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Title: SOLAR WAVE-FIELD SIMULATION FOR TESTING PROSPECTS OF HELIOSEISMIC MEASUREMENTS OF DEEP MERIDIONAL FLOWS

Abstract

The meridional flow in the Sun is an axisymmetric flow that is generally directed poleward at the surface, and is presumed to be of fundamental importance in the generation and transport of magnetic fields. Its true shape and strength, however, are debated. We present a numerical simulation of helioseismic wave propagation in the whole solar interior in the presence of a prescribed, stationary, single-cell, deep meridional circulation serving as synthetic data for helioseismic measurement techniques. A deep-focusing time-distance helioseismology technique is applied to the synthetic data, showing that it can in fact be used to measure the effects of the meridional flow very deep in the solar convection zone. It is shown that the ray approximation that is commonly used for interpretation of helioseismology measurements remains a reasonable approximation even for very long distances between 12 Degree-Sign and 42 Degree-Sign corresponding to depths between 52 and 195 Mm. From the measurement noise, we extrapolate that time-resolved observations on the order of a full solar cycle may be needed to probe the flow all the way to the base of the convection zone.

Authors:
; ;  [1];  [2]
  1. W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA (United States)
  2. NASA Ames Research Center, Moffett Field, CA (United States)
Publication Date:
OSTI Identifier:
22167252
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 762; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; APPROXIMATIONS; ASTRONOMY; ASTROPHYSICS; AXIAL SYMMETRY; COMPUTERIZED SIMULATION; CONVECTION; DISTANCE; FOCUSING; MAGNETIC FIELDS; NOISE; OSCILLATIONS; SOLAR CYCLE; SUN; SURFACES; TIME RESOLUTION

Citation Formats

Hartlep, T., Zhao, J., Kosovichev, A. G., and Mansour, N. N. SOLAR WAVE-FIELD SIMULATION FOR TESTING PROSPECTS OF HELIOSEISMIC MEASUREMENTS OF DEEP MERIDIONAL FLOWS. United States: N. p., 2013. Web. doi:10.1088/0004-637X/762/2/132.
Hartlep, T., Zhao, J., Kosovichev, A. G., & Mansour, N. N. SOLAR WAVE-FIELD SIMULATION FOR TESTING PROSPECTS OF HELIOSEISMIC MEASUREMENTS OF DEEP MERIDIONAL FLOWS. United States. https://doi.org/10.1088/0004-637X/762/2/132
Hartlep, T., Zhao, J., Kosovichev, A. G., and Mansour, N. N. 2013. "SOLAR WAVE-FIELD SIMULATION FOR TESTING PROSPECTS OF HELIOSEISMIC MEASUREMENTS OF DEEP MERIDIONAL FLOWS". United States. https://doi.org/10.1088/0004-637X/762/2/132.
@article{osti_22167252,
title = {SOLAR WAVE-FIELD SIMULATION FOR TESTING PROSPECTS OF HELIOSEISMIC MEASUREMENTS OF DEEP MERIDIONAL FLOWS},
author = {Hartlep, T. and Zhao, J. and Kosovichev, A. G. and Mansour, N. N.},
abstractNote = {The meridional flow in the Sun is an axisymmetric flow that is generally directed poleward at the surface, and is presumed to be of fundamental importance in the generation and transport of magnetic fields. Its true shape and strength, however, are debated. We present a numerical simulation of helioseismic wave propagation in the whole solar interior in the presence of a prescribed, stationary, single-cell, deep meridional circulation serving as synthetic data for helioseismic measurement techniques. A deep-focusing time-distance helioseismology technique is applied to the synthetic data, showing that it can in fact be used to measure the effects of the meridional flow very deep in the solar convection zone. It is shown that the ray approximation that is commonly used for interpretation of helioseismology measurements remains a reasonable approximation even for very long distances between 12 Degree-Sign and 42 Degree-Sign corresponding to depths between 52 and 195 Mm. From the measurement noise, we extrapolate that time-resolved observations on the order of a full solar cycle may be needed to probe the flow all the way to the base of the convection zone.},
doi = {10.1088/0004-637X/762/2/132},
url = {https://www.osti.gov/biblio/22167252}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 762,
place = {United States},
year = {Thu Jan 10 00:00:00 EST 2013},
month = {Thu Jan 10 00:00:00 EST 2013}
}