ON THE DIFFERENTIAL ROTATION OF MASSIVE MAIN-SEQUENCE STARS

ABSTRACT 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 , show rotation profiles ranging from uniform to counter-rotation. Although they have a variety of masses, these stars all have...

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Bibliographic Details
Published in:Astrophysical journal. Letters 2015-12, Vol.815 (2), p.1-5
Main Author: Rogers, T. M.
Format: Article
Language:English
Subjects:
ANGULAR MOMENTUM
asteroseismology
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Computer simulation
COMPUTERIZED SIMULATION
Differential rotation
GRAVITY WAVES
MAIN SEQUENCE STARS
MASS
ROTATION
Stars
stars: rotation
SURFACES
Transport
Two dimensional
TWO-DIMENSIONAL CALCULATIONS
waves
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Summary:ABSTRACT 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 , 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.
ISSN:2041-8205
2041-8213
2041-8213
DOI:10.1088/2041-8205/815/2/L30