Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21349104s&link_type=abstract
American Astronomical Society, AAS Meeting #213, #491.04; Bulletin of the American Astronomical Society, Vol. 41, p.467
Astronomy and Astrophysics
Astronomy
1
Scientific paper
I collect virtually all photometry of the ten known galactic recurrent novae (RNe). This consists of my modern measures of nearly all archival plates (providing the only data for half of 37 known eruptions), my own 10,000 CCD magnitudes from 1987 to present (providing virtually all of the magnitudes in quiescence for seven RNe), over 140,000 visual magnitude estimates recorded by amateur astronomers (who discovered half the known eruptions), and the small scattering of magnitudes from all the literature. From this, I produce various uniform products; (1) BVRIJHK comparison star magnitudes and BV comparison star sequences to cover the entire range of eruption, (2) complete light curves for all eruptions, (3) best fit B and V light curve templates, (4) orbital periods for all-but-one RN, (5) exhaustive searches for all missed eruptions, (6) measured discovery efficiencies since 1890, (7) true recurrence time scales, (8) predicted next eruption dates, (9) variations on time scales of minutes, hours, days, months, years, decades, and century, (10) uniform distances and extinctions to all RNe, (11) BV colors at peak and UBVRIJHK colors at minimum all with extinction corrections, and (12) the spectral energy distributions over UBVRIJHK. Highlights of this work include the discoveries of one new RN, seven previously-undiscovered eruptions, and five new orbital periods. I have also measured the orbital period change of two RNe across recent eruptions with accuracies of 0.5 ppm, and I have determined the RN death rate in our Local Group to an accuracy of a factor of 3. An important utility of this work is the determination of whether RNe can be the progenitors of Type Ia supernovae, in particular, whether there are enough RNe to produce the observed supernova rate and whether the RN white dwarf is gaining mass over each eruption cycle.
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