Standing shocks in the inner slow solar wind

Details Standing shocks in the inner slow solar wind Standing shocks in the inner slow solar wind

2011-03-27

arxiv.org/abs/1103.5209v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

4 pages, 3 figures, accepted by Chinese Physics Letters, volume 28, number 5, id 059601

Scientific paper

The slow solar wind, or at least a significant part of it, originates from the region bordering streamer helmets, where the flow tube geometry is distinct from flow tubes rooted in the center of coronal holes. We examine whether this particular tube geometry leads to standing shocks in the inner slow wind in this region. To isolate the influence of tube geometry, a simple isothermal wind model is employed and is solved in terms of the Lambert W function. In addition to a continuous solution, the model may also admit solutions with shocks, readily constructed with a graphical approach. When allowed, the shock solutions appear in pairs, one with a shock located in the streamer stalk, the other with a shock below the cusp along the streamer border. We show that solutions with standing shocks exist in a broad area in the parameter space characterizing the wind temperature and flow tube. In particular, streamers with cusps located at a heliocentric distance $\gtrsim 3.2 R_\odot$ can readily support discontinuous slow winds with temperatures barely higher than 1 MK.

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