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Radial Distribution of Compressive Waves in the Solar Corona Revealed by Akatsuki Radio Occultation Observations View all abstracts by submitter

Takeshi Imamura   Submitted: 2015-06-24 06:16

Radial variations of the amplitude and the energy flux of compressive waves in the solar corona were explored for the first time using a spacecraft radio occultation technique. By applying wavelet analysis to the frequency time series taken at heliocentric distances of 1.5-20.5 Rs (solar radii), quasi-periodic density disturbances were detected at almost all distances. The period ranges from 100 to 2000 s. The amplitude of the fractional density fluctuation increases with distance and reaches ~30% around 5 Rs, implying that nonlinearity of the wave field is potentially important. We further estimate the wave energy flux on the assumption that the observed periodical fluctuations are manifestations of acoustic waves. The energy flux increases with distance below ~6 Rs and seems to saturate above this height, suggesting that the acoustic waves do not propagate from the low corona but are generated in the extended corona, probably through nonlinear dissipation of Alfvén waves. The compressive waves should eventually dissipate through shock generation to heat the corona.

Authors: Mayu Miyamoto, Takeshi Imamura, Munetoshi Tokumaru, Hiroki Ando, Hiroaki Isobe, Ayumi Asai, Daikou Shiota, Tomoaki Toda, Bernd Häusler, Martin Pätzold, Alexander Nabatov, and Masato Nakamura
Projects: Other

Publication Status: ApJ (Published 2014 November 25)
Last Modified: 2015-06-24 14:44
Go to main E-Print page  25 Years of Self-Organized Criticality: Numerical Detection Methods  Outflow structure of the quiet Sun corona probed by spacecraft radio scintillations in strong scattering  Edit Entry  Download Preprint  Delete Entry 

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