Inbound waves in the solar corona: a direct indicator of Alfvén Surface location

Abstract

The tenuous supersonic solar wind that streams from the top of the corona passes through a natural boundary -- the Alfvén surface -- that marks the causal disconnection of individual packets of plasma and magnetic flux from the Sun itself. The Alfvén surface is the locus where the radial motion of the accelerating solar wind passes the radial Alfvén speed, and therefore any displacement of material cannot carry information back down into the corona. It is thus the natural outer boundary of the solar corona, and the inner boundary of interplanetary space. Using a new and unique motion analysis to separate inbound and outbound motions in synoptic visible-light image sequences from the COR2 coronagraph on board the STEREO-A spacecraft, we have identified inbound wave motion in the outer corona beyond 6 solar radii for the first time, and used it to determine that the Alfvén surface is at least 12.5 solar radii from the Sun over the polar coronal holes and 17 solar radii in the streamer belt, well beyond the distance planned for NASA's upcoming Solar Probe Plus mission. To our knowledge this is the first measurement of inbound waves in the outer solar corona, and the first direct measurement of lower bounds for the Alfvén surface.

Accepted by Astrophysical Journal, 11-April-2014 v2: corrected typos; formatted with emulateapj

References in corpus (2)

• Solar Magnetic Tracking. I. Software Comparison and Recommended Practices
• Turbulence in the sub-Alfvénic solar wind driven by reflection of low-frequency Alfvén waves

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