HFA-like signatures observed with interball-tail spacecraft

Details HFA-like signatures observed with interball-tail spacecraft HFA-like signatures observed with interball-tail spacecraft

Jun 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aipc..471..551v&link_type=abstract

The solar wind nine conference. AIP Conference Proceedings, Volume 471, pp. 551-554 (1999).

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Magnetosphere Interactions

Scientific paper

We analyze HFAs observed with Interball-Tail in 1996. They are distinguished by a rotation of the magnetic field, by associated change in the shock regime from quasi-perpendicular to quasi-parallel and by a stronger flow deflection than at the bow shock. The magnetic field within an HFA is strongly varying, and its magnitude is often comparable to the solar wind value or less. Temperature jumps at HFAs are usually a factor of 2 higher, and the number density jumps are a factor of 2 lower than at the shock transition. Shock-like structure is frequently seen in the sunward part of an HFA and less frequently seen in the earthward part. Double (non-symmetric) structure is often seen in plasma parameters with a more isotropic velocity distribution in the sunward part of an HFA. A region with a cold ion component propagating antisunward separates these parts. Two ion components are usually seen inside an HFA, one of which seems to be a diluted and/or heated solar wind beam, and another which resembles diffuse upstream ions. A number of strong flow anomalies have been observed in the magnetosheath. A set of flow anomalies seen on April 12, 1996, in the magnetosheath suggests their upstream origin and may indicate that these flow anomalies may survive throughout the magnetosheath and lead to strong pressure variations at the magnetopause.

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