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Titolo:
Evolution of a strong shock in the distant heliosphere
Autore:
Whang, YC; Lu, JY; Burlaga, LF;
Indirizzi:
Catholic Univ Amer, Dept Mech Engn, Washington, DC 20064 USA Catholic UnivAmer Washington DC USA 20064 Engn, Washington, DC 20064 USA NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA NASA Greenbelt MD USA 20771 , Extraterr Phys Lab, Greenbelt, MD 20771 USA
Titolo Testata:
JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
fascicolo: A9, volume: 104, anno: 1999,
pagine: 19787 - 19795
SICI:
0148-0227(19990901)104:A9<19787:EOASSI>2.0.ZU;2-M
Fonte:
ISI
Lingua:
ENG
Soggetto:
WIND TERMINATION SHOCK; PRESSURE-BALANCED STRUCTURES; MERGED INTERACTION REGIONS; ANOMALOUS COSMIC-RAYS; SOLAR-WIND; OUTER HELIOSPHERE; VOYAGER-2 OBSERVATIONS; PICKUP PROTONS; INTERPLANETARY SPACE; NEUTRAL HYDROGEN;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
47
Recensione:
Indirizzi per estratti:
Indirizzo: Whang, YC Catholic Univ Amer, Dept Mech Engn, Washington, DC 20064 USA Catholic Univ Amer Washington DC USA 20064 ington, DC 20064 USA
Citazione:
Y.C. Whang et al., "Evolution of a strong shock in the distant heliosphere", J GEO R-S P, 104(A9), 1999, pp. 19787-19795

Abstract

The 1991 global merged interaction region (GMIR) shock is a strong forwardshock observed from Voyager 2 on day 146 of 1991 at 34.6 AU at the leadingedge of the 1991 GMIR. This shock is the strongest shock ever identified from the Voyager data in the distant heliosphere. In this paper we study theevolution and propagation of the 1991 GMIR shock outside 34.6 AU in the upwind direction taking into account the influence of interstellar pickup protons. We calculate the time, location, and various variables of this shock in the subsequent 400 days. We use the shock interaction model to develop aR,t-simulation code to study this problem. The model treats the shock as asurface of discontinuity with zero thickness and uses the method of characteristics to study the evolution of the solar wind in the disturbed region. This model can accurately calculate the propagation speed and the strengthof the shock. The numerical solution shows that as the GMIR shock propagates from 35 AU to 150 AU, the shock speed decreases monotonically from 543 km/s to 478 km/s and the density ratio decreases from 2.55 to 2.09. The solar wind proton temperature and the pickup proton temperature on two sides ofthe shock decrease monotonically with increasing heliocentric distance. Across the shock the solar wind proton temperature ratio is high, namely, similar to 22 at 35 AU and similar to 11.5 at 150 AU, while the pickup proton temperature ratio is an order of magnitude smaller: similar to 2.1 at 35 AUand similar to 1.8 at 150 AU.

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Documento generato il 28/09/20 alle ore 21:32:40