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Manifestation of the Jupiter's synodic period in the solar wind, interplanetary magnetic field and geophysical parameters

Published online by Cambridge University Press:  26 February 2010

S. N. Samsonov  and
N. G. Skryabin
S. N. Samsonov
Affiliation:
Yu. G. Shafer Institute of Cosmophysical Research and Aeronomy, SB RAS, 677980, Yakutsk, Russia email: s_samsonov@ikfia.ysn.ru
N. G. Skryabin
Affiliation:
Yu. G. Shafer Institute of Cosmophysical Research and Aeronomy, SB RAS, 677980, Yakutsk, Russia email: s_samsonov@ikfia.ysn.ru
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Abstract

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Studying by the authors of paper of solar wind parameters, namely: density, speed and temperature and also a module of interplanetary magnetic field (IMF) intensity has allowed to find out in them fluctuations with the period of 399 days. From references it is known that this period coincidence with the synodic period of Jupiter. So long as close by the given period another source of such fluctuations is not known we have assumed that fluctuations with the period of 399 days are fluctuations with the synodic period of Jupiter. The change of the solar wind plasma parameters and IMF intensity can lead to the change of the Earth's magnetic field parameters and, as a consequence, to the change of charged particle fluxes in the Earth's magnetosphere. On this assumption the IMF intensity in the Earth's vicinity, geomagnetic disturbance (Kp-index) and riometer absorption for the years of 1986-1996 have been analyzed. The analysis of the data has shown the presence of certain changes of these physical parameters with the period of 399 days. When the Earth and Jupiter were found to be on the same magnetic field line, the IMF intensity was decreasing up to 3.0±0.57, the geomagnetic activity and riometer absorption were decreasing up to 5.2±1.46% and 9.4±2.63%, respectively.

Keywords

Sun: activitysolar windsolar system: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S264: Solar and Stellar Variability: Impact on Earth and Planets , August 2009 , pp. 452 - 454
Copyright
Copyright © International Astronomical Union 2010

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