The effects of He-3 on nova outbursts - A possible recurrent nova trigger

Details The effects of He-3 on nova outbursts - A possible recurrent nova trigger The effects of He-3 on nova outbursts - A possible recurrent nova trigger

Jul 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...239..581s&link_type=abstract

Astrophysical Journal, Part 1, vol. 239, July 15, 1980, p. 581-585.

Astronomy and Astrophysics

Astrophysics

13

Binary Stars, Helium Isotopes, Novae, Red Giant Stars, White Dwarf Stars, Abundance, Nuclear Fusion, Stellar Envelopes, Stellar Models

Scientific paper

Observations and theory strongly imply that recurrent novae are massive white dwarf (having a mass not less than 1.25 solar mass) red giant binaries. If this is the case, it is argued that hydrogen-rich material transferred from the red giant to the white dwarf should be quite rich in He-3 (Y3 not less than 0.001). This should be sufficient to heat a degenerate hydrogen-rich envelope on a white dwarf by Delta T of 10 million K on a time scale of years, thus triggering a thermonuclear runaway. Numerical simulations of two models, identical except for their envelope He-3 abundances, confirm these estimates. A low-mass, He-3 deficient (Y3 equals 0) envelope produces no instability, while the Y3 equals 0.002 model produces a nova outburst at t equals 26 years after the start of the simulation.

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