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

Authors

326

  1. LH
    Lee Hartmann

    Center for Astrophysics Harvard & Smithsonian, United States

    4 publications · 321 citations

    4

    h-index

  2. ES
    Elena Sabbi

    Space Telescope Science Institute, United States

    3 publications · 126 citations

    3

    h-index

  3. NC
    Nuria Calvet

    University of Michigan, United States

    3 publications · 296 citations

    3

    h-index

  4. JR
    J. R. Stauffer

    California Institute of Technology, United States

    3 publications · 96 citations

    3

    h-index

  5. JS
    J. S. Gallagher

    University of Wisconsin–Madison, United States

    3 publications · 123 citations

    3

    h-index

1–5 of 326

Venues

  1. The Astrophysical Journal

    ApJ · 42 publications · 2.4K citations

    28

    h-index

  2. The Astronomical Journal

    AJ · 17 publications · 610 citations

    14

    h-index

  3. Astronomy and Astrophysics

    11 publications · 426 citations

    11

    h-index

  4. 9

    h-index

  5. Publications of the Astronomical Society of the Pacific

    PASP · 5 publications · 129 citations

    5

    h-index

1–5