Solar structure and evolution. (arXiv:2007.06488v2 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Christensen_Dalsgaard_J/0/1/0/all/0/1">Joergen Christensen-Dalsgaard</a>
The Sun provides a critical benchmark for the general study of stellar
structure and evolution. Also, knowledge about the internal properties of the
Sun is important for the understanding of solar atmospheric phenomena,
including the solar magnetic cycle. Here I provide a brief overview of the
theory of stellar structure and evolution, including the physical processes and
parameters that are involved. This is followed by a discussion of solar
evolution, extending from the birth to the latest stages. As a background for
the interpretation of observations related to the solar interior I provide a
rather extensive analysis of the sensitivity of solar models to the assumptions
underlying their calculation. I then discuss the detailed information about the
solar interior that has become available through helioseismic investigations
and the detection of solar neutrinos, with further constraints provided by the
observed abundances of the lightest elements. Revisions in the determination of
the solar surface abundances have led to increased discrepancies, discussed in
some detail, between the observational inferences and solar models. I finally
briefly address the relation of the Sun to other similar stars and the
prospects for asteroseismic investigations of stellar structure and evolution.
The Sun provides a critical benchmark for the general study of stellar
structure and evolution. Also, knowledge about the internal properties of the
Sun is important for the understanding of solar atmospheric phenomena,
including the solar magnetic cycle. Here I provide a brief overview of the
theory of stellar structure and evolution, including the physical processes and
parameters that are involved. This is followed by a discussion of solar
evolution, extending from the birth to the latest stages. As a background for
the interpretation of observations related to the solar interior I provide a
rather extensive analysis of the sensitivity of solar models to the assumptions
underlying their calculation. I then discuss the detailed information about the
solar interior that has become available through helioseismic investigations
and the detection of solar neutrinos, with further constraints provided by the
observed abundances of the lightest elements. Revisions in the determination of
the solar surface abundances have led to increased discrepancies, discussed in
some detail, between the observational inferences and solar models. I finally
briefly address the relation of the Sun to other similar stars and the
prospects for asteroseismic investigations of stellar structure and evolution.
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