Orbital Periods for Three Recurrent Novae

Abstract

I report on the discovery of the orbital periods of three recurrent novae in our galaxy. V745 Sco has an orbital period of 510 ± 20 days with ellipsoidal modulations, based on SMARTS photometry from 2004-2008. V3890 Sgr has an orbital period of 519.7 ± 0.3 days with ellipsoidal modulations and a shallow eclipse, based primarily on SMARTS and AAVSO photometry from 1995-2008, but also extending back to 1899 with archival plates. In addition, a sinusoidal modulation of amplitude 0.2 mag and period 103.8 ± 0.4 days is seen mainly in the red, with this attributed to ordinary pulsations in the giant companion star. V394 CrA has an orbital period equal to twice its primary photometric period (P orb = 1.515682 ± 0.000008 days), as based on photometry extending from 1989-2008. I use all available information (including the UBVRIJHK spectral energy distributions) to get distances to the four RNe with red giant companions as 800 ± 140 pc for T CrB, 4300 ± 700 pc for RS Oph, 7300 ± 1200 pc for V745 Sco, and 6000 ± 1000 pc for V3890 Sgr. Further, the red giant in the RS Oph system has a mass loss rate of close to 3.7 × 10 −8 M ⊙ yr −1 as based on many confident measures, and this is too weak (by a factor of 100,000) to supply the white dwarf with mass at the known rate of 3.9 × 10 −6 M ⊙ yr −1 . Thus, the only way to get matter onto the white dwarf fast enough is through Roche lobe overflow, and this confidently demonstrates that the distance to RS Oph is 3000 pc.

The Change of the Orbital Periods Across Eruptions and the Ejected Mass for Recurrent Novae Ci Aquilae and U Scorpii

“…So I started a program for seeking photometric orbital modulation. This succeeded with the discovery of P for five RNe (Schaefer 1990(Schaefer , 2009Schaefer et al 1992). One of the early discoveries was that the RN U Scorpii (U Sco) was a deeply eclipsing binary with a 1.23 day orbital period.…”

Symbiotic Stars as Possible Progenitors of SNe Ia: Binary Parameters and Overall Outlook

“…So far, such changes have been detected in ∼ 30 % of the systems 164 J. Miko lajewska with orbital periods below ∼1000 days, including the three SyRNe (Miko lajewska 2007;Schaefer 2009;Gromadzki et al 2011, in preparation). Such changes can be, however, detected only in systems with relatively high inclination, and, in addition, they usually show up only in the red and near-IR light where the cool giant dominates the spectrum, whereas for most systems only the optical light curves are available.…”

The 2011 Eruption of the Recurrent Nova T Pyxidis: The Discovery, the Pre-Eruption Rise, the Pre-Eruption Orbital Period, and the Reason for the Long Delay

“…Schaefer 2008) so that most papers in the past decade give 1600 pc as the canonical distance by dint of sheer repetition (Schaefer 2009). For T Pyx, the bottom line is that all distances involving the strength of interstellar absorption are now known to be invalid.…”