Hostname: page-component-78c5997874-fbnjt Total loading time: 0 Render date: 2024-11-19T11:41:48.539Z Has data issue: false hasContentIssue false
  • English
  • Français

Comparison of numerical simulations and observations of helioseismic MHD waves in sunspots

Published online by Cambridge University Press:  26 August 2011

K. V. Parchevsky ,
J. Zhao ,
A. G. Kosovichev  and
M. Rempel
K. V. Parchevsky
Affiliation:
Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA email: [email protected]
J. Zhao
Affiliation:
Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA email: [email protected]
A. G. Kosovichev
Affiliation:
Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA email: [email protected]
M. Rempel
Affiliation:
HAO/NCAR, Boulder, CO 80307, USA email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Numerical 3D simulations of MHD waves in magnetized regions with background flows are very important for the understanding of propagation and transformation of waves in sunspots. Such simulations provide artificial data for testing and calibration of helioseismic techniques used for analysis of data from space missions SOHO/MDI, SDO/HMI, and HINODE. We compare with helioseismic observations results of numerical simulations of MHD waves in different models of sunspots. The simulations of waves excited by a localized source provide a detailed picture of the interaction of the MHD waves with the magnetic field and background flows (deformation of the waveform, wave transformation, amplitude variations and anisotropy). The observed cross-covariance function represents an effective Green's function of helioseismic waves. As an initial step, we compare it with simulations of waves generated by a localized source. More thorough analysis implies using multiple sources and comparison of the observed and simulated cross-covariance functions. We plan to do such calculations in the nearest future. Both, the simulations and observations show that the wavefront inside the sunspot travels ahead of a reference “quiet Sun” wavefront, when the wave enters the sunspot. However, when the wave passes the sunspot, the time lag between the wavefronts becomes unnoticeable.

Keywords

HelioseismologyMHDsunspots
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 422 - 425
Copyright
Copyright © International Astronomical Union 2011

References

Khomenko, E. & Collados, M. 2008, Astrophys. J., 689, 1379CrossRefGoogle Scholar
Low, B. C. 1975, Astrophys. J., 197, 251CrossRefGoogle Scholar
Parchevsky, K. V. & Kosovichev, A. G. 2007, Astrophys. J., 666, 547Google Scholar
Parchevsky, K. V. & Kosovichev, A. G. 2009, Astrophys. J., 694, 573Google Scholar
Parchevsky, K. V., Kosovichev, A. G., Khomenko, E., Olshevsky, V., & Collados, M. 2010, arXiv:1002.1117v1Google Scholar
Pizzo, V. J. 1986, Astrophys. J., 302, 785CrossRefGoogle Scholar
Rempel, M., Schüssler, M., Cameron, R. H., & Knölker, M. 2009, Science, 325, 171Google Scholar
Tam, C. & Webb, J. 1993, J. Comput. Phys. 107, 262Google Scholar