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

Published online by Cambridge University Press:  27 October 2016

Joyce A. Guzik ,
T. H. Morgan ,
N. J. Nelson ,
C. Lovekin ,
K. Kosak ,
I. N. Kitiashvili ,
N. N. Mansour  and
A. Kosovichev
Joyce A. Guzik
Affiliation:
Los Alamos National Laboratory, Los Alamos, NMUSA87545 email: [email protected]
T. H. Morgan
Affiliation:
Los Alamos National Laboratory, Los Alamos, NMUSA87545 email: [email protected] Brigham Young University, Provo, UT 84602USA
N. J. Nelson
Affiliation:
Los Alamos National Laboratory, Los Alamos, NMUSA87545 email: [email protected]
C. Lovekin
Affiliation:
Mount Allison University, Sackville, NB E4L 1H3Canada
K. Kosak
Affiliation:
Florida Institute of Technology, Melbourne, FL 32901USA
I. N. Kitiashvili
Affiliation:
NASA Ames Research Center, Mountain View, CA 94035USA
N. N. Mansour
Affiliation:
NASA Ames Research Center, Mountain View, CA 94035USA
A. Kosovichev
Affiliation:
Physics Department, New Jersey Institute of Technology, Newark, NJ 07103USA
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Abstract

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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.

Keywords

stars: convectionstars: oscillationsstars: rotationKepler spacecraft
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B: Astronomy in Focus , August 2015 , pp. 540 - 543
Copyright
Copyright © International Astronomical Union 2016 

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