Simulation of the Solar Wind Dynamic Pressure Increase in 2014 and Its Effect on Energetic Neutral Atom Fluxes from the Heliosphere

2018 ◽  
Vol 859 (2) ◽  
pp. 104 ◽  
Author(s):  
E. J. Zirnstein ◽  
J. Heerikhuisen ◽  
D. J. McComas ◽  
N. V. Pogorelov ◽  
D. B. Reisenfeld ◽  
...  
Keyword(s):  
Solar Wind ◽  
Neutral Atom ◽  
Dynamic Pressure ◽  
Pressure Increase ◽  
Solar Wind Dynamic Pressure ◽  
Energetic Neutral Atom

scholarly journals Energetic neutral atom response to solar wind dynamic pressure enhancements

2007 ◽  
Vol 112 (A9) ◽  
pp. n/a-n/a ◽  
Author(s):  
D.-Y. Lee ◽  
S. Ohtani ◽  
P. C. Brandt ◽  
L. R. Lyons
Keyword(s):  
Solar Wind ◽  
Neutral Atom ◽  
Dynamic Pressure ◽  
Solar Wind Dynamic Pressure ◽  
Energetic Neutral Atom

Breathing of the Heliosphere

2021 ◽  
Vol 922 (2) ◽  
pp. 250
Author(s):  
Justyna M. Sokół ◽  
Maher A. Dayeh ◽  
Stephen A. Fuselier ◽  
Georgios Nicolaou ◽  
D. J. McComas ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Activity ◽  
Neutral Atom ◽  
Pressure Pulse ◽  
Dynamic Pressure ◽  
Ecliptic Plane ◽  
Abrupt Increase ◽  
Maximum Phase ◽  
Energetic Neutral Atom

Abstract In late 2016, the Interstellar Boundary Explorer (IBEX) observed an enhancement of hydrogen energetic neutral atom (ENA) flux in ∼20° south from the nose direction. This enhancement was a consequence of an abrupt increase of the solar wind (SW) dynamic pressure observed at 1 au in late 2014. In subsequent years, the increased flux of 4.3 keV ENAs was observed at higher latitudes filling in the heliosheath, in ENAs at lower energies, and the Ribbon flux. We observe that the rapid increase of SW pressure occurs every solar cycle (SC) from the beginning of the regular in situ SW measurements in the ecliptic plane. The SW pressure pulse happens about 4.7 yr from the beginning of each SC, it is during the maximum phase of solar activity, and repeats with a period of ∼10.2 yr. These repeating pulses of the SW pressure can cause periodic SC variations of the ENA production in the heliosheath. We follow McComas et al. results for the relation between SW pressure increase and ENA flux enhancement to investigate the periodic SW pressure increases and their consequences for the heliosphere. Our study of time delay between the cause (pressure pulse at 1 au) and the consequence (ENA enhancement) show that IBEX observed in 2009–2011 remnants of the SW pressure pulse that happened during the maximum of SC 23.

scholarly journals Vortex Generation and Auroral Response to a Solar Wind Dynamic Pressure Increase: Event Analyses

2021 ◽  
Author(s):  
Jinyan Zhao ◽  
Quanqi Shi ◽  
Anmin Tian ◽  
Xiao‐Chen Shen ◽  
James M Weygand ◽  
...  
Keyword(s):  
Solar Wind ◽  
Dynamic Pressure ◽  
Pressure Increase ◽  
Solar Wind Dynamic Pressure ◽  
Vortex Generation

scholarly journals Effects of a solar wind dynamic pressure increase in the magnetosphere and in the ionosphere

2010 ◽  
Vol 28 (10) ◽  
pp. 1945-1959 ◽  
Author(s):  
L. Juusola ◽  
K. Andréeová ◽  
O. Amm ◽  
K. Kauristie ◽  
S. E. Milan ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Dynamic Pressure ◽  
Timing Analysis ◽  
Leading Edge ◽  
Double Star ◽  
Pressure Increase ◽  
Solar Wind Dynamic Pressure ◽  
Positive Variation ◽  
First Contact

