Pre-main-sequence Stellar Evolution

Pre-Main-Sequence Stellar Evolution is a theoretical construct in astrophysics denoting the phase of stellar development from gravitational collapse of a molecular cloud core to the onset of stable hydrogen fusion on the main sequence, distinguished by energy generation primarily through gravitational contraction and accretion rather than core nuclear fusion.

417

Publications

40.2K

Citations

1K

Authors

455

Institutions

Publications per year

2017–2026

67

Authors

1K

  1. SW
    Steven W. Stahler

    University of California, Berkeley, United States

    9 publications · 1.9K citations

    9

    h-index

  2. BT
    B. T. Gänsicke

    University of Warwick, United Kingdom

    8 publications · 746 citations

    8

    h-index

  3. FP
    F. Palla

    Arcetri Astrophysical Observatory, Italy

    8 publications · 1.4K citations

    8

    h-index

  4. GM
    G. Meynet

    University of Geneva, Switzerland

    8 publications · 523 citations

    8

    h-index

  5. AM
    A. Maeder

    Global Social Observatory, Switzerland

    7 publications · 419 citations

    7

    h-index

1–5 of 1K

Venues

  1. The Astrophysical Journal

    ApJ · 130 publications · 17.3K citations

    60

    h-index

  2. Astronomy and Astrophysics

    70 publications · 5.2K citations

    40

    h-index

  3. Monthly Notices of the Royal Astronomical Society

    57 publications · 4.6K citations

    30

    h-index

  4. The Astronomical Journal

    AJ · 28 publications · 1.3K citations

    20

    h-index

  5. The Astrophysical Journal Supplement Series

    14 publications · 4.4K citations

    14

    h-index

1–5