2020ApJ...902...91H -
Astrophys. J., 902, 91-91 (2020/October-3)
A theory for the maximum magnitude versus rate of decline relation of classical novae.
HACHISU I., SAIO H., KATO M., HENZE M. and SHAFTER A.W.
Abstract (from CDS):
We propose a theory for the maximum magnitude versus rate of decline (MMRD) relation of novae using free-free emission model light curves built on the optically thick wind theory. We calculated (t3,MV,{max}) for various sets of ({dot}Macc,MWD), where MV,{max} is the peak absolute V magnitude, t3 is the 3 mag decay time from the peak, and {dot}Macc is the mass accretion rate onto the white dwarf (WD) of mass MWD. The model light curves are uniquely characterized by x≡Menv/Msc, where Menv is the hydrogen-rich envelope mass and Msc is the scaling mass at which the wind has a certain wind mass-loss rate. For a given ignition mass Mig, we can specify the first point x0=Mig/Msc on the model light curve and calculate the corresponding peak brightness and t3 time from this first point. Our (t3,MV,{max}) points cover well the distribution of existing novae. The lower the mass accretion rate, the brighter the peak. The maximum brightness is limited to MV,{max}≳-10.4 by the lowest mass accretion rate of {dot}Macc≳1×10–11M☉ yr–1. A significant part of the observational MMRD trend corresponds to the {dot}Macc∼5×10–9M☉ yr–1 line with different WD masses. A scatter from the trend line indicates a variation in their mass accretion rates. Thus, the global trend of an MMRD relation does exist, but its scatter is too large for it to be a precision distance indicator of individual novae.
Abstract Copyright:
© 2020. The American Astronomical Society. All rights reserved.
Journal keyword(s):
Cataclysmic variable stars - Classical novae - White dwarf stars - Distance indicators - Stellar winds
Simbad objects:
14
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