Observational data needs for plasma phenomena

Details Observational data needs for plasma phenomena Observational data needs for plasma phenomena

Oct 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981motc.conf...21n&link_type=abstract

In JPL Mod. Observational Tech. for Comets p 21-32 (SEE N82-13989 04-89)

Physics

Comet Heads, Comet Tails, Plasmas (Physics), Magnetic Fields, Radiation Pressure, Solar Wind

Scientific paper

Bright comets display a rich variety of interesting plasma phenomena which occur over an enormous range of spatial scales, and which require different observational techniques to be studied effectively. Wide-angle photography of high time resolution is probably the best method of studying the phenomenon of largest known scale: the plasma tail disconnection event (DE), which has been attributed to magnetic reconnection at interplanetary sector boundary crossings. These structures usually accelerate as they recede from the head region and observed velocities are typically in the range 50 V km/s. They are often visible for several days following the time of disconnection, and are sometimes seen out past 0.2 AU from the cometary head. The following areas pertaining to plasma phenomena in the ionoshere are addressed: the existence, size, and heliocentric distance variations of the contact surface, and the observational signatures of magnetic reconnection at sector boundary crossings.

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