Orbital Period Changes Across the Recent Eruptions of Two Recurrent Novae, the Dynamical Measure of the Ejected Mass, and Whether These Will Become Type Ia Supernovae

Details Orbital Period Changes Across the Recent Eruptions of Two Recurrent Novae, the Dynamical Measure of the Ejected Mass, and Whether These Will Become Type Ia Supernovae Orbital Period Changes Across the Recent Eruptions of Two Recurrent Novae, the Dynamical Measure of the Ejected Mass, and Whether These Will Become Type Ia Supernovae

Feb 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011noao.prop...96s&link_type=abstract

NOAO Proposal ID #2011A-0096

Computer Science

Scientific paper

U Scorpii is the archetypal recurrent nova (RN) and is one of the best candidates for being a progenitor of Type Ia supernovae, but only if the nova eruption ejects less mass than is accreted during the previous cycle. The mass accreted can be measured to within roughly a factor of two, but the usual method for *measuring* (and modeling) the ejected mass has 3 orders-of-magnitude uncertainty. The only solution is to measure the orbital period change across the eruption, and for this I have eclipse times to produce accurate pre-eruption orbital periods for U Sco (across both its 1999 and 2010 eruptions) and CI Aql (2000 eruption). This two-decade program with big implications is nearing completion, but a final year or two is needed to pull out the mass ejected and to answer the question (``Are RNe the progenitors of Ia supernovae?"). Also, the most critical U Sco eclipse times for the 2010 eruption are those just after the eruption, so the proposed 2011 eclipse times are required to get a mass ejected for the 2010 eruption.

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