scholarly journals The variation of reconnection rate at the dayside magnetopause and cusp ion precipitation

1992 ◽  
Vol 97 (A10) ◽  
pp. 14841 ◽  
Author(s):  
M. Lockwood ◽  
M. F. Smith
Keyword(s):  
Reconnection Rate ◽  
Dayside Magnetopause

scholarly journals Dependence of the dayside magnetopause reconnection rate on local conditions

2015 ◽  
Vol 120 (8) ◽  
pp. 6386-6408 ◽  
Author(s):  
Shan Wang ◽  
Lynn M. Kistler ◽  
Christopher G. Mouikis ◽  
Steven M. Petrinec
Keyword(s):  
Reconnection Rate ◽  
Local Conditions ◽  
Dayside Magnetopause ◽  
Magnetopause Reconnection

scholarly journals On the location of dayside magnetic reconnection during an interval of duskward oriented IMF

2007 ◽  
Vol 25 (1) ◽  
pp. 219-238 ◽  
Author(s):  
J. A. