Interchange Reconnection and Coronal Hole Dynamics

Details Interchange Reconnection and Coronal Hole Dynamics Interchange Reconnection and Coronal Hole Dynamics

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010apj...714..517e&link_type=abstract

The Astrophysical Journal, Volume 714, Issue 1, pp. 517-531 (2010).

Astronomy and Astrophysics

Astronomy

13

Sun: Activity, Sun: Corona, Sun: Magnetic Topology, Solar Wind

Scientific paper

We investigate the effect of magnetic reconnection between open and closed fields, often referred to as "interchange" reconnection, on the dynamics and topology of coronal hole boundaries. The most important and most prevalent three-dimensional topology of the interchange process is that of a small-scale bipolar magnetic field interacting with a large-scale background field. We determine the evolution of such a magnetic topology by numerical solution of the fully three-dimensional MHD equations in spherical coordinates. First, we calculate the evolution of a small-scale bipole that initially is completely inside an open field region and then is driven across a coronal hole boundary by photospheric motions. Next the reverse situation is calculated in which the bipole is initially inside the closed region and driven toward the coronal hole boundary. In both cases, we find that the stress imparted by the photospheric motions results in deformation of the separatrix surface between the closed field of the bipole and the background field, leading to rapid current sheet formation and to efficient reconnection. When the bipole is inside the open field region, the reconnection is of the interchange type in that it exchanges open and closed fields. We examine, in detail, the topology of the field as the bipole moves across the coronal hole boundary and find that the field remains well connected throughout this process. Our results, therefore, provide essential support for the quasi-steady models of the open field, because in these models the open and closed flux are assumed to remain topologically distinct as the photosphere evolves. Our results also support the uniqueness hypothesis for open field regions as postulated by Antiochos et al. On the other hand, the results argue against models in which open flux is assumed to diffusively penetrate deeply inside the closed field region under a helmet streamer. We discuss the implications of this work for coronal observations.

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