The Nascent Solar Wind: Origin and Acceleration

2003 ◽  
Vol 588 (1) ◽  
pp. 566-577 ◽  
Author(s):  
Luca Teriaca ◽  
Giannina Poletto ◽  
Marco Romoli ◽  
Doug A. Biesecker
Keyword(s):  
Solar Wind ◽  
Solar Wind Origin

Coexistence of Earth-origin O+and solar wind-origin H+/He++in the distant magnetotail

1996 ◽  
Vol 23 (9) ◽  
pp. 985-988 ◽  
Author(s):  
K. Seki ◽  
M. Hirahara ◽  
T. Terasawa ◽  
I. Shinohara ◽  
T. Mukai ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Wind Origin

scholarly journals The superdense plasma sheet: Plasmaspheric origin, solar wind origin, or ionospheric origin?

1997 ◽  
Vol 102 (A10) ◽  
pp. 22089-22097 ◽  
Author(s):  
Joseph E. Borovsky ◽  
Michelle F. Thomsen ◽  
David J. McComas
Keyword(s):  
Solar Wind ◽  
Plasma Sheet ◽  
Solar Wind Origin

scholarly journals Observation of three distinct ion populations at the Kelvin-Helmholtz-unstable magnetopause

2008 ◽  
Vol 26 (6) ◽  
pp. 1559-1566 ◽  
Author(s):  
M. G. G. T. Taylor ◽  
B. Lavraud
Keyword(s):  
Boundary Layer ◽  
Solar Wind ◽  
Solar Wind Plasma ◽  
Double Star ◽  
Single Event ◽  
Helmholtz Instability ◽  
Temperature Anisotropy ◽  
Low Latitude ◽  
Solar Wind Origin ◽  
Unambiguous Conclusion

Abstract. We report Double Star spacecraft observations of the dusk-flank magnetopause and its boundary layer under predominantly northward interplanetary magnetic field (IMF). Under such conditions the flank low-latitude boundary layers (LLBL) of the magnetosphere are known to broaden. The primary candidate processes associated with the transport of solar wind plasma into the LLBL are: (1) local diffusive plasma transport associated with the Kelvin-Helmholtz instability (KHI), (2) local plasma penetration owing to magnetic reconnection in the vicinity of the KHI-driven vortices, and (3) via a pre-existing boundary layer formed through double high-latitude reconnection on the dayside. Previous studies have shown that a cold population of solar wind origin is typically mixed with a hot population of magnetospheric origin in the LLBL. The present observations show the coexistence of three distinct ion populations in the dusk LLBL, during an interval when the magnetopause is unstable to the KHI: (1) a typical hot magnetospheric population, (2) a cold population that shows parallel temperature anisotropy, and (3) a distinct third cold population that shows perpendicular temperature anisotropy. Although no unambiguous conclusion may be drawn from this single event, we discuss the possible mechanisms at work and the origin of each population by envisaging three likely sources: hot magnetospheric plasma sheet, cold magnetosheath of solar wind origin, and cold plasma of ionospheric origin.

scholarly journals Unusually high magnetic fields in the coma of 67P/Churyumov-Gerasimenko during its high-activity phase

2019 ◽  
Vol 630 ◽  
pp. A38 ◽  
Author(s):  
C. Goetz ◽  
B. T. Tsurutani ◽  
P. Henri ◽  
M. Volwerk ◽  
E. Behar ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Unusual Behavior ◽  
Cometary Plasma ◽  
Unusual Event ◽  
Interplanetary Coronal Mass Ejection ◽  
Magnetic Field Magnitude ◽  
Solar Wind Origin ◽  
The Impact ◽  
The Magnetic Field

Aims. On July 3, 2015, an unprecedented increase in the magnetic field magnitude was measured by the Rosetta spacecraft orbiting comet 67P/Churyumov-Gerasimenko (67P). This increase was accompanied by large variations in magnetic field and ion and electron density and energy. To our knowledge, this unusual event marks the highest magnetic field ever measured in the plasma environment of a comet. Our goal here is to examine possible physical causes for this event, and to explain this reaction of the cometary plasma and magnetic field and its trigger. Methods. We used observations from the entire Rosetta Plasma Consortium as well as energetic particle measurements from the Standard Radiation Monitor on board Rosetta to characterize the event. To provide context for the solar wind at the comet, observations at Earth were compared with simulations of the solar wind. Results. We find that the unusual behavior of the plasma around 67P is of solar wind origin and is caused by the impact of an interplanetary coronal mass ejection, combined with a corotating interaction region. This causes the magnetic field to pile up and increase by a factor of six to about 300 nT compared to normal values of the enhanced magnetic field at a comet. This increase is only partially accompanied by an increase in plasma density and energy, indicating that the magnetic field is connected to different regions of the coma.

MHD waves detected by ICE at distances ≥ 28 106 km from comet P/Halley: Cometary or solar wind origin?

1988 ◽  
pp. 97-102
Author(s):  
B. T. Tsurutani ◽  
A. L. Brinca ◽  
E. J. Smith ◽  
R. M. Thorne ◽  
F. L. Scarf ◽  
...  
Keyword(s):  
Solar Wind ◽  
Mhd Waves ◽  
Solar Wind Origin

Solar wind origin of 36Ar on Venus

Icarus ◽  
1981 ◽  
Vol 46 (1) ◽  
pp. 70-80 ◽  
Author(s):  
George W. Wetherill
Keyword(s):  
Solar Wind ◽  
Solar Wind Origin
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