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Solar activity and differential rotation

Published online by Cambridge University Press:  26 August 2011

Hari Om Vats  and
Satish Chandra
Hari Om Vats
Affiliation:
Physical Research Laboratory, Navrangpura, Ahmedabad, Gujarat, India email: [email protected]
Satish Chandra
Affiliation:
Department of Physics, PPN College, Parade, Kanpur, UP, India email: [email protected]
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Abstract

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The coronal sidereal rotation rate as a function of latitude for each year, extending from 1992 to 2001 for soft X-ray images and from 1998 - 2005 for radio images are obtained. The present analysis reveals that the equatorial rotation rate of the corona is comparable to the photosphere and the chromosphere, However, at the higher latitudes, the corona rotation quite differently than the photosphere and chromosphere. The latitude differential obtained by both radio and X-ray images is quite variable throughout the period of the study. The equatorial rotation period seems to vary almost systematically with sunspot numbers which indicates its dependence on the phases of the solar activity cycle.

Keywords

Sun: corona – Sun: rotation – Sun: radio radiation – Sun: X-raysgamma rays
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 298 - 302
Copyright
Copyright © International Astronomical Union 2011

References

Antia, H. M. & Basu, S. 2001, Astrophys. J., 559, L67CrossRefGoogle Scholar
Aschwanden, M. J. & Benz, A. O. 1995, Astrophys. J., 438, 997CrossRefGoogle Scholar
Basu, S. & Antia, H. M. 2000, Solar Phys., 192, 469CrossRefGoogle Scholar
Balthasar, H., Vázquez, M., & Wöhl, H. 1986, Astron. Astrophys., 155, 87Google Scholar
Beck, J. G. 2000, Solar Phys., 191, 47CrossRefGoogle Scholar
Casas, R., Vaquero, J. M., & Vazquez, M. 2006, Solar Phys., 234, 379CrossRefGoogle Scholar
Chandra, S., Vats, H. O., & Iyer, K. N. 2009, Mon. Not. Roy. Astron. Soc. Letters, 400, L34CrossRefGoogle Scholar
Chandra, S., Vats, H. O., & Iyer, K. N. 2009, Mon. Not. Roy. Astron. Soc., 407, 1108CrossRefGoogle Scholar
Howard, R. F. 1996, ARAA, 34, 75CrossRefGoogle Scholar
Howe, R. 2009, Living Rev. Solar Phys., 6, 1CrossRefGoogle Scholar
Ribes, J. C. & Nesme-Ribes, E. 1993, Astron. Astrophys, 276, 549Google Scholar
Vats, H. O., Deshpande, M. R., Mehta, M., Shah, C. R., & Shah, K. J. 1998a, Earth, Moon & Planets, 76, 141CrossRefGoogle Scholar
Vats, H. O., Deshpande, M. R., Shah, C. R., & Mehta, M. 1998b, Solar Phys., 118, 351CrossRefGoogle Scholar
Vats, H. O., Cecatto, J. R., Mehta, M., Sawant, H. S., & Neri, J. A. C. F. 2001, Astrophys. J., 548, L87CrossRefGoogle Scholar