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What determines the penumbral size and Evershed flow speed?

Published online by Cambridge University Press:  26 August 2011

Na Deng ,
Toshifumi Shimizu ,
Debi Prasad Choudhary  and
Haimin Wang
Na Deng
Affiliation:
Physics and Astronomy Department, California State University Northridge, 18111 Nordhoff St., Northridge, CA 91330, United States email: na.deng@csun.edu Space Weather Research Laboratory, New Jersey Institute of Technology, 323 Martin Luther King Blvd., Newark, NJ 07102, United States
Toshifumi Shimizu
Affiliation:
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
Debi Prasad Choudhary
Affiliation:
Physics and Astronomy Department, California State University Northridge, 18111 Nordhoff St., Northridge, CA 91330, United States email: na.deng@csun.edu
Haimin Wang
Affiliation:
Space Weather Research Laboratory, New Jersey Institute of Technology, 323 Martin Luther King Blvd., Newark, NJ 07102, United States
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Abstract

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Using Hinode SP and G-band observations, we examined the relationship between magnetic field structure and penumbral length as well as Evershed flow speed. The latter two are positively correlated with magnetic inclination angle or horizontal field strength within 1.5 kilogauss, which is in agreement with recent magnetoconvective simulations of Evershed effect. This work thus provides direct observational evidence supporting the magnetoconvection nature of penumbral structure and Evershed flow in the presence of strong and inclined magnetic field.

Keywords

SunspotsSun: magnetic fieldsSun: atmospheric motionsSun: photosphere
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 216 - 220
Copyright
Copyright © International Astronomical Union 2011

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