ON the DIFFERENTIAL ROTATION of MASSIVE MAIN-SEQUENCE STARS

Research output: Contribution to journalArticlepeer-review

50 Scopus citations

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.

Original languageEnglish (US)
Article numberL30
JournalAstrophysical Journal Letters
Volume815
Issue number2
DOIs
StatePublished - Dec 20 2015

Keywords

  • asteroseismology
  • stars: rotation
  • waves

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Fingerprint

Dive into the research topics of 'ON the DIFFERENTIAL ROTATION of MASSIVE MAIN-SEQUENCE STARS'. Together they form a unique fingerprint.

Cite this