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Titolo:
OBSERVATION BY ULYSSES OF HOT (SIMILAR-TO-270 KEV) CORONAL PARTICLES AT 32-DEGREES SOUTH HELIOLATITUDE AND 4.6 AU
Autore:
ARMSTRONG TP; HAGGERTY D; LANZEROTTI LJ; MACLENNAN CG; ROELOF EC; PICK M; SIMNETT GM; GOLD RE; KRIMIGIS SM; ANDERSON KA; LIN RP; SARRIS ET; FORSYTH R; BALOGH A;
Indirizzi:
UNIV KANSAS,DEPT PHYS & ASTRON LAWRENCE KS 66045 AT&T BELL LABS MURRAY HILL NJ 07974 APPL PHYS LAB LAUREL MD 00000 OBSERV PARIS F-92190 MEUDON FRANCE UNIV BIRMINGHAM BIRMINGHAM B15 2TT W MIDLANDS ENGLAND UNIV CALIF BERKELEY BERKELEY CA 94720 DEMOCRITOS UNIV THRACE ATHENS GREECE UNIV LONDON IMPERIAL COLL SCI TECHNOL & MED,DEPT PHYS LONDON SW7 2AZ ENGLAND
Titolo Testata:
Geophysical research letters
fascicolo: 17, volume: 21, anno: 1994,
pagine: 1747 - 1750
SICI:
0094-8276(1994)21:17<1747:OBUOH(>2.0.ZU;2-5
Fonte:
ISI
Lingua:
ENG
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Science Citation Index Expanded
Citazioni:
4
Recensione:
Indirizzi per estratti:
Citazione:
T.P. Armstrong et al., "OBSERVATION BY ULYSSES OF HOT (SIMILAR-TO-270 KEV) CORONAL PARTICLES AT 32-DEGREES SOUTH HELIOLATITUDE AND 4.6 AU", Geophysical research letters, 21(17), 1994, pp. 1747-1750

Abstract

An unusual event of streaming 60 keV-2 MeV ions (with energy spectrumpeaked approximately 270 keV) and of 42-315 keV electrons occurred during the passage of a coronal mass ejection (CME) over the Ulysses spacecraft June 9-13, 1993, located at helioradius 4.6 AU and heliolatitude 32-degrees south. The topology of the interplanetary magnetic field(IMF) within the CME has been identified as a helical magnetic flux rope by Gosling et al. [1994]. The ion and electron pitch angle distributions (PADs) had a bidirectional component in the outer (large-pitch)regions of the flux rope, while there were strongly unidirectional (antisunward) beams in the inner (small-pitch) core of the structure, where the electron PADs also displayed a distinctive depletion of electrons moving inward (sunward). Because the core ion beam was narrow, we can associate the observed energy spectrum in the peak direction of the beam (characterized by a Maxwellian with kT = 270 keV) directly withthe spectrum injected in the inner heliosphere. The well-defined spatial structure of the event and the absence of any clear signatures of local interplanetary shock acceleration during the period June 9-17 implies that the injection source could have been a long-lived hot coronal ion population. The ''weak scattering'' electron PAD implies that the other (antisunward) end of the core of the flux rope was magnetically connected, not back to the sun, but rather to the outer heliosphere.

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Documento generato il 26/11/20 alle ore 20:33:33