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Louise Harra   Submitted: 2008-03-26 02:00

The formation of the slow solar wind has been debated for many years. In this paper we show evidence of persistent outflow at the edges of an active region as measured by the EUV Imaging Spectrometer onboard Hinode. The Doppler velocity ranged between 20-50 km s-1 and was consistent with a steady flow seen in the X-ray Telescope. The latter showed steady, pulsing outflowing material and some transverse motions of the loops. We analyse the magnetic field around the active region and produce a coronal magnetic field model. We determine from the latter that the outflow speeds adjusted for line-of-sight effects can reach over 100 km s-1. We can interpret this outflow as expansion of loops that lie over the active region, which may either reconnect with neighbouring large-scale loops or are likely to open to the interplanetary space. This material constitutes at least part of the slow solar wind.

Authors: Harra, Sakao, Mandrini,Hara, Imada, Young, van Driel-Gesztelyi, Baker
Projects: Hinode/EIS

Publication Status: ApJ Letters, 676, L147, 2008
Last Modified: 2008-09-23 21:12
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