Constructing and Characterising Solar Structure Models for Computational Helioseismology
Abstract
In local helioseismology, numerical simulations of wave propagation are useful to model the interaction of solar waves with perturbations to a background solar model. However, the solution to the linearised equations of motion include convective modes that can swamp the helioseismic waves that we are interested in. In this article, we construct background solar models that are stable against convection, by modifying the vertical pressure gradient of Model S (ChristensenDalsgaard et al., 1996, Science 272, 1286) relinquishing hydrostatic equilibrium. However, the stabilisation affects the eigenmodes that we wish to remain as close to Model S as possible. In a bid to recover the Model S eigenmodes, we choose to make additional corrections to the sound speed of Model S before stabilisation. No stabilised model can be perfectly solarlike, so we present three stabilised models with slightly different eigenmodes. The models are appropriate to study the f and p _{1} to p _{4} modes with spherical harmonic degrees in the range from 400 to 900. Background model CSM has a modified pressure gradient for stabilisation and has eigenfrequencies within 2% of Model S. Model CSM_A has an additional 10% increase in sound speed in the top 1 Mm resulting in eigenfrequencies within 2% of Model S and eigenfunctions that are, in comparison with CSM, closest to those of Model S. Model CSM_B has a 3% decrease in sound speed in the top 5 Mm resulting in eigenfrequencies within 1% of Model S and eigenfunctions that are only marginally adversely affected. These models are useful to study the interaction of solar waves with embedded threedimensional heterogeneities, such as convective flows and model sunspots. We have also calculated the response of the stabilised models to excitation by random nearsurface sources, using simulations of the propagation of linear waves. We find that the simulated power spectra of wave motion are in good agreement with an observed SOHO/MDI power spectrum. Overall, our convectively stabilised background models provide a good basis for quantitative numerical local helioseismology. The models are available for download from http://www.mps.mpg.de/projects/seismo/NA4/.
 Publication:

Solar Physics
 Pub Date:
 July 2011
 DOI:
 10.1007/s112070119790x
 arXiv:
 arXiv:1105.0219
 Bibcode:
 2011SoPh..271....1S
 Keywords:

 Solar models;
 Helioseismology;
 Numerical methods;
 Astrophysics  Solar and Stellar Astrophysics
 EPrint:
 35 pages, 23 figures Changed title Updated Figure 18