Journal
ASTROPHYSICAL JOURNAL
Volume 761, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/761/2/182
Keywords
binaries: symbiotic; circumstellar matter; novae, cataclysmic variables; shock waves; supernovae: general
Categories
Funding
- National Science Foundation [PHY 11-25915, AST 11-09174]
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1109174] Funding Source: National Science Foundation
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We present models of spherically symmetric recurrent nova shells interacting with circumstellar material (CSM) in a symbiotic system composed of a red giant (RG) expelling a wind and a white dwarf accreting from this material. Recurrent nova eruptions periodically eject material at high velocities (greater than or similar to 10(3) km s(-1)) into the RG wind profile, creating a decelerating shock wave as CSM is swept up. High CSM densities cause the shocked wind and ejecta to have very short cooling times of days to weeks. Thus, the late-time evolution of the shell is determined by momentum conservation instead of energy conservation. We compute and show evolutionary tracks of shell deceleration, as well as post-shock structure. After sweeping up all the RG wind, the shell coasts at a velocity similar to 100 km s(-1), depending on system parameters. These velocities are similar to those measured in blueshifted CSM from the symbiotic nova RS Oph, as well as a few Type Ia supernovae that show evidence of CSM, such as 2006X, 2007le, and PTF 11kx. Supernovae occurring in such systems may not show CSM interaction until the inner nova shell gets hit by the supernova ejecta, days to months after the explosion.
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