Pre-main Sequence Stars

Pre-Main Sequence Stars is a stellar astrophysical category denoting a young star in the evolutionary phase preceding its arrival on the main sequence, distinguished by its ongoing gravitational contraction and absence of sustained hydrogen fusion in the core.

1.4K

Publications

115.4K

Citations

3K

Authors

801

Institutions

Publications per year

2017–2026

198

Authors

3K

  1. FP
    F. Palla

    Arcetri Astrophysical Observatory, Italy

    22 publications · 2.5K citations

    18

    h-index

  2. LH
    Lee Hartmann

    Center for Astrophysics Harvard & Smithsonian, United States

    18 publications · 4.1K citations

    17

    h-index

  3. SW
    Steven W. Stahler

    University of California, Berkeley, United States

    17 publications · 2.7K citations

    16

    h-index

  4. GM
    G. Meynet

    University of Geneva, Switzerland

    16 publications · 2.8K citations

    16

    h-index

  5. RD
    R. D. Jeffries

    Keele University, United Kingdom

    14 publications · 859 citations

    14

    h-index

1–5 of 3K

Venues

  1. The Astrophysical Journal

    ApJ · 424 publications · 34.7K citations

    102

    h-index

  2. Astronomy and Astrophysics

    245 publications · 17.9K citations

    66

    h-index

  3. Monthly Notices of the Royal Astronomical Society

    222 publications · 11.3K citations

    59

    h-index

  4. The Astronomical Journal

    AJ · 124 publications · 8.7K citations

    52

    h-index

  5. The Astrophysical Journal Supplement Series

    30 publications · 9.7K citations

    28

    h-index

1–5