By Christopher T. Russell (auth.), D. Edgar Page (eds.)
The 1969 ESLAB symposium 'Intercorrelated satellite tv for pc Observations on the topic of sun occasions' used to be held at a time whilst the significance of bringing jointly degree ments made concurrently in numerous areas of area was once commencing to be liked. To-day it's universally authorized that the key experimental steps ahead in figuring out the physics of the Sun-Earth relationships usually are made via pre-planned correlated satellite tv for pc stories. Such issues have ended in the service provider of the overseas Magnetospheric research and the joint ESROj NASA overseas Magnetospheric Explorer, (Mother-Daughter-Heliocentric) undertaking. The 7th ESLAB symposium used to be deliberate as a stick to as much as that of 1969 with the purpose of deriving greatest take advantage of these spacecraft which via luck came across themselves at the same time working in numerous areas of the magnetosphere and interplanetary house. ESRO had introduced in early 1972 its HEOS-2 satellite tv for pc to enquire fields and debris within the unexplored area some distance above the North pole of the Earth and it grew to become transparent that the attention-grabbing new effects strolling back from that venture may profitably be associated with these from quite a few American and the U.S.S.R. PROGNOZ satellites. The publication follows the order of the symposium (unfortunately the PROGNOZ contribution didn't materialise) concentrating, via either evaluation lectures and of recent experimental effects, at the nature of the limits among the presentation the interplanetary medium and the magnetosphere and the interplay of every sector at the other.
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Additional info for Correlated Interplanetary and Magnetospheric Observations: Proceedings of the Seventh ESLAB Symposium Held at Saulgau, W. Germany, 22–25 May, 1973
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1973). --r-'--'--' -25 rl ,,, r-> March 4. 1968 IJ G*F L March 3. 1968 ~ 50 wE - ...... ::? RUSSELL value, and then repeat for the next interval. Since Dst is also responsive to the solar wind dynamic pressure, an attempt is also made to remove dynamic pressure contribution and calculate ring current losses using a 'true' ring current strength, Dst'. The calculation proceeds as follows: (I) Dst'(t)=Dst(t)-a Jmn(t) V2 (t)+b, (2) ot (Dst' (t)) = -cE~(t-r)-dDst'(t), (3) Dst(t+L1)=Dst(t)+L1 ot (Dst'(t)), o o where m is the proton mass, n the number density and V the velocity of the solar wind.
Geophys. Res. 77, 6696. Burch, J. : 1973, J. Geophys. Res. 78, 1047. Burton, R. , McPherron, R. , and Russell, C. : 1973, EOS Trans. AGU54, 415 (abstract). Caan, M. , McPherron, R. , and Russell, C. : 1973a, J. Geophys. , in press. Caan, M. , McPherron, R. , and Russell, C. : 1973b, in Proceedings of the Chapman Memorial Symposium on Magnetospheric Motions, Boulder, Colorado, June. Camidge, F. P. : 1970, Can. J. Phys. 48, 2002. Carpenter, D. L. : 1972, J. Geophys. Res. 77, 6854. Chapman, S. : 1940, Geomagnetism, vol.