Physics
Scientific paper
Mar 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985natur.314..337a&link_type=abstract
Nature (ISSN 0028-0836), vol. 314, March 28, 1985, p. 337, 338.
Physics
119
Carbon Stars, Gravitational Collapse, Hubble Constant, Stellar Models, Supernovae, White Dwarf Stars, Binary Stars, Chandrasekhar Equation, Nickel Isotopes, Oxygen, Stellar Evolution, Stellar Luminosity, Stellar Mass Accretion
Scientific paper
The immediate progenitor of a Type I supernova (SN I) is thought to be a mass-accreting carbon-oxygen (C-O) white dwarf in a binary system. In the supernova explosion the C-O fuel is partly incinerated to radioactive 56Ni. The optical luminosity results from the trapping and thermalization of the γ rays and positrons emitted by the decay of 56Ni through 56Co to 56Fe. The authors estimate the amount of 56Ni synthesized and the corresponding peak luminosity of a SN I from the model. This estimate is combined with the observed Hubble diagram of SN I to derive the value of the Hubble constant H0. It is found that H0 is in the range 39 - 73 km s-1Mpc-1 with a best estimate of 59 km s-1Mpc-1.
Arnett David. W.
Branch David
Wheeler Justin C.
No associations
LandOfFree
Hubble's constant and exploding carbon-oxygen white dwarf models for Type I supernovae does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Hubble's constant and exploding carbon-oxygen white dwarf models for Type I supernovae, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Hubble's constant and exploding carbon-oxygen white dwarf models for Type I supernovae will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-825964