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Title: ON THE DIFFERENTIAL ROTATION OF MASSIVE MAIN-SEQUENCE STARS

To date, asteroseismology has provided core-to-surface differential rotation measurements in eight main-sequence stars. These stars, ranging in mass from ∼1.5–9 M{sub ⊙}, show rotation profiles ranging from uniform to counter-rotation. Although they have a variety of masses, these stars all have convective cores and overlying radiative regions, conducive to angular momentum transport by internal gravity waves (IGWs). Using two-dimensional numerical simulations, we show that angular momentum transport by IGWs can explain all of these rotation profiles. We further predict that, should high mass, faster rotating stars be observed, the core-to-envelope differential rotation will be positive, but less than one.
Authors:
 [1] ;  [2]
  1. Department of Mathematics and Statistics, Newcastle University (United Kingdom)
  2. (United States)
Publication Date:
OSTI Identifier:
22518648
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal Letters; Journal Volume: 815; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ANGULAR MOMENTUM; COMPUTERIZED SIMULATION; GRAVITY WAVES; MAIN SEQUENCE STARS; MASS; ROTATION; SURFACES; TWO-DIMENSIONAL CALCULATIONS