|Number of pages||5|
|Journal||Monthly Notices of the Royal Astronomical Society Letters|
|Publication status||Published - 10 Jun 2013|
According to current models, solar closed-field active regions are isolated from contributing directly to the solar wind except through small- or large-scale magnetic reconnection, including coronal mass ejections. Here we show the first direct evidence of active regions contributing directly to the solar wind by a steady-state, quiescent expansion. Advanced image processing of coronagraph data reveals a large system of nested closed-field magnetic structures expanding and accelerating to heights of at least 14 R⊙ within a helmet streamer above a large active region. The system persists for several days, and must therefore be an important contribution to the slow solar wind.
- Sun: corona, Sun: heliosphere, Sun: magnetic topology, solar wind
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- An observation of solar active region expansion into the heliosphere
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