Restricted Three-Body Dynamics and Morphologies of Early Novae Shells and their Spectral Signatures

Details Restricted Three-Body Dynamics and Morphologies of Early Novae Shells and their Spectral Signatures Restricted Three-Body Dynamics and Morphologies of Early Novae Shells and their Spectral Signatures

Aug 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003dda....34.1207l&link_type=abstract

American Astronomical Society, DDA meeting #34, #12.07; Bulletin of the American Astronomical Society, Vol. 35, p.1048

Astronomy and Astrophysics

Astronomy

Scientific paper

The goal of this work is to calculate emission line profiles of classical novae systems for comparison to line profiles we observe in an attempt to deduce geometrical and dynamical properties of the system from the spectra. The material ejected by the thermonuclear runaway on the surface of the white dwarf (WD) is modeled as a large number of massless particles that are launched instantaneously and move ballistically thereafter. Each particle's position is propagated independently in three-dimensional space with a particle's track terminating if it impacts the WD or the secondary. Predicted line profiles, assuming an optically thin shell, are generated by computing a histogram of the number of particles in radial velocity space for a given observing projection. At high ejection velocities, a nearly spherical shell is produced. At ejection speeds near the WD's escape velocity, very complicated and ever changing geometries result and the material remains close to the system's barycenter. We present animations of computer simulations of novae shell development and the associated line profiles.
This work supported by The Aerospace Corporation's Independent Research and Development program and by the US Air Force Space and Missile Systems Center through the Mission Oriented Investigation and Experimentation program, under contract F4701-00-C-0009 with the US Air Force.

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