Pre-main-sequence Structure
Pre-Main-Sequence Structure is a theoretical astrophysical model that describes the internal physical and thermal configuration of a forming star during the evolutionary phase preceding the onset of core hydrogen fusion, distinguishing it from main-sequence stellar structures by its non-equilibrium state and gravitational contraction-driven energy generation.
108
Publications
5.3K
Citations
326
Authors
170
Institutions
Publications per year
2017–2026
7
Parents
108
The Inner Regions of Protoplanetary Disks
Annual Review of Astronomy and Astrophysics · 2010 · 282 citations · Full text
Natural Sciences, Astronomy, Physics +15
Spiral Structure in the Circumstellar Disk around AB Aurigae
Misato Fukagawa, Masahiko Hayashi, Motohide Tamura et al. · The Astrophysical Journal · 2004 · 213 citations · Full text
Natural Sciences, Astronomy, Physics +14
1–5 of 108
326
Center for Astrophysics Harvard & Smithsonian, United States
4 publications · 321 citations
4
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3
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3
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3
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3
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1–5 of 326
170
Center for Astrophysics Harvard & Smithsonian
Cambridge, United States
7 h-index
17 publications
1.2K citations
California Institute of Technology
Pasadena, United States
7 h-index
16 publications
397 citations

Space Telescope Science Institute
Baltimore, United States
6 h-index
13 publications
539 citations
Max Planck Institute for Astronomy
Heidelberg, Germany
6 h-index
9 publications
660 citations
University of Michigan
Ann Arbor, United States
5 h-index
12 publications
670 citations

Centre National de la Recherche Scientifique
Paris, France
5 h-index
15 publications
846 citations
Max Planck Society
Munich, Germany
4 h-index
8 publications
453 citations
Osservatorio Astronomico di Palermo
Palermo, Italy
4 h-index
14 publications
736 citations
1–8 of 170
ApJ · 42 publications · 2.4K citations
28
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AJ · 17 publications · 610 citations
14
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11 publications · 426 citations
11
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9 publications · 337 citations
9
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PASP · 5 publications · 129 citations
5
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1–5