Journal
ASTROPHYSICAL JOURNAL
Volume 697, Issue 2, Pages 1384-1391Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/697/2/1384
Keywords
solar wind; Sun: corona; Sun: magnetic fields
Categories
Funding
- National Science Foundation through the NCAR Strategic Initiative Fund
- National Aeronautics and Space Administration [NNX08AU30G]
- Living with a Star Targeted Research and Technology Program
- SWM [ATM-0541567, NNG06GC89G, NNX08AL22G]
- National Science Foundation
Ask authors/readers for more resources
We employ a sequence of Doppler images obtained with the Coronal Multi-channel Polarimeter (CoMP) instrument to perform time-distance seismology of the solar corona. We construct the first k-omega diagrams of the region. These allow us to separate outward and inward propagating waves and estimate the spatial variation of the plane-of-sky-projected phase speed, and the relative amount of outward and inward directed wave power. The disparity between outward and inward wave power and the slope of the observed power-law spectrum indicate that low-frequency Alfvenic motions suffer significant attenuation as they propagate, consistent with isotropic MHD turbulence.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available