Abstract. On 17 July 2005, an earthward bound north-south oriented magnetic cloud and its sheath were observed by the ACE, SoHO, and Wind solar wind monitors. A steplike increase of the solar wind dynamic pressure during northward interplanetary magnetic field conditions was related to the leading edge of the sheath. A timing analysis between the three spacecraft revealed that this front was not aligned with the GSE y-axis, but had a normal (−0.58,0.82,0). Hence, the first contact with the magnetosphere occurred on the dawnside rather than at the subsolar point. Fortunately, Cluster, Double Star 1, and Geotail happened to be distributed close to the magnetopause in this region, which made it possible to closely monitor the motion of the magnetopause. After the pressure front had impacted the magnetosphere, the magnetopause was perceived first to move inward and then immediately to correct the overshoot by slightly expanding again such that it ended up between the Cluster constellation with Double Star 1 inside the magnetosphere and Geotail in the magnetosheath. Coinciding with the inward and subsequent outward motion, the ground-based magnetic field at low latitudes was observed to first strengthen and then weaken. As the magnetopause position stabilised, so did the ground-based magnetic field intensity, settling at a level slightly higher than before the pressure increase. Altogether the magnetopause was moving for about 15 min after its first contact with the front. The high latitude ionospheric signature consisted of two parts: a shorter (few minutes) and less intense preliminary part comprised a decrease of AL and a negative variation of PC. A longer (about ten minutes) and more intense main part of the signature comprised an increase of AU and a positive variation of PC. Measurements from several ground-based magnetometer networks (210 MM CPMN, CANMOS, CARISMA, GIMA, IMAGE, MACCS, SuperMAG, THEMIS, TGO) were used to obtain information on the ionospheric E×B drift. Before the pressure increase, a configuration typical for the prevailing northward IMF conditions was observed at high latitudes. The preliminary signature coincided with a pair of reverse convection vortices, whereas during the main signature, mainly westward convection was observed at all local time sectors. Afterwards, the configuration preceding the pressure increase was recovered, but with slightly enhanced convection. Based on the timing analysis, the existence of the preliminary signature coincided with the passage of the oblique pressure front, whereas during the main signature the front was already well past Earth. The main signature existed during the time the magnetopause was observed to move. As the position stabilised, also the signature disappeared.

scholarly journals Dayside reconnection enhancement resulting from a solar wind dynamic pressure increase

2007 ◽  
Vol 112 (A6) ◽  
pp. n/a-n/a ◽  
Author(s):  
A. Boudouridis ◽  
L. R. Lyons ◽  
E. Zesta ◽  
J. M. Ruohoniemi
Keyword(s):  
Solar Wind ◽  
Dynamic Pressure ◽  
Pressure Increase ◽  
Solar Wind Dynamic Pressure

Solar wind dynamic pressure enhancements and polar auroras

1998 ◽  
Vol 22 (9) ◽  
pp. 1305-1308 ◽  
Author(s):  
Y Zhang ◽  
D.J McEwen ◽  
I Oznovich
Keyword(s):  
Solar Wind ◽  
Dynamic Pressure ◽  
Solar Wind Dynamic Pressure

Statistical study of the effect of solar wind dynamic pressure fronts on the dayside and nightside ionospheric convection

2011 ◽  
Vol 116 (A10) ◽  
pp. n/a-n/a ◽  
Author(s):  
A. Boudouridis ◽  
L. R. Lyons ◽  
E. Zesta ◽  
J. M. Weygand ◽  
A. J. Ribeiro ◽  
...  
Keyword(s):  
Solar Wind ◽  
Statistical Study ◽  
Dynamic Pressure ◽  
Solar Wind Dynamic Pressure ◽  
Ionospheric Convection
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