be a close match to the famous recurrent nova T Pyxidis. Both stars appear to have very high accretion rates, sufficient to drive the recurrent-nova events. Both have quiescent light curves, which suggest strong heating of the low-mass secondary, and very wide orbital minima, which suggest obscuration of a large “corona” around the primary. And both have very rapid orbital period increases, as expected from a short-period binary with high mass transfer from the low-mass component. These two stars may represent a final stage of nova—and cataclysmic variable—evolution, in which irradiation-driven winds drive a high rate of mass transfer, thereby evaporating the donor star in a paroxysm of nova outbursts. -
Gosnell, Natalie M. ; Leiner, Emily M. ; Mathieu, Robert D. ; Geller, Aaron M. ; Knigge, Christian ; Sills, Alison ; Leigh, Nathan W. ( , The Astrophysical Journal)