Hostname: page-component-8448b6f56d-c4f8m Total loading time: 0 Render date: 2024-04-23T11:43:36.037Z Has data issue: false hasContentIssue false

Transition Region Blinkers

Published online by Cambridge University Press:  13 May 2016

C. E. Parnell
Affiliation:
School of Mathematical and Computational Sciences, University of St Andrews, North Haugh, St Andrews, Fife, KY16 9SS, SCOTLAND
D. Bewsher
Affiliation:
School of Mathematical and Computational Sciences, University of St Andrews, North Haugh, St Andrews, Fife, KY16 9SS, SCOTLAND
R. A. Harrison
Affiliation:
School of Mathematical and Computational Sciences, University of St Andrews, North Haugh, St Andrews, Fife, KY16 9SS, SCOTLAND Rutherford Appleton Laboratory, Chilton, Didcot, Oxon, OX11 0QX, ENGLAND
A. W. Hood
Affiliation:
School of Mathematical and Computational Sciences, University of St Andrews, North Haugh, St Andrews, Fife, KY16 9SS, SCOTLAND

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.

To allow an objective study of transition region blinkers an automated identification program has been developed to analyse the CDS/SoHO data. The general properties of blinkers identified by this method confirmed the properties of those identified by eye in previous studies. Blinkers have typical lifetimes of about 20 minutes, areas of about 2.8 × 107 km2 and intensity enhancement factors of about 2. For the first time, blinkers have been identified in active regions. These blinkers have the same general properties as quiet-region blinkers. The automated approach found many more blinkers than previously had been found giving a global birth rates of about 9 s−1 for quiet-region blinkers and 16 s−1 for active-region blinkers. Most blinkers, active or quiet region, are red shifted with typical velocities of about 13 km s−1. Finally, we can confirm that blinkers are not enhancements in temperature, but either enhancements in density or increases in the filling factor.

Type
Session IV: Structure and Dynamics of the Transiton Region and Corona
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

Berghmans, D., Clette, F. and Moses, D. 1998, A&A, 336, 10391055.Google Scholar
Harrison, R.A. 1997, Solar Physics, 175, 467485.Google Scholar
Harrison, R.A., Lang, J., Brooks, D.H. and Innes, D.E. 1999, A&A, 351, 11151132.Google Scholar