Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...190...72m&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 190, no. 1-2, Jan. 1988, p. 72-78.
Astronomy and Astrophysics
Astrophysics
43
Accretion Disks, Astronomical Models, Dwarf Novae, Ultraviolet Radiation, Gas Ionization, Helium, Hydrogen, Stellar Temperature
Scientific paper
The present disk-instability model calculation of an accretion disk's time evolution gives attention to the outer region's behavior at the onset of type A outbursts, and discovers that the outer cool region does not jump directly to the T(eff) greater-than-10,000 K state, but rather halts at an intermediate nonequilibrium state whose T(eff) is of the order of 6000 K. This is due to the increased thermal time-scale and opacity in the H and He ionization zone; the heating front continues inward to form an extended warm region, radiating in the optical wavelength range, that is presently designated the 'stagnation stage' of dwarf-nova outbursts. The warm region is eventually heated to the hot equilibrium state, whereupon it begins to radiate significant UV flux.
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