Abstract
The Sun is a large sphere of luminous plasma — that is, ionized matter. High densities in its interior are produced by the gravitational pull of its central mass on the surrounding solar matter. A high interior temperature and the consequent thermonuclear reactions keep the entire solar matter ionized. The high central density (about 1.5 X 102 gcm-3) and temperature (about 1.5 · 107K) define its central pressure (about 3 · 1017 dyne cm−2), which prevents the Sun from collapsing.
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© 1986 D. Reidel Publishing Company, Dordrecht, Holland
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Huebner, W.F. (1986). Atomic and Radiative Processes in the Solar Interior. In: Sturrock, P.A., Holzer, T.E., Mihalas, D.M., Ulrich, R.K. (eds) Physics of the Sun. Geophysics and Astrophysics Monographs, vol 24. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-5253-9_3
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DOI: https://doi.org/10.1007/978-94-009-5253-9_3
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