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Variation in Coronal Activity from Solar Cycle 24 Minimum to Maximum Using Three-Dimensional Reconstructions of the Coronal Electron Density from STEREO/COR1Three-dimensional electron density distributions in the solar corona are reconstructed for 100 Carrington rotations (CR 2054 - 2153) during 2007/03 - 2014/08 using the spherically symmetric method from polarized white-light observations with the inner coronagraph (COR1) onboard the twin Solar Terrestrial Relations Observatory (STEREO). These three-dimensional electron density distributions are validated by comparison with similar density models derived using other methods such as tomography and a magnetohydrodynamics (MHD) model as well as using data from the Solar and Heliospheric Observatory (SOHO)/Large Angle and Spectrometric Coronagraph (LASCO)-C2. Uncertainties in the estimated total mass of the global corona are analyzed based on differences between the density distributions for COR1-A and -B. Long-term variations of coronal activity in terms of the global and hemispheric average electron densities (equivalent to the total coronal mass) reveal a hemispheric asymmetry during the rising phase of Solar Cycle 24, with the northern hemisphere leading the southern hemisphere by a phase shift of 7 - 9 months. Using 14 CR (approx. equal to 13-month) running averages, the amplitudes of the variation in average electron density between Cycle 24 maximum and Cycle 23/24 minimum (called the modulation factors) are found to be in the range of 1.6 - 4.3. These modulation factors are latitudinally dependent, being largest in polar regions and smallest in the equatorial region. These modulation factors also show a hemispheric asymmetry: they are somewhat larger in the southern hemisphere. The wavelet analysis shows that the short-term quasi-periodic oscillations during the rising and maximum phases of Cycle 24 have a dominant period of 7 - 8 months. In addition, it is found that the radial distribution of the mean electron density for streamers at Cycle 24 maximum is only slightly larger (by approx. equal to 30%) than at cycle minimum.
Document ID
20180003106
Acquisition Source
Goddard Space Flight Center
Document Type
Reprint (Version printed in journal)
Authors
Wang, Tongjiang
(Catholic Univ. of America Washington, DC, United States)
Reginald, Nelson L.
(Catholic Univ. of America Washington, DC, United States)
Davila, Joseph M.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
St. Cyr, O. Chris
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Thompson, William T.
(Adnet Systems, Inc. Greenbelt, MD, United States)
Date Acquired
May 27, 2018
Publication Date
July 21, 2017
Publication Information
Publication: Solar Physics
Publisher: Springer Verlag (Germany)
Volume: 292
Issue: 97
ISSN: 0038-0938
e-ISSN: 1573-093X
Subject Category
Solar Physics
Report/Patent Number
GSFC-E-DAA-TN50924
Report Number: GSFC-E-DAA-TN50924
ISSN: 0038-0938
E-ISSN: 1573-093X
Funding Number(s)
CONTRACT_GRANT: NNG11PL10A
CONTRACT_GRANT: 80GSFC17C0003
Distribution Limits
Public
Copyright
Other

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