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Solar Physics

, Volume 291, Issue 5, pp 1323–1340 | Cite as

Seismic Holography of the Solar Interior near the Maximum and Minimum of Solar Activity

  • M. Díaz Alfaro
  • F. Pérez Hernández
  • I. González Hernández
  • T. Hartlep
Article
  • 150 Downloads

Abstract

The base of the convection zone and the tachocline play a major role in the study of the dynamics of the Sun, especially in the solar dynamo. Here, we present a phase-sensitive helioseismic holography method to infer changes in the sound-speed profile of the solar interior. We test the technique using numerically simulated data by Zhao et al. (Astrophys. J. 702, 1150, 2009) with sound-speed perturbations at \(0.7 R_{\odot }\). The technique adequately recovers the perturbed sound-speed profile and is seen to be capable of detecting changes in the sound speed as low as 0.05 %. We apply the method to two GONG solar time series of approximately one year, each comprising 13 Bartels rotations, BR2295–BR2307 and BR2387–BR2399, near the maximum and at a minimum of solar activity, respectively. We successfully recover a sound-speed variation with respect to a standard solar model, consistent with previous results. However, we fail to recover a realistic sound-speed variation between maximum and minimum.

Keywords

Helioseismology Solar activity Tachocline 

Notes

Acknowledgements

We thank C. Lindsey and D. Braun for making available a large part of the far-side code used here and adapted for use with foci well below the surface. Part of this research was supported by the Spanish National Research Plan under project AYA2010-17803. This work uses data obtained by the Global Oscillation Network Group (GONG) program, managed by the National Solar Observatory, which is operated by AURA, Inc. under a cooperative agreement with the National Science Foundation. The data were acquired by instruments operated by the Big Bear Solar Observatory, High Altitude Observatory, Learmonth Solar Observatory, Udaipur Solar Observatory, Instituto de Astrofísica de Canarias, and Cerro Tololo Interamerican Observatory. We thankfully acknowledge the technical expertise and assistance provided by the Spanish Supercomputing Network (Red Española de Supercomputación), as well as the computer resources used: the LaPalma Supercomputer, located at the Instituto de Astrofísica de Canarias, as well as the contribution of Teide High-Performance Computing facilities to the results of this research. TeideHPC facilities are provided by the Instituto Tecnológico y de Energías Renovables (ITER, SA). URL: http://teidehpc.iter.es .

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Copyright information

© Springer Science+Business Media Dordrecht 2016

Authors and Affiliations

  1. 1.Instituto de Astrofísica de CanariasLa Laguna, TenerifeSpain
  2. 2.Departamento de AstrofísicaUniversidad de La LagunaLa Laguna, TenerifeSpain
  3. 3.National Solar ObservatoryTucsonUSA
  4. 4.Bay Area Environmental Research InstituteNASA Ames Research CenterMoffett FieldUSA

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