scholarly journals Cusp energetic ions: A bow shock source

1998 ◽  
Vol 25 (19) ◽  
pp. 3729-3732 ◽  
Author(s):  
S.-W. Chang ◽  
J. D. Scudder ◽  
S. A. Fuselier ◽  
J. F. Fennell ◽  
K. J. Trattner ◽  
...  
Keyword(s):  
Bow Shock ◽  
Shock Source ◽  
Energetic Ions

scholarly journals Cusp Energetic Ions: A Bow Shock Source.

1998 ◽  
Author(s):  
S. -W. Chang ◽  
J. D. Scudder ◽  
S. A. Fuselier ◽  
J. F. Fennell ◽  
K. J. Trattner
Keyword(s):  
Bow Shock ◽  
Shock Source ◽  
Energetic Ions

scholarly journals Autogenous and efficient acceleration of energetic ions upstream of Earth’s bow shock

Nature ◽  
2018 ◽  
Vol 561 (7722) ◽  
pp. 206-210 ◽  
Author(s):  
D. L. Turner ◽  
L. B. Wilson ◽  
T. Z. Liu ◽  
I. J. Cohen ◽  
S. J. Schwartz ◽  
...  
Keyword(s):  
Bow Shock ◽  
Energetic Ions ◽  
Earth’S Bow Shock

Magnetosheath high speed jets and foreshock transients observed by Cluster and MMS

2021 ◽  
Author(s):  
C.-Philippe Escoubet ◽  
Keyword(s):  
Solar Wind ◽  
High Speed ◽  
Cone Angle ◽  
Bow Shock ◽  
Magnetic Data ◽  
Energetic Ions ◽  
Dust Clouds ◽  
Simultaneous Measurements ◽  
Wind Measurements ◽  
Dominant Period

<p>Magnetosheath High Speed Jets (HSJs) are regularly observed downstream of the Earth’s bow shock. Determining their origin from spacecraft observations is however a challenge since (1) L1 solar wind monitors are usually used with their inherent inaccuracy when plasma and magnetic data are propagated to the bow shock, (2) the number of measurement points around the bow shock are always limited. Various mechanisms have been proposed to explain HSJs such as bow shock ripples, solar wind discontinuities, foreshock transients, pressure pulses or nano dust clouds and it is difficult to relate these to HSJs with the lack of simultaneous measurements near the bow shock and immediately upstream.  We will use a special Cluster campaign, where one spacecraft was lagged 8 hours behind the three other spacecraft, to obtain near-Earth solar wind measurements upstream of the bow shock, together with simultaneous measurements in the magnetosheath. The event of interest is first observed by ACE on 13 January 2019 as a short 10 minutes period of IMF-Bx dominant (cone angle around 140 deg.). This IMF-Bx dominant period is also observed, one hour later, by THEMIS B and C (ARTEMIS) and Geotail, which were at 60 and 25 R<sub>E</sub> from Earth on the dawnside. Cluster 1 and Cluster 2 just upstream of the bow shock, at 17 R<sub>E</sub> from Earth, observed also such IMF-Bx dominant period together with energetic ions reflected from the bow shock and foreshock transients. Preliminary analysis indicate that these transients would be hot flow anomalies. Finally, Cluster 3 and 4 and MMS1-4, a few R<sub>E</sub> from each other downstream of the shock, observed a turbulent magnetosheath with HSJs for 15 minutes. The HSJ characteristics are investigated with the constellation of 6 spacecraft, as well as their relation to hot flows anomalies observed upstream.</p>

scholarly journals Radial dependence of foreshock cavities: a case study

2004 ◽  
Vol 22 (12) ◽  
pp. 4143-4151 ◽  
Author(s):  
D. G. Sibeck ◽  
K. Kudela ◽  
T. Mukai ◽  
Z. Nemecek ◽  
J. Safrankova
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Field Strength ◽  
Magnetic Field Strength ◽  
Bow Shock ◽  
Radial Dependence ◽  
Energetic Ions ◽  
Interplanetary Physics ◽  
Bow Shocks

Abstract. We present a case study of Geotail, Interball-1, IMP-8, and Wind observations of density and magnetic field strength cavities excavated by the enhanced pressures associated with bursts of energetic ions in the foreshock. Consistent with theoretical predictions, the pressure of the energetic ions diminishes rapidly with upstream distance due to a decrease in the flux of energetic ions and a transition from near-isotropic to streaming pitch angle distributions. Consequently, the cavities can only be observed immediately upstream from the bow shock. A comparison of conditions upstream from the pre- and post-noon bow shock demonstrates that foreshock cavities introduce perturbations into the oncoming solar wind flow with dimensions smaller than those of the magnetosphere. Dayside geosynchronous magnetic field strength variations observed by GOES-8 do not track the density variations seen by any of the spacecraft upstream from the bow shock in a one-to-one manner, indicating that none of these spacecraft observed the precise sequence of density variations that actually struck the subsolar magnetopause. Key words. Interplanetary physics (energetic particles; planetary bow shocks) – Magnetospheric physics (solar wind-magnetosphere interactions)

Acceleration of energetic ions at the Earth's bow shock

1981 ◽  
Vol 8 (4) ◽  
pp. 401-404 ◽  
Author(s):  
M. A. Lee ◽  
G. Skadron ◽  
L. A. Fisk
Keyword(s):  
Bow Shock ◽  
Energetic Ions ◽  
Earth’S Bow Shock

scholarly journals Oscillations of energetic ions flux near the Earth's bow shock

2015 ◽  
Vol 120 (6) ◽  
pp. 4700-4710 ◽  
Author(s):  
A. A. Petrukovich ◽  
T. Inamori ◽  
J. Balaz ◽  
K. Kudela ◽  
M. Slivka ◽  
...  
Keyword(s):  
Bow Shock ◽  
Energetic Ions ◽  
Earth’S Bow Shock

scholarly journals A new MIR bow shock source in the Galactic center

2013 ◽  
Vol 9 (S303) ◽  
pp. 150-152 ◽  
Author(s):  
N. Sabha ◽  
M. Zamaninasab ◽  
A. Eckart ◽  
L. Moser
Keyword(s):  
Black Hole ◽  
Symmetry Axis ◽  
Galactic Center ◽  
Bow Shock ◽  
Shock Source ◽  
Stellar Cluster ◽  
Supermassive Black Hole ◽  
Sgr A ◽  
Central Parsec

AbstractWe find a convex-like feature at a distance of 0.68 pc (17″) from the position of the supermassive black hole, Sgr A*, at the center of the nuclear stellar cluster. This feature resembles a stellar bow shock with a symmetry axis pointing to the center. We discuss the possible nature of the feature and the implications of its alignment with other dusty comet-like objects inside the central parsec.

Sign in / Sign up

Export Citation Format

Share Document