Are Dynamical Sources Essential for the Production of the Ambient Solar Wind?
Abstract
At a basic level, the large structure of the solar corona and its connection to the solar wind has been known for many years. In the classic (near-solar minimum) picture, the slow solar wind is associated with the streamer belt at low latitudes, while the fast solar wind arises from coronal holes at higher latitudes. At a deeper level, important aspects of this connection still puzzle us. One such controversy is the origin of the slow solar wind. One group of theories assume that the slow wind primarily arises quasi-statically from regions of large expansion factor near the boundaries of coronal holes, while a contrasting set of theories argue that the slow solar wind is primarily dynamic in origin and involves the reconnection and exchange of open and closed fields. In this talk, we describe evidence for both sets of theories, and ongoing and future work that may help to resolve this question. Work supported by NASA, NSF and AFOSR.
- Publication:
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SDO 2016: Unraveling the Sun's Complexity
- Pub Date:
- October 2016
- Bibcode:
- 2016usc..confE..70L
- Keywords:
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- SDO;
- SDO 2016;
- Solar Dynamic Observatory;
- SDO-2016;
- SDO Workshop;
- SDO 2016: Unraveling the Sun's Complexity