In this paper, a solution of the problem about how a massive star knows that it gets rid of its excess of mass before it can become a white dwarf, a pulsar or a black hole, is proposed. Many astronomers believe that this may take place in the form of a nova and supernova outburst, as well as in the form of a continuous outflow of gas [1].
References
[1]
Struve, O. (1963) The Universe. The M.I.T. Press, Massachusetts Institute of Technology, Cambridge.
[2]
Abell, G. (1964) Exploration of the Universe. Holt, Rinehart and Winston.
[3]
Eddington, A.S. (1988) The Internal Constitution of the Stars. Cambridge University Press, New Rochelle, New York, Melbourne. http://dx.doi.org/10.1017/CBO9780511600005
[4]
Fierros Palacios, A. (2006) The Hamilton-Type Principle in Fluid Dynamics. Fundamentals and Applications to Magnetohydrodynamics, Thermodynamics, and Astrophysics. Springer-Verlag, Wien..
[5]
Fierros Palacios, A. (2015) The Magnetic Field in the Stability of the Stars. To Be Publishing.
[6]
Fierros Palacios, A. (2015) The Problem of the Existence of Planetary Systems Similar to the Solar System. To Be Publishing.
