Electron Density from white light coronal observations
Using WSM white light observations from SOHO/LASCO and Mauna Loa Mark 3,
we determine the electron density distributions .
We use data from
August 17 (DOY 230) ,
August 18 (DOY 231) ,
August 19 (DOY 232) ,
August 20 (DOY 233) .
and
August 24 (DOY 237) .
West limb streamer density radial profiles
August 17 (DOY 230) - densities averaged over 10 degrees latitude
August 18 (DOY 231) - densities averaged over 10 degrees latitude
August 19 (DOY 232) - densities averaged over 10 degrees latitude
August 20 (DOY 233) - densities avewraged over 10 degrees latitude
August 17-20 (DOY 230-233) - densities averaged over four days (approx. 56 degrees longitude) and 10 degrees latitude
Temperatures (and densities again) calculated assuming radial hydrostatic equilibrium and the ideal gas law for August 17-20, 1996, West limb colatitude 265-275.
Original pB data and fit for August 17-20, 1996, West limb colatitude 265-275.
Shortcut to the coefficients for radial profile of averaged over August 17-20, 1996, West limb colatitude 265-275.
North coronal hole density radial profiles
August 24 (DOY 237) - densities averaged over 10 degrees latitude
Temperatures (and densities again) calculated assuming radial hydrostatic equilibrium and the ideal gas law for August 24, 1996, North pole colatitudes 350 - 360.
Original pB data and fit August 24, 1996, North pole colatitudes 350 - 359.
Shortcut to the coefficients for radial profile of averaged over August 24, 1996, North pole colatitude 350 - 359.
