Author： Fisk L.A. Zurbuchen T.H. Schwadron N.A.
Publisher： Springer Publishing Company
ISSN： 0038-6308
Source： Space Science Reviews, Vol.87, Iss.1, 1999-01, pp. : 43-54
Disclaimer: Any content in publications that violate the sovereignty, the constitution or regulations of the PRC is not accepted or approved by CNPIEC.
Abstract
Coronal hole boundaries are the interfaces between regions where the coronal magnetic field contains a significant component which is open into the heliosphere and regions where the field is primarily closed. It is pointed out that there are constraints on the magnetic field which opens into the heliosphere that must be satisfied in the corona: it must come into pressure equilibrium in the high corona, and the component of the field which connects to the polar regions of the Sun must differentially rotate. A model is presented in which satisfying these constraints determines which field lines are open and which are closed, and thus where the polar coronal hole boundaries occur. Some of the consequences of this model are discussed.
Related content
Access to resources
Recommend
Comparing Quiet Sun and Coronal Hole Regions with CDS/SOHO
Space Science Reviews, Vol. 87, Iss. 1, 1999-01 ,pp. :
Brightness distribution at the base of a coronal hole
By Teplitskaya R. Ozhogina O. Turova I.
Astronomy Letters, Vol. 32, Iss. 2, 2006-02 ,pp. :