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2018
This chapter introduces the basics of radiative transfer, which is a primary energy-transport mechanism inside stars, and also contributes to keeping stars ‘inflated’ and balanced against gravity. The roles of opacity and cross-sections in scattering photons are described.
Paul A. Taylor, Prasenjit Saha
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This chapter introduces the basics of radiative transfer, which is a primary energy-transport mechanism inside stars, and also contributes to keeping stars ‘inflated’ and balanced against gravity. The roles of opacity and cross-sections in scattering photons are described.
Paul A. Taylor, Prasenjit Saha
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Pre-Main-Sequence Outflows [PDF]
Astrophysics and Space Science, 1995 In the 3 decades since winds from young stars were discovered, there have been many observations of bipolar molecular flows and ionized jets, and it has been recognized that outflows are intimately linked to star formation. Despite many observational clues and theoretical ideas, we still do not have a fully coherent picture of the outflow process.
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Evolution on the Main Sequence
2012Stars spend most of their lifes in the phase of central hydrogen burning. In observations of groups or populations of stars the corresponding location in the Hertzsprung-Russell diagram is therefore the most dominant feature and consequently has been termed Main Sequence.
Rudolf Kippenhahn +2 more
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2012
The simplicity and the importance of the results obtained for the main sequence suggest the extension of this concept to stars of quite different composition. We can then describe a main sequence as any sequence of homogeneous models with various masses M in complete equilibrium, consisting (mainly) of a certain element which burns in the central ...
Rudolf Kippenhahn +2 more
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The simplicity and the importance of the results obtained for the main sequence suggest the extension of this concept to stars of quite different composition. We can then describe a main sequence as any sequence of homogeneous models with various masses M in complete equilibrium, consisting (mainly) of a certain element which burns in the central ...
Rudolf Kippenhahn +2 more
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2014
We have so far covered topics that describe how a star forms, how the mass of stars can be determined by observing binary-star systems, and how long it takes to become a star. Now we shall discuss how long a star will remain on the main sequence and then look at what happens due to changes in its internal structure.
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We have so far covered topics that describe how a star forms, how the mass of stars can be determined by observing binary-star systems, and how long it takes to become a star. Now we shall discuss how long a star will remain on the main sequence and then look at what happens due to changes in its internal structure.
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Pre-Main-Sequence Binary Stars [PDF]
Annual Review of Astronomy and Astrophysics, 1994 The observational study of pre-main-sequence (PMS) binary stars is in many ways a very young field; most PMS binaries known today were discovered in the past decade. Nonetheless, T Tauri stars have been under study for more than a half century, and the serendipitous discovery of visual pairs has always been a by-product of their observation (e.g. Joy &
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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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