Abstract
Supernovae: Little Bear's mass loss rate
Highlights
! how do they do it? Astronomers have de- clude that only stars in excess of 18 M(')
Three recent cont- 18 - 40 M0 stars need never go through a ributions', seem to have resolved at least WR phase at all. This permits a reasonable one facet of this problem, The current range of intermediate mass stars to retain consensus is that Tpe 1 their extended, hydrogen-rich supergiant events arise in relatively old, low-mass envelopes and make Type II light curves stars and derive energy from explosive and spectra
Broad-peaked spectrum shows N III and He II emission light curves cannot be reproduced by the lines superimposed on a strong blue conmodels"·, And lies the main dis- tinuum, suggesting a progenitor whose crepancy with the present majority view surface composition resembled that of a that all or most single and wide binary OB WR star
Summary
! how do they do it? Astronomers have de- clude that only stars in excess of 18 M('). This permits a reasonable one facet of this problem, The current range of intermediate mass stars to retain consensus is that Tpe 1 (hydrogen free) their extended, hydrogen-rich supergiant events arise in relatively old, low-mass envelopes and make Type II light curves stars and derive energy from explosive and spectra.
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