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

Journal Article · Mon May 01 04:00:00 EDT 1989 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/167452· OSTI ID:5643911

Kutter, G S; Sparks, W M ^[1]

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1. NASA, Goddard Space Flight Center, Greenbelt, MD (USA)

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. 58 refs.

• OSTI ID: 5643911
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 340; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ANGULAR MOMENTUM
BINARY STARS
DWARF STARS
ERUPTIVE VARIABLE STARS
MAGNETIC FIELDS
MASS
MASS TRANSFER
MATHEMATICAL MODELS
MIXING
NOVAE
NUCLEAR REACTIONS
STAR ACCRETION
STAR BURNING
STAR EVOLUTION
STAR MODELS
STARS
VARIABLE STARS
WHITE DWARF STARS