How does the structure of a 0.2 solar mass star differ than the Sun?
Answers: Most stars are between 0.1 and 1 solar mass range. At the low closing you have stars similar to red dwarfs (see ref 3). In the 0.2 - 0.25 solar mass range the stars finish off more like red giant and less resembling helium-rich dwarf stars. Another feature of low mass stars is they convect almost adjectives their material and thus extension up fusing 98% of their hydrogen - unlike our Sun which ends up fusing only roughly speaking 8% of its hydrogen on the Main Sequence. See ref 1.
Quoting from the Wikipedia (ref 2):
Stars with vastly low mass
If the mass of a main-sequence star is lower than approximately half a solar mass, it will never become hot satisfactory to fuse helium at its core. It is thought that, over a lifespan exceeding the age (~13.7 billion years)[10] of the Universe, such a star will eventually burn all its hydrogen and winding up its evolution as a helium white dwarf composed chiefly of helium-4 nuclei. Owing to the time this process take, it is not thought to be the origin of observed helium white dwarfs. Rather, they are thought to be the product of mass loss contained by binary systems or mass loss due to a large planetary companion.
It is 0.2 times as big as our sun.
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Answers: Most stars are between 0.1 and 1 solar mass range. At the low closing you have stars similar to red dwarfs (see ref 3). In the 0.2 - 0.25 solar mass range the stars finish off more like red giant and less resembling helium-rich dwarf stars. Another feature of low mass stars is they convect almost adjectives their material and thus extension up fusing 98% of their hydrogen - unlike our Sun which ends up fusing only roughly speaking 8% of its hydrogen on the Main Sequence. See ref 1.
Quoting from the Wikipedia (ref 2):
Stars with vastly low mass
If the mass of a main-sequence star is lower than approximately half a solar mass, it will never become hot satisfactory to fuse helium at its core. It is thought that, over a lifespan exceeding the age (~13.7 billion years)[10] of the Universe, such a star will eventually burn all its hydrogen and winding up its evolution as a helium white dwarf composed chiefly of helium-4 nuclei. Owing to the time this process take, it is not thought to be the origin of observed helium white dwarfs. Rather, they are thought to be the product of mass loss contained by binary systems or mass loss due to a large planetary companion.
It is 0.2 times as big as our sun.
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