Results 301 to 310 of about 3,957,653 (321)
Some of the next articles are maybe not open access.
1990
We consider here a sequence of chemically homogeneous models in complete (mechanical and thermal) equilibrium with central hydrogen burning. All of them are composed of the same hydrogen-rich mixture, while the stellar mass M varies from model to model along the sequence.
Alfred Weigert, Rudolf Kippenhahn
openaire +2 more sources
We consider here a sequence of chemically homogeneous models in complete (mechanical and thermal) equilibrium with central hydrogen burning. All of them are composed of the same hydrogen-rich mixture, while the stellar mass M varies from model to model along the sequence.
Alfred Weigert, Rudolf Kippenhahn
openaire +2 more sources
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
openaire +1 more source
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
openaire +1 more source
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.
openaire +1 more source
Main sequence stars as calibrators for interferometry [PDF]
SPIE Proceedings, 2004 We present in this paper new and accurate calibrations of the surface brightness-color relations that can be used to predict accurately the angular diameter of dwarf stars and subgiants. These stars present significant advantages as calibrators for interferometric observations.
Kervella, Pierre +3 more
openaire +2 more sources
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.
openaire +2 more sources
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.
openaire +2 more sources
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
openaire +2 more sources
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
openaire +2 more sources
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
openaire +2 more sources
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 &
openaire +2 more sources
Signature of main sequence internal structure in post-main sequence stars
2009Post Main Sequence (post MS) stars keep a trace of their past main sequence history. Typically, the presence or not of an Intermediate Convective Zone (ICZ) above the H-burning shell of massive stars critically depends on the details of the Main Sequence (MS) phase modeling (convection criterion, mass loss,~...).
Dupret, Marc-Antoine +3 more
openaire +1 more source
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.
openaire +2 more sources
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.
openaire +2 more sources