The mass profile in the solar-mass stars

Details The mass profile in the solar-mass stars The mass profile in the solar-mass stars

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003nupha.722..465n&link_type=abstract

Nuclear Physics A, Volume 722, p. C465-C468.

Physics

Nuclear Physics

Scientific paper

It does seem clear that, the solar-mass stars are born from molecular clouds. We have no well-confirmed observation of a solar-mass protostar. However, the mass distribution in a star, mass of the core, and mass of the dark interstellar cloud from which the star was formed as well as the other characteristics related to the early stages of the star formation are predicted by the Energy Transfer Model. Two main assumed sources of energy for the solar-mass stars formation are originated from the gravitational pressure and thermonuclear reactions. The model was tested for the nearest us star, the Sun. The results are in good agreement with the Standard Solar Model.

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