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Titolo:
Corotating interaction regions at high latitudes - Report of Working Group3
Autore:
Kunow, H; Lee, MA; Fisk, LA; Forsyth, RJ; Heber, B; Horbury, TS; Keppler, E; Kota, J; Lou, YQ; McKibben, RB; Paizis, C; Potgieter, MS; Roelof, EC; Sanderson, TR; Simnett, GM; Von Steiger, R; Tsurutani, BT; Wimmer-Schweingruber, RF; Jokipii, JR;
Indirizzi:
Univ Kiel, Inst Expt & Angew Phys, D-24118 Kiel, Germany Univ Kiel Kiel Germany D-24118 Expt & Angew Phys, D-24118 Kiel, Germany Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA Univ New Hampshire Durham NH USA 03824 tr Space Sci, Durham, NH 03824 USA Univ Michigan, Dept Atmospher & Space Sci, Ann Arbor, MI 48109 USA Univ Michigan Ann Arbor MI USA 48109 & Space Sci, Ann Arbor, MI 48109 USA Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London, EnglandUniv London Imperial Coll Sci Technol & Med London England don, England Max Planck Inst Aeron, Katlenburg Lindau, Germany Max Planck Inst Aeron Katlenburg Lindau Germany lenburg Lindau, Germany Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA Univ Arizona Tucson AZ USA 85721 Dept Planetary Sci, Tucson, AZ 85721 USA Univ Arizona, Dept Astron, Tucson, AZ USA Univ Arizona Tucson AZ USAUniv Arizona, Dept Astron, Tucson, AZ USA Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA Univ Chicago Chicago IL USA 60637 nrico Fermi Inst, Chicago, IL 60637 USA Univ Milan, Dipartimento Fis, Milan, Italy Univ Milan Milan ItalyUniv Milan, Dipartimento Fis, Milan, Italy Potchefstroom Univ Christian Higher Educ, ZA-2520 Potchefstroom, South Africa Potchefstroom Univ Christian Higher Educ Potchefstroom South Africa ZA-2520 Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA Johns Hopkins Univ Laurel MD USA ins Univ, Appl Phys Lab, Laurel, MD USA ESA, ESTEC, Dept Space Sci, Noordwijk, Netherlands ESA Noordwijk Netherlands ESTEC, Dept Space Sci, Noordwijk, Netherlands Univ Birmingham, Dept Phys & Astron, Birmingham, W Midlands, England Univ Birmingham Birmingham W Midlands England ngham, W Midlands, England Int Space Sci Inst, Bern, Switzerland Int Space Sci Inst Bern Switzerland t Space Sci Inst, Bern, Switzerland CALTECH, Jet Prop Lab, Pasadena, CA USA CALTECH Pasadena CA USACALTECH, Jet Prop Lab, Pasadena, CA USA Univ Bern, Inst Phys, Bern, Switzerland Univ Bern Bern SwitzerlandUniv Bern, Inst Phys, Bern, Switzerland
Titolo Testata:
SPACE SCIENCE REVIEWS
fascicolo: 1-2, volume: 89, anno: 1999,
pagine: 221 - 268
SICI:
0038-6308(1999)89:1-2<221:CIRAHL>2.0.ZU;2-X
Fonte:
ISI
Lingua:
ENG
Soggetto:
HELIOSPHERIC MAGNETIC-FIELD; SOLAR-WIND STREAM; INTERPLANETARY SECTOR STRUCTURE; ROTATING INTERACTION REGIONS; HIGH HELIOGRAPHIC LATITUDES; PLANETARY CURRENT SHEET; GALACTIC COSMIC-RAYS; ULYSSES OBSERVATIONS; ECLIPTIC-PLANE; ENERGETIC PARTICLES;
Keywords:
Solar wind; interplanetary medium; CIRs; high latitude heliosphere;
Tipo documento:
Review
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
71
Recensione:
Indirizzi per estratti:
Indirizzo: Kunow, H Univ Kiel, Inst Expt & Angew Phys, Leibnizstr 11-19, D-24118 Kiel, Germany Univ Kiel Leibnizstr 11-19 Kiel Germany D-24118 18 Kiel, Germany
Citazione:
H. Kunow et al., "Corotating interaction regions at high latitudes - Report of Working Group3", SPACE SCI R, 89(1-2), 1999, pp. 221-268

Abstract

Ulysses observed a stable strong CIR from early 1992 through 1994 during its first journey into the southern hemisphere. After the rapid latitude scan in early 1995, Ulysses observed a weaker CIR from early 1996 to mid-1997 in the northern hemisphere as it traveled back to the ecliptic at the orbitof Jupiter. These two CIRs are the observational basis of the investigation into the latitudinal structure of CIRs. The first CIR was caused by an extension of the northern coronal hole into the southern hemisphere during declining solar activity, whereas the second CIR near solar minimum activity was caused by small warps in the streamer belt. The latitudinal structure is described through the presentation of three 26-day periods during the southern CIR. The first at similar to 24 degrees S shows the full plasma interaction region including fast and slow wind streams, the compressed shocked flows with embedded stream interface and heliospheric current sheet (HCS), and the forward and reverse shocks with associated accelerated ions and electrons. The second at 40 degrees S exhibits only the reverse shock, accelerated particles, and the 26-day modulation of cosmic rays. The third at 60 degrees S shows only the accelerated particles and modulated cosmic rays. The possible mechanisms for the access of the accelerated particles and the CIR-modulated cosmic rays to high latitudes above the plasma interaction region are presented. They include direct magnetic field connection across latitude due to stochastic field line weaving or to systematic weaving caused by solar differential rotation combined with non-radial expansion of the fast wind. Another possible mechanism is particle diffusion across the average magnetic field, which includes stochastic field line weaving. A constraint on connection to a distant portion of the CIR is energy loss in the solarwind, which is substantial for the relatively slow-moving accelerated ions. Finally, the weaker northern CIR is compared with the southern CIR. It isweak because the inclination of the streamer belt and HCS decreased as Ulysses traveled to lower latitudes so that the spacecraft remained at about the maximum latitudinal extent of the HCS.

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Documento generato il 04/12/20 alle ore 22:28:10