A theoretical explanation of the absolute magnitude-decline time /M[SUB]B-t[/SUB] sub 3/ relationship for classical novae

Abstract

view Abstract Citations (95) References (33) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS A theoretical explanation of the absolute magnitude-decline time /MB-t sub 3/ relationship for classical novae Shara, M. M. Abstract An analytic explanation is proposed for the observed strong correlation between the absolute photographic magnitude of a nova at maximum and the time it takes to dim from maximum by 3 magnitudes. The observational basis of the magnitude-decay time and associated ejection velocity-decay time relations is reviewed, and the steady-state, constant luminosity, continuous ejection model of classical novae is summarized. The maximum magnitude-decay time relation for novae is then derived from considerations of the classical model, the assumption of nova shut-off from envelope exhaustion, and the conditions necessary for the appearance of a thermonuclear runaway on the white dwarf surface. The relation is shown to be in good agreement with observations, with faster novae occurring on more massive white dwarfs. The correlation between ejection velocity and decay time is also reproduced, being a direct consequence of the equipartition of the energy flux of the radiation field and the ejected matter. Scatter in the observational relation is attributed to scatter in the prenova white dwarf luminosity, and it is predicted that the absolute magnitude at maximum-decay time relation should be the same for all galaxies, populations and epochs where binaries form. Publication: The Astrophysical Journal Pub Date: February 1981 DOI: 10.1086/158657 Bibcode: 1981ApJ...243..926S Keywords: Novae; Stellar Magnitude; Stellar Models; White Dwarf Stars; Approximation; Mathematical Models; Stellar Mass Ejection; Stellar Temperature; Astrophysics full text sources ADS | data products NED (3)