Abstract
Laboratory experiments are presented simulating aspects of perpendicular ion heating and conic formation that are observed or hypothesized to occur in the terrestrial ionosphere and magnetosphere. Previous laboratory observations of ion conics in the presence of the current‐driven electrostatic ion cyclotron wave are reviewed. Field‐aligned ion beams, accompanied by beam‐generated electrostatic ion cyclotron modes, resulted in perpendicular energization of beam ions and also the heating of background plasma ions. Antenna‐launched broadband and narrow‐band lower hybrid waves produced considerable perpendicular ion heating and non‐Maxwellian “tail” formation. Laboratory results are discussed in light of in situ measurements by the S3‐3 satellite and the MARIE sounding rocket.
Highlights
Kintner, 1980; Cattell, 1981; Ternerin et al, 1981] and electrostatic ion cyclotron waves (EICW)This paper describesongoingresearchin laboratoryplasmasof phenomenathat are known or hypothesizedto occur in the terrestrial ionosphereand magnetosphereabove the auroraloval
EICW have been stimulated at low altitudes by man-made ion beams [Jones, 1981;Kintner and Kelley, 1981, 1982, 1983]
Theoretical and experimentalstudiesof parallel and perpendicularion beam injection into plasmasindicate that several electrostatic ion cyclotron modes may be destabilized and lead to ion acceleration and heating of beam and target plasma [Perkins, 1976;BOhmer et al, 1976; Hendel et al, 1976; Hauck et al, 1978;Yamadaet al., 1977].Reviewsof proposedion heating mechanismsare given by Mozer et al [1980], Kintner and Gorney [1984], Johnson [1979], and Lysak [1986]
Summary
This paper describesongoingresearchin laboratoryplasmasof phenomenathat are known or hypothesizedto occur in the terrestrial ionosphereand magnetosphereabove the auroraloval. We focuson processesleadingto perpendicularion heatingprocessesand someof the plasma conditionsrelevant to the formation of ion conics, upward flowingion distributionsexhibitinga preferredpitch anglein velocity space [Gorney et al, 1981; Horwitz, 1980; Ghielmetti et al, 1978; Whalen et al, 1978; Yau et al, 1983; Shelley, 1979].Magnetosphericionscommonlyare heatedto over 100 times their initial temperaturesperpendicularlyto geomagneticfield lines. They have been observedby sounding rockets and satellites from 400-km to over 130,000-km altitudewith variablecompositionosf H +, O+, andHe+. As indicated by equation (1), velocity components along the axes perpendicular to kr are not preferentially selected
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