Astronomers employ complex models of magnetic interaction between a star and its accretion disk during a star’s early formation in order to explain why stars rotate so slowly. \u00a0 Subquantum kinetics avoids this issue entirely since generally, most new matter is formed from within the core of the star, thereby not imparting any angular momentum to the star.<\/p>\n
http:\/\/www.physorg.com\/news\/2011-06-stars.html<\/a><\/p>\n ————-<\/p>\n Yes, gmagee makes a good point here. \u00a0According to the continuous matter creation cosmology of subquantum kinetics, a main sequence star grows in size primarily through internal matter creation. \u00a0Consequently, it is able to ascend the main sequence without increasing its rate of rotation. \u00a0If they grew entirely by matter accretion, as conventional theory maintains, the large amount of acquired angular momentum that they acquired would cause them to spin so fast as to fly apart. \u00a0Thus, to counter this tendency,\u00a0standard theory is forced to postulate magnetic braking effects arising from the interaction of the star’s magnetic field with its surrounding dust disk. \u00a0But a study of one open cluster has shown that 30% of the stars in the cluster have inner disc radii beyond the reach of their magnetic field, hence no means of braking their rotation. \u00a0The stellar evolution theory of \u00a0subquantum kinetics offers a much simpler explanation.<\/p>\n P. LaViolette<\/p>\n","protected":false},"excerpt":{"rendered":" Astronomers employ complex models of magnetic interaction between a star and its accretion disk during a star’s early formation in order to explain why stars rotate so slowly. \u00a0 Subquantum kinetics avoids this issue entirely since generally, most new matter is formed from within the core of the star, thereby \u2026 Continue reading