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

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

2008 ◽  
Vol 26 (6) ◽  
pp. 1559-1566 ◽  
Author(s):  
M. G. G. T. Taylor ◽  
B. Lavraud

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.


2019 ◽  
Vol 630 ◽  
pp. A38 ◽  
Author(s):  
C. Goetz ◽  
B. T. Tsurutani ◽  
P. Henri ◽  
M. Volwerk ◽  
E. Behar ◽  
...  

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.


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

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

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