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Titolo:
Relation between cusp and mantle in MHD simulation
Autore:
Siscoe, GL; Erickson, GM; Sonnerup, BUO; Maynard, NC; Siebert, KD; Weimer, DR; White, WW;
Indirizzi:
Boston Univ, Ctr Space Phys, Boston, MA 02215 USA Boston Univ Boston MA USA 02215 niv, Ctr Space Phys, Boston, MA 02215 USA Dartmouth Coll, Thayer Sch Engn, Hanover, NH 03755 USA Dartmouth Coll Hanover NH USA 03755 hayer Sch Engn, Hanover, NH 03755 USA Mission Res Corp, Nashua, NH 03060 USA Mission Res Corp Nashua NH USA 03060 ssion Res Corp, Nashua, NH 03060 USA
Titolo Testata:
JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
fascicolo: A6, volume: 106, anno: 2001,
pagine: 10743 - 10749
SICI:
0148-0227(20010601)106:A6<10743:RBCAMI>2.0.ZU;2-T
Fonte:
ISI
Lingua:
ENG
Soggetto:
COLD O+ BEAMS; MAGNETOTAIL BOUNDARY; POLAR MAGNETOSPHERE; LOBE/MANTLE REGIONS; PLASMA MANTLE; GEOTAIL DATA; MODEL; LAYER;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
21
Recensione:
Indirizzi per estratti:
Indirizzo: Siscoe, GL Boston Univ, Ctr Space Phys, 725 Commonwealth Ave, Boston, MA 02215 USA Boston Univ 725 Commonwealth Ave Boston MA USA 02215 02215 USA
Citazione:
G.L. Siscoe et al., "Relation between cusp and mantle in MHD simulation", J GEO R-S P, 106(A6), 2001, pp. 10743-10749

Abstract

A global MHD simulation illustrates the relative contributions to magnetotail structure of two mantle models. One model is the data-based picture that Rosenbauer et al. [1975] originally put forth showing the cusp to be the source of the mantle. In this model the cusp is populated by magnetosheath particles that enter it as a consequence of magnetic reconnection on the dayside magnetopause. The other model, which derives from MHD considerations,notes that since the mantle lies on open magnetic field lines, the solar wind should be able to enter it along the tail magnetopause downwind from the cusp. In the simulation results presented here, both modes of plasma entry into the mantle occur and their relative contributions are seen. The mantle, identified in the simulation as the volume of the tail occupied by a slow-mode expansion wave filled with magnetosheath plasma, lies mostly on streamlines that originate in the dayside cusp (cusp model), but the bulk of plasma inflow comes directly from the magnetosheath (magnetosheath model). The demarcation between streamlines originating in the cusp (cusp model) andstreamlines originating in the solar wind (magnetosheath model) is sharp. We call this demarcation the fluopause. The fluopause is the downwind extension of the solar wind stagnation streamline. At 100 R-E downtail the fluopause lies several R-E inside the magnetopause identified by the peak in theelectrical current that defines the magnetotail boundary. The spatial separation between the fluopause and the magnetopause defines the volume to which the magnetosheath model refers. Whereas the magnetopause clearly marks the start of the slow-mode expansion wave that defines the mantle, all MHD parameters and their slopes are continuous across the fluopause. The fluopause is only determinable by following streamlines. Streamlines in the mantlethat originate in the solar wind (magnetosheath model) do not converge on the plasma sheet and, so, are not a likely source of particles for the plasma sheet. Streamlines in the mantle that originate in the cusp (cusp model)do converge on the plasma sheet and, so, are likely candidates for the particles that supply the plasma sheet. At their earthward ends, streamlines that originate in the cusp reach low altitudes and might, in nature, be populated with ionospheric plasma. An implication of the present result is thatthe inner portions of mantle encounters that have been identified in IMP 8and Geotail data refer to plasma that has spent part of its life in the dayside cusp and possibly in the ionosphere. The latter possibility might account for Geotail observations that identify O+ as a common constituent of deep-mantle plasma.

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Documento generato il 30/03/20 alle ore 20:07:13