By F. Paul Esposito, Louis Witten
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Additional info for Asymptotic structure of space-time Proc. Cincinnati
The K-corona is dominant close to the sun, but falls off more rapidly 22 Fig. 2. Coronal brightness and flattening vs. solar elongation. Upper panel: Brightness of the K- and Fcoronae at solar equator and pole in units of the mean photospheric brightness. The background sky level at total solar eclipse is indicated. 1 0 1 2 SOLAR ELONGATION R/ Re 30 with solar distance than the F-corona because the electron density decreases faster than the dust number density. TIe asymptotic falloff rates for each contribution are shown.
PASS TlME'195400-70600 ,. ••• -. -16 (b) • •• •••• • • SEP-15°154 Ro .. -~-". ..... ".... f .. 7a,b. Helios 1 electron content measurements close to the first perihelion passage. Two contrasting examples are shown: (a) "quiet" corona (R = 63R 0 , 7 March 1975), and (b) "disturbed" corona (R = 54R0, 21 March 1975). The change in electron content Lllt(t) is given in units of 1016 eVm2 on the right or in terms of residual range on the left scale (D = plasma time delay x velocity of light). The rms variation in Lllt(t) given by the error bars for each curve is ca.
The change in electron content Lllt(t) is given in units of 1016 eVm2 on the right or in terms of residual range on the left scale (D = plasma time delay x velocity of light). The rms variation in Lllt(t) given by the error bars for each curve is ca. ±2 x 1016 el/m2 (a), and ±15 x 1016 el/m2 (b). S. 5R0 from west solar limb Kcoronagraph measurements during Carrington rotations 1625 and 1626. Time runs from right to left; the central meridian passages (CMP) of each date are indicated in the upper abscissa scale, Carrington longitude in the lower scale.
Asymptotic structure of space-time Proc. Cincinnati by F. Paul Esposito, Louis Witten