2-D and 3-D models of convective turbulence and oscillations in intermediate-mass main-sequence stars

Joyce A. Guzik, T. H. Morgan, N. J. Nelson, C. Lovekin, K. Kosak, I. N. Kitiashvili, N. N. Mansour, A. Kosovichev

Research output: Contribution to journalArticlepeer-review


We present multidimensional modeling of convection and oscillations in main-sequence stars somewhat more massive than the Sun, using three separate approaches: 1) Using the 3-D planar StellarBox radiation hydrodynamics code to model the envelope convection zone and part of the radiative zone. Our goals are to examine the interaction of stellar pulsations with turbulent convection in the envelope, excitation of acoustic modes, and the role of convective overshooting; 2) Applying the spherical 3-D MHD ASH (Anelastic Spherical Harmonics) code to simulate the core convection and radiative zone. Our goal is to determine whether core convection can excite low-frequency gravity modes, and thereby explain the presence of low frequencies for some hybrid γ Dor/δ Sct variables for which the envelope convection zone is too shallow for the convective blocking mechanism to drive gravity modes; 3) Applying the ROTORC 2-D stellar evolution and dynamics code to calculate evolution with a variety of initial rotation rates and extents of core convective overshooting. The nonradial adiabatic pulsation frequencies of these nonspherical models are calculated using the 2-D pulsation code NRO. We present new insights into pulsations of 1-2 M⊙ stars gained by multidimensional modeling.

Original languageEnglish (US)
Pages (from-to)540-543
Number of pages4
JournalProceedings of the International Astronomical Union
Issue numberA29B
StatePublished - 2015

All Science Journal Classification (ASJC) codes

  • Medicine (miscellaneous)
  • Astronomy and Astrophysics
  • Nutrition and Dietetics
  • Public Health, Environmental and Occupational Health
  • Space and Planetary Science


  • Kepler spacecraft
  • stars: convection
  • stars: oscillations
  • stars: rotation


Dive into the research topics of '2-D and 3-D models of convective turbulence and oscillations in intermediate-mass main-sequence stars'. Together they form a unique fingerprint.

Cite this