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The profile and polarization of the coronal l? Beckers, j. M. , chipman, e.
We have constructed an instrument to measure the polarization of light emitted by the solar corona and prominences in order to constrain the strength and orientation of coronal magnetic fields. For the scattering in the forbidden lines of the solar corona it is appropriate, as we shall see later, to treat the y- and 2-oscillators as com- pletely coupled. We calculate the profile and polarization of the lî± line in the solar corona. Coronal temperature variation, solar wind and other non-thermal motions have been taken into account. By means of a photographic polarimeter, we attempted to measure both the amount and direction of linear polarization of all emission lines between 3400 and 9000 å in the inner corona (1. 034 ≤ r/r 0 ≤ … Coronal holes are open field regions, where the magnetic field has a predominant polarity, and leaves the sun (it must eventually return, but the closure of open field lines occurs at large distances from …
By means of a photographic polarimeter, we attempted to measure both the amount and direction of linear polarization of all emission lines between 3400 and 9000 å in the inner corona (1. 034 ≤ r/r 0 ≤ … Coronal holes are open field regions, where the magnetic field has a predominant polarity, and leaves the sun (it must eventually return, but the closure of open field lines occurs at large distances from …
