The Unique Recurrent Nova T Pyxidis: The Decline and Transition to Quiescence The Unique Recurrent Nova T Pyxidis: The Decline and Transition to Quiescence Starrfield is requesting 1 summer month in 2013 to work full time on studies of the outburst of T Pyx. He will assist in the data analysis and the preparation of the observation paper on the HST data on T Pyx. He will continue his modeling of the outburst of T Pyx using MESA (Paxton, B., et al. 2011, ApJS, 192, 3) and continuing his studies of accretion of hydrogen rich material onto white dwarfs (Starrfield, S., et al. 2012, Baltic Astronomy, 21, 76). In his 2012 study he used his own code, NOVA, but is now switching to MESA because it includes the latest nuclear reaction rate libraries, pulsation, diffusion, and rotation and NOVA does not. One of the problems that he proposes to investigate is why mixing of core material with accreted material occurs in Classical Novae and not in Recurrent Novae. He makes this last statement because Classical Novae show that large amounts of white dwarf core material have been mixed up into the accreted material while abundance studies of Recurrent Novae ejecta (RS Oph, U Sco, T Pyx) suggest that little, if any, mixing has occurred in these systems. Of necessity, he will evolve a broad range in white dwarf mass, white dwarf luminosity, and composition of the accreting material.
|Effective start/end date||1/1/13 → 12/31/15|
- National Aeronautics Space Administration (NASA): $25,540.00
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