Hostname: page-component-cd9895bd7-7cvxr Total loading time: 0 Render date: 2024-12-25T16:39:32.940Z Has data issue: false hasContentIssue false
  • English
  • Français

EUV and Microwave Observation of a Filament

Published online by Cambridge University Press:  12 April 2016

F. Chiuderi-Drago ,
K. Bocchialini ,
S. Lamartinie ,
J.-C. Vial ,
T. Bastian ,
C.E. Alissandrakis ,
R. Harrison ,
J.-P. Delaboudinière  and
P. Lemaire
F. Chiuderi-Drago
Affiliation:
DASOP-Observatoire de Paris-Meudon, 92195 Meudon Cedex, France
K. Bocchialini
Affiliation:
Institut d’Astrophysique Spatiale, Bât. 121, Université Paris XI-CNRS, 91405 Orsay Cedex, France
S. Lamartinie
Affiliation:
Institut d’Astrophysique Spatiale, Bât. 121, Université Paris XI-CNRS, 91405 Orsay Cedex, France
J.-C. Vial
Affiliation:
Institut d’Astrophysique Spatiale, Bât. 121, Université Paris XI-CNRS, 91405 Orsay Cedex, France
T. Bastian
Affiliation:
National Radio Astronomy Observatory, Soccoro, NM 87801, USA
C.E. Alissandrakis
Affiliation:
Section of Astro-Geophysics, Department of Physics, Universiy of Ioannina, 45110 Ioannina, Greece
R. Harrison
Affiliation:
Space Science Department, Rutherford Appleton Laboratory, Chilton, Didcot Oxfordshire OX11, OXX, UK
J.-P. Delaboudinière
Affiliation:
Institut d’Astrophysique Spatiale, Bât.121, Université Paris XI-CNRS, 91405 Orsay Cedex, France
P. Lemaire
Affiliation:
Institut d’Astrophysique Spatiale, Bât.121, Université Paris XI-CNRS, 91405 Orsay Cedex, France

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.

Simultaneous XUV and microwave (μ – ѡ) observations of a solar filament, performed by several instruments onboard SOHO and by the Very Large Array (VLA), are analyzed. The filament appears as a dark structure, very similar in shape to the optical Hα filament, in all images taken in the transition region (TR) lines observed by CDS, in the Ne VIII lines observed by SUMER at λ = 770Å and 780Å and at all radio wavelengths with 1.7 cm ≤ λ ≤ 6 cm. Contrary to that, in six TR lines observed by SUMER at λ > 1300Å no trace of the filament, either in absorption or in emission, is visible. Finally, at λ = 21 cm, as well as in all images taken in coronal lines by CDS and EIT, a dark feature is present at the filament position, although with less defined contours than in the first-mentioned TR images. The constraints imposed by all these observations are discussed and interpreted.

Type
Filaments and Their Environment
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 55 - 58
Copyright
Copyright © Astronomical Society of the Pacific 1998

References

Alissandrakis, C.E., Drago, F., Bastian, T., Bocchialini, K., Delaboudinière, J.-P., Lemaire, P., Vial, J.-C., Harrison, R.A., and Thompson, B. 1997, in Advances in the Physics of Sunspots,Schmieder, B., Toro del Iniesta, J.C. and Vazquez, M. (eds.), ASP Conf. Series, Vol. 118 Google Scholar
Chiuderi, C. and Chiuderi Drago, F. 1990, Solar Phys., 132, 81 CrossRefGoogle Scholar
Chiuderi Drago, F. 1990, in Dynamics of Quiescent Prominences, Ruzdjak, V. and Tandberg-Hanssen, E. (eds.), Springer-Verlag, New York, p. 70 CrossRefGoogle Scholar
Engvold, O. 1989, in Dynamics and Structure of Quiescent Solar Prominences, Priest, E.R. (ed.), Kluwer Acad. Publ., Dordecht, Holland, p. 47 Google Scholar
Engvold, O., Kjeldseth-Moe, O. Bartoe, J-D.F. and Brueckner, G.E. 1987, 21st ESLAB Symp. ESA SP-275, p. 21 Google Scholar
Leroy, J.L. 1989, in Dynamics and Structure of Quiescent Solar Prominences, Priest, E.R. (ed.), Kluwer Acad. Publ., Dordrecht, Holland, p. 77 Google Scholar
Schmahl, E.J. and Orrall, F.Q. 1986, in Coronal and Prominence Plasma, Poland, A. (ed.), NASA Conf. Pub. 2442, p. 127 Google Scholar