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.

138

Publications

10K

Citations

331

Authors

213

Institutions

Publications per year

2017–2026

25

Authors

331

  1. SW
    Steven W. Stahler

    University of California, Berkeley, United States

    4 publications · 761 citations

    4

    h-index

  2. FP
    F. Palla

    Arcetri Astrophysical Observatory, Italy

    4 publications · 754 citations

    4

    h-index

  3. MK
    Masanobu Kunitomo

    Kurume University, Japan

    3 publications · 122 citations

    3

    h-index

  4. SI
    Shigeru Ida

    Tokyo Institute of Technology, Japan

    3 publications · 122 citations

    3

    h-index

  5. LK
    L. Kaper

    University of Amsterdam, Netherlands

    3 publications · 90 citations

    3

    h-index

1–5 of 331

Venues

  1. The Astrophysical Journal

    ApJ · 42 publications · 4.3K citations

    30

    h-index

  2. Astronomy and Astrophysics

    24 publications · 1.8K citations

    19

    h-index

  3. 17

    h-index

  4. The Astronomical Journal

    AJ · 6 publications · 198 citations

    6

    h-index

  5. Springer Link (Chiba Institute of Technology)

    Repository · 4 publications · 164 citations

    4

    h-index

1–5