Pre-main-sequence Stellar Structure
Pre-Main-Sequence Stellar Structure is a theoretical astrophysical model that describes the internal physical and dynamical configuration of a young stellar object during its gravitational contraction phase prior to the onset of sustained hydrogen fusion, distinguishing it from main-sequence stellar structures by its non-equilibrium thermodynamic state and accretion-driven evolution.
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10K
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331
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213
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2017–2026
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138
Star Formation in the Orion Nebula Cluster
F. Palla, Steven W. Stahler · The Astrophysical Journal · 1999 · 570 citations
Natural Sciences, Astronomy, Physics +17
The <i>Y</i> <sup>2</sup> Isochrones for α‐Element Enhanced Mixtures
Yong‐Cheol Kim, P. Demarque, Sukyoung K. Yi et al. · The Astrophysical Journal Supplement Series · 2002 · 380 citations · Full text
Natural Sciences, Astronomy, Physics +15
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Centre National de la Recherche Scientifique
Paris, France
15 h-index
36 publications
3K citations
Arcetri Astrophysical Observatory
Florence, Italy
7 h-index
11 publications
1.8K citations
California Institute of Technology
Pasadena, United States
5 h-index
15 publications
994 citations

Observatoire de Paris
Paris, France
5 h-index
13 publications
368 citations
Center for Astrophysics Harvard & Smithsonian
Cambridge, United States
5 h-index
7 publications
329 citations

University of Amsterdam
Amsterdam, The Netherlands
4 h-index
15 publications
438 citations
KU Leuven
Leuven, Belgium
4 h-index
8 publications
344 citations
United States Naval Observatory
Flagstaff, United States
4 h-index
5 publications
190 citations
1–8 of 213
ApJ · 42 publications · 4.3K citations
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24 publications · 1.8K citations
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20 publications · 878 citations
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AJ · 6 publications · 198 citations
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Repository · 4 publications · 164 citations
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