HR: 0830h
AN: SH21B-0154    [PDF]
TI: Solar Cycle Changes of Coronal Streamer Properties
AU: * Strachan, L
EM: lstrachan@cfa.harvard.edu
AF: Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-50, Cambridge, MA 02138 United States
AU: Baham, M
EM: michaelb@i-55.com
AF: Southern University and A&M College, Department of Physics, Baton Rouge, LA 70813 United States
AU: Miralles, M
EM: mmiralle@cfa.harvard.edu
AF: Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-50, Cambridge, MA 02138 United States
AU: Panasyuk, A
EM: apansyuk@cfa.harvard.edu
AF: Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-50, Cambridge, MA 02138 United States
AB: We have measured UV spectroscopic parameters, as a function of height for more than 30 coronal streamers in order to identify similarities between streamers at different phases of the solar cycle. For the period from 1996-2002, we provide line intensities, line widths, and line ratios for the O VI 1032/1037 doublet and intensities and line widths for the H I Ly-alpha line for these streamers. From such measurements we can derive plasma parameters (densities, temperatures, and outflow velocities) for O$^5+$ and protons as a function of heliocentric height $(1.5 > r/R_o > 5)$ in the streamers. This information is useful for setting empirical constraints on coronal heating and solar wind acceleration in streamers. This work is supported by NASA Grant NAG5-12781 to the Smithsonian Astrophysical Observatory and NASA subcontract OGSP21010200061SAO awarded to SAO through a grant to Southern Universty at Baton Rouge.
DE: 7509 Corona
DE: 7536 Solar activity cycle (2162)
DE: 7549 Ultraviolet emissions
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting