Role of field line topology and anomalous viscosity and resistivity in the mechanism leading to the formation of the slow solar wind

Details Role of field line topology and anomalous viscosity and resistivity in the mechanism leading to the formation of the slow solar wind Role of field line topology and anomalous viscosity and resistivity in the mechanism leading to the formation of the slow solar wind

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh21a0275r&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH21A-0275

Physics

7509 Corona

Scientific paper

The observation by the Large Angle and Spectrometric Coronagraph (LASCO) instrument on the Solar and Heliospheric Observatory of blobs of plasma generated near the cusp region of the streamer belt has sparked the hope of gaining new insight into the genesis of the slow solar wind. The observations suggest that open and closed field lines reconnect near the cusp of the helmet streamer to form blobs of higher density plasmas that are ejected into the slow solar wind. Models of this process have been suggested, and simulation studies have been conducted. We take the recent simulation work of Einaudi et al.[1] as our starting point to investigate the formation of the slow solar wind and of the blobs observed by LASCO. We report two main conclusions. First, we consider the role of resistivity and viscosity in the evolution time-scale. Second, by employing more realistic two- dimensional configurations including the cusp and bent field lines with fast solar wind flow [2], we find that reconnection giving rise to plasma blobs is driven by converging flows with reconnection rates largely insensitive to changes in resistivity. [1] Einaudi et al, ApJ, 547, 1167 (2001) [2] Lapenta and Knoll, 624,1049 (2005)

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