Abstract
Active sunspot group n° 4567 was observed with high angular magnification on Sept. 2, 1984, using the instrument FPSS at Meudon Observatory. Within the sunspots umbrae, the longitudinal magnetic field shows a collection of small elements down to the limit of resolution of around 600 km. Between the trailing and leading spots, there were very sharp gradients, both in magnetization (450 gauss over 1000 km) and in Doppler velocity (350 m s-1 over 1 000 km). The line defined by these gradients was the location of a flare. Evershed driving forces may be responsible for building up these gradients and flare.
This is a preview of subscription content, log in via an institution to check access.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
Preview
Unable to display preview. Download preview PDF.
References
Dollfus A., Colson F., Crussaire D. and Launay F. (1985). Ann. Astrophys. 151, 235-253.
Dollfus A., Crussaire D. Pernot E. and Lioure A. (1985). Ann. Astrophys. 151, 235-253.
Author information
Authors and Affiliations
Editor information
Editors and Affiliations
Rights and permissions
Copyright information
© 1990 International Astronomical Union
About this paper
Cite this paper
Dollfus, A. (1990). Small Scale Magnetic Structures in Active Centers. In: Stenflo, J.O. (eds) Solar Photosphere: Structure, Convection, and Magnetic Fields. International Astronomical Union, vol 138. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-1061-4_17
Download citation
DOI: https://doi.org/10.1007/978-94-009-1061-4_17
Publisher Name: Springer, Dordrecht
Print ISBN: 978-0-7923-0530-9
Online ISBN: 978-94-009-1061-4
eBook Packages: Springer Book Archive