Difference between revisions of "Main Sequence Star"

Revision as of 11:24, 19 July 2019

This is an image of The Sun which is a main sequence star.

A main sequence star is a star in which the nuclear fusion of Hydrogen isotopes produces Helium.

The main sequence stage of a star's life is the longest and most stable stage.

The inward pressure on the matter of the star, due to gravity, is balanced by the outward pressure on the matter of the star due to nuclear fusion of Hydrogen heating the matter so the star remains at a constant size.

During this stage mass is converted to energy due to the Mass-Energy Equivalence by the fusion of Hydrogen isotopes.

@@ Line 7: / Line 7: @@
 : The '''main sequence''' stage of a [[star]]'s life is the longest and most stable stage.
 : The inward [[pressure]] on the [[matter]] of the [[star]], due to [[gravity]], is balanced by the outward pressure on the [[matter]] of the [[star]] due to [[Nuclear Fusion|nuclear fusion]] of [[Hydrogen]] [[heating]] the [[matter]] so the [[star]] remains at a constant size.
-: During this stage [[Rest Mass Energy|rest mass]] is converted to [[energy]] by the [[Nuclear Fusion|fusion]] of [[Hydrogen]] [[isotopes]].
+: During this stage [[mass]] is converted to [[energy]] due to the [[Mass-Energy Equivalence]] by the [[Nuclear Fusion|fusion]] of [[Hydrogen]] [[isotopes]].
 : [[Energy]] from the [[Nuclear Potential Energy Store|nuclear potential energy store]] is [[Energy Transfer|transferred]] to the [[Thermal Energy Store|thermal energy store]] of the [[star]].