Examining Periodic Solar Wind Density Structures in SECCHI HI1A

Details Examining Periodic Solar Wind Density Structures in SECCHI HI1A Examining Periodic Solar Wind Density Structures in SECCHI HI1A

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21630303v&link_type=abstract

American Astronomical Society, AAS Meeting #216, #303.03; Bulletin of the American Astronomical Society, Vol. 41, p.850

Astronomy and Astrophysics

Astronomy

Scientific paper

We present an analysis of small-scale periodic solar wind density enhancements observed in SECCHI HI1. We discuss their possible relationship to periodic fluctuations of the proton density observed in-situ with the Wind SWE data. Viall et al. [2008] used 11 years of solar wind density measurements at 1 AU and demonstrated that in addition to turbulent fluctuations, non-turbulent periodic density structures with length scales of tens to hundreds of megameters exist in the solar wind. Event studies of the periodic density structures reveal instances in which the density structures have alpha/proton abundance ratio changes associated with the density structures. Specifically, the alpha density varies with the same periodicity as the protons, but in antiphase. For those events, this strongly suggests either time varying or spatially varying coronal source plasma that created the density structures. If such periodic density structures observed at 1 AU are generated in the corona, then they may be observable in SECCHI HI1 data. We identify periodic density structures as they convect with the solar wind into the field of view of SECCHI HI and follow the train of structures as a function of time. The periodic density structures we analyze are comparable in size to the larger structures identified in-situ at 1 AU.
This research was supported through NASA Grant No. NNG05GK65G and an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA.

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