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Observations of a Post-Eruptive Arcade on October 22, 2001 with CORONAS-F, other Spaceborne Telescopes, and in Microwaves

Published online by Cambridge University Press:  03 June 2005

V.N. Borovik ,
V.V. Grechnev ,
O.I. Bugaenko ,
S.A. Bogachev ,
I.Y. Grigorieva ,
S.V. Kuzin ,
S.V. Lesovoi ,
M.A. Livshits ,
A.A. Pertsov  and
G.V. Rudenko
...Show all authors
V.N. Borovik
Affiliation:
Main Astronomical Observatory, St. Petersburg, Russia, email: [email protected]
V.V. Grechnev
Affiliation:
Institute of Solar-Terrestrial Physics, Irkutsk, Russia
O.I. Bugaenko
Affiliation:
Sternberg Astronomical Institute, Moscow, Russia
S.A. Bogachev
Affiliation:
Sternberg Astronomical Institute, Moscow, Russia
I.Y. Grigorieva
Affiliation:
Main Astronomical Observatory, St. Petersburg, Russia, email: [email protected]
S.V. Kuzin
Affiliation:
P.N.Lebedev Physical Institute, Moscow, Russia
S.V. Lesovoi
Affiliation:
Institute of Solar-Terrestrial Physics, Irkutsk, Russia
M.A. Livshits
Affiliation:
Institute of Terrestrial Magnetism, Aeronomy and Radiowave Propagation, Troitsk, Russia
A.A. Pertsov
Affiliation:
P.N.Lebedev Physical Institute, Moscow, Russia
G.V. Rudenko
Affiliation:
Institute of Solar-Terrestrial Physics, Irkutsk, Russia
V.A. Slemzin
Affiliation:
P.N.Lebedev Physical Institute, Moscow, Russia
A.I. Stepanov
Affiliation:
Institute of Terrestrial Magnetism, Aeronomy and Radiowave Propagation, Troitsk, Russia
K. Shibasaki
Affiliation:
Nobeyama Radio Observatory, Japan
A.M. Uralov
Affiliation:
Institute of Solar-Terrestrial Physics, Irkutsk, Russia
V.G. Zandanov
Affiliation:
Institute of Solar-Terrestrial Physics, Irkutsk, Russia
I.A. Zhitnik
Affiliation:
P.N.Lebedev Physical Institute, Moscow, Russia
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Abstract

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Using multi-spectral data, we estimate plasma parameters in the post-eruptive arcade observed on October 22, 2001 at 100 Mm above the limb: the temperature is 6 MK and the plasma density is $(5-9) \cdot 10^9$ cm$^{-3}$. We state a problem of the long-term equilibrium of the hot top of the arcade high in the corona: either the magnetic field surrounding the arcade well exceeds that one extrapolated in the potential approximation, or $\beta > 1$ both inside and outside the arcade. A downflow observed in soft X-rays can contribute to the equilibrium.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

Sun: activitycoronal mass ejectionsUV radiation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS226 , September 2004 , pp. 108 - 109
Copyright
© 2005 International Astronomical Union