Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh52b..03h&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH52B-03
Astronomy and Astrophysics
Astrophysics
[7522] Solar Physics, Astrophysics, And Astronomy / Helioseismology, [7544] Solar Physics, Astrophysics, And Astronomy / Stellar Interiors And Dynamo Theory
Scientific paper
The meridional flow is of fundamental importance for understanding magnetic flux transport in the solar interior. Reliable measurements of the flow could provide important constraints for dynamo theories. The actual shape and strength of the meridional flow, particularly in the deep interior, remains unknown. Detecting such weak flows with a speed of 10-20 m/s in the deep solar interior is a challenging problem for helioseismology. Numerical simulations of helioseismic wave propagation provide means for testing and calibrating measurement techniques, and can help increase our confidence in the inferences obtained from helioseismic inversions. We have developed a 3D numerical spectral code to simulate the propagation of acoustic waves in the whole-Sun. With this code, we simulate the propagation of stochastic wave fields given mean meridional flows of different strength and circulation patterns (including flow models with deep and shallow stagnation points). Our helioseismic measurement techniques are based on estimating acoustic travel times from wave-field cross-correlations (time-distance helioseismology method). We investigate various cross-correlation schemes, and study the sensitivity of acoustic travel times to the depth and speed of the meridional flow. Using the numerical simulation results we discuss the prospects of measuring the Sun's meridional flow from Solar Dynamics Observatory (SDO/HMI) data.
Hartlep Thomas
Kosovichev Aleksandr G.
Mansour Nagi N.
Pipin Valery V.
Rempel Matthias
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