Modeling the classical nova outburst. I - Exploring the physics of a new mechanism

Details Modeling the classical nova outburst. I - Exploring the physics of a new mechanism Modeling the classical nova outburst. I - Exploring the physics of a new mechanism

May 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...340..985k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 340, May 15, 1989, p. 985-1005.

Statistics

Computation

33

Binary Stars, Novae, Stellar Models, White Dwarf Stars, Angular Momentum, Computational Astrophysics, Nuclear Astrophysics, Stellar Envelopes, Stellar Magnetic Fields, Stellar Mass Accretion

Scientific paper

Model calculations were performed to describe a mechanism that produces classical nova outbursts on white dwarfs of 1 solar mass or less and for accretion rates of 4 x 10 to the -10th solar mass/yr or greater, i.e., the parameters corresponding to observed data of nova systems. Calculations point to four factors that can induce nuclear runaways of sufficient strength to eject about 0.0001 solar mass at speeds of several hundred to a few thousand km per second, as is observed in classical novae. These are (1) the effects of storage of angular momentum in the star's envelope during the accretion phase; (2) the reduction of centrifugal forces in the star's outer layers during the early nuclear runaway phase, through the inward transport of angular momentum; (3) the inward movement of the zone of peak nuclear burning through the convectively induced shear instability during the runaway phase; and (4) the mixing of original CO stellar matter and H-rich matter, also through the convectively induced shear instability.

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