Hostname: page-component-586b7cd67f-rdxmf Total loading time: 0 Render date: 2024-11-25T17:55:06.054Z Has data issue: false hasContentIssue false
  • English
  • Français

Mass and Energy Supply of Fine Structure to the Solar Corona

Published online by Cambridge University Press:  26 May 2016

Kostas Tziotziou  and
Georgia Tsiropoula
Kostas Tziotziou
Affiliation:
Sterrekunding Instituut Utrecht, Postbus 80000, 3508 TA Utrecht, The Netherlands
Georgia Tsiropoula
Affiliation:
National Observatory of Athens, Institute for Space Applications and Remote Sensing, Lofos Koufos, 15236 Palea Penteli, Greece

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.

We investigate the role of chromospheric fine structures, e.g. mottles (spicules), in the mass balance and heating of the solar atmosphere by studying two-dimensional high-resolution Hα observations. The temporal and spatial variations of the line-of-sight (LOS) velocity, obtained with an inversion technique based on a cloud model, provide strong indications that the mechanism responsible for the driving of the observed flows is magnetic reconnection. Apart from the LOS velocity, application of the cloud model enables the derivation of several other physical parameters, like pressure, temperature, density etc. Mean values of these parameters permit the estimation of the role of these structures in the mass balance of the solar atmosphere. They, furthermore, permit a reasonable estimate of the energy provided by magnetic reconnection which is available for the heating of the solar corona.

Type
Part 3: The Sun as a Prototype and Laboratory for Stellar Physics
Information
Symposium - International Astronomical Union , Volume 219: Stars as Suns : Activity, Evolution and Planets , 2004 , pp. 123 - 127
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Beckers, J.M. 1964, A study of the fine structures in the solar chromosphere, Ph.D. Thesis, Utrecht.Google Scholar
Beckers, J.M. 1972, ARA&A, 10, 73.Google Scholar
Nagai, F. 1980, Solar Phys. 68, 351.CrossRefGoogle Scholar
Pneumann, G.W., & Kopp, R.A. 1978, Solar Phys., 57, 49.Google Scholar
Schrijver, C.J., Title, A.M., Van Ballegooijen, A.A., Hagenaar, H.J., & Shine, R.A. 1997, ApJ, 487, 424.CrossRefGoogle Scholar
Tsiropoula, G., & Schmieder, B. 1997, A&A, 324, 1183 (Paper I).Google Scholar
Tziotziou, K., Tsiropoula, G., & Mein, P. 2003, A&A, 402, 361 (Paper II).Google Scholar
Ulmschneider, P. 1971, A&A, 12, 297.Google Scholar
Wang, H., Tang, F., Zirin, H., & Wang, J. 1996, Solar Phys., 165, 223.Google Scholar
Withbroe, G.L. 1983, ApJ, 267, 825.CrossRefGoogle Scholar
Withbroe, G. L., & Noyes, R. W. 1977, ARA&A, 15, 363.Google Scholar