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Signature of main sequence internal structure in post-main sequence stars
2009International ...
Dupret, Marc-Antoine +3 more
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2012
Numerical solutions to the equations of stellar structure can provide detailed description of the interiors of stars. Some general features of stellar structure can be discovered through these solutions. The mass distribution indicates that for high-mass stars with M ≥ 1. 2 M⊙ over 95 % of the mass is contained within ∼ 60 % of the radius.
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Numerical solutions to the equations of stellar structure can provide detailed description of the interiors of stars. Some general features of stellar structure can be discovered through these solutions. The mass distribution indicates that for high-mass stars with M ≥ 1. 2 M⊙ over 95 % of the mass is contained within ∼ 60 % of the radius.
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2002
The matter in the Universe (its barionic component) is concentrated mainly in stars. Inside galaxies, stars contain more than 90% of the matter, and in galactic clusters, due to the existence of intercluster gas, stars contain more than 70% of the matter. The presence of heavy elements (heavier than carbon) in the intercluster gas, with an abundance of
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The matter in the Universe (its barionic component) is concentrated mainly in stars. Inside galaxies, stars contain more than 90% of the matter, and in galactic clusters, due to the existence of intercluster gas, stars contain more than 70% of the matter. The presence of heavy elements (heavier than carbon) in the intercluster gas, with an abundance of
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2003
Most of the stars that we observe in the night sky have all got one thing in common — they are on the main sequence. There are, of course, exceptions: Betelgeuse has left the main sequence and has become a red giant star, the hydrogen burning at the centre of its core has stopped, and now helium is burning by fusion processes; while Sirius B has ...
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Most of the stars that we observe in the night sky have all got one thing in common — they are on the main sequence. There are, of course, exceptions: Betelgeuse has left the main sequence and has become a red giant star, the hydrogen burning at the centre of its core has stopped, and now helium is burning by fusion processes; while Sirius B has ...
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Symposium - International Astronomical Union, 1978
About 3/4 of the sky were searched spectroscopically for stars whose ultraviolet spectra (3640–4100 Å) match that of the Sun, at 20 Å resolution. Down to the limit of the BSC, only two were found: HR 7504 and HR 2290. No G2 V star matches the Sun. Stars that do match have (B-V) = 0m.66. The search has a bearing on effective temperatures of G dwarfs and
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About 3/4 of the sky were searched spectroscopically for stars whose ultraviolet spectra (3640–4100 Å) match that of the Sun, at 20 Å resolution. Down to the limit of the BSC, only two were found: HR 7504 and HR 2290. No G2 V star matches the Sun. Stars that do match have (B-V) = 0m.66. The search has a bearing on effective temperatures of G dwarfs and
openaire +2 more sources
2011
The time for the completion of protostellar evolution is effectively 2–3 times the free-fall time of the outer layers, which lies in the range 105–106 yr, depending on the initial density. As the accretion rate tapers off in the later phases and the infalling envelope becomes less and less opaque, the observable surface of the protostar declines in ...
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The time for the completion of protostellar evolution is effectively 2–3 times the free-fall time of the outer layers, which lies in the range 105–106 yr, depending on the initial density. As the accretion rate tapers off in the later phases and the infalling envelope becomes less and less opaque, the observable surface of the protostar declines in ...
openaire +2 more sources