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SEARCHING FOR THE ORIGINS OF THE FAST SOLAR WIND M. D. POPESCU 1;2 and J. G. DOYLE 1
 

Summary: SEARCHING FOR THE ORIGINS OF THE FAST SOLAR WIND
M. D. POPESCU 1;2 and J. G. DOYLE 1
1 Armagh Observatory
College Hill, Armagh BT61 9DG, N. Ireland
2 Astronomical Institute of the Romanian Academy
RO-75212 Bucharest 28, Romania
Abstract. Here we present the lowest evidence, observed in the solar atmosphere, of the
fast solar wind streams. They originate from coronal holes (CH) network boundaries, as
seen in the low transition region (TR) line, O iii 703.87  A (Te  8  10 4 K). Higher in
the solar corona, the plasma out ow is seen in the Mg ix 706.02  A line (Te  10 6 K),
as an increased blue-shift inside the CH region. An interesting change in behaviour is
observed at the quiet Sun (QS)/CH boundaries, where plasma from the network changes
its velocity sign, and, following the closed magnetic structures, falls back to the Sun. This
is also the site where signature of magnetic reconnection between the open CH lines and
the closed QS loops is seen, in the form of an increased number of bi-directional jets,
which represent evidence for the slow solar wind origins.
1. Introduction
Today there is general agreement that the fast solar wind originates mainly
from magnetically open regions in the coronal holes (CHs) (Krieger et al.,
1973). In order to nd more precisely what are the small-scale features

  

Source: Armagh Observatory

 

Collections: Physics