SH13B-4097:
A COMPUTATIONAL MODEL TO APROACH THE STUDY OF P MODES ON ACTIVE REGIONS IN THE SUN
Monday, 15 December 2014
Carlos Andrés Galarza1, Benjamin Calvo-Mozo1 and Juan Carlos Martinez Oliveros2, (1)National University of Colombia, Bogotá, Colombia, (2)Space Sciences Laboratory, Berkeley, CA, United States
Abstract:
In the last decades the internal structure of the Sun has been studied by analyzing the properties of propagating waves in the solar interior and it observational signatures in the photosphere. In fact, helioseismology has become in one of the best and powerful tools we have to study the Sun's interior. Actually, we already know that there are three different kind of oscillation modes: acoustic (due to pressure), internal gravity and surface gravity waves named as p, g and f modes respectively. The purpose of this work is to simulate an acoustic signal (focusing on p modes) that is being propagated through a 2D region of plasma immersed in a homogeneous and constant magnetic field based on the previous research made by Schunker and Cally (2006). This simulation will show how magnetic fields can affect the trajectory of the acoustic signal and therefore reproducing previous results but based on a different computational algorithm.
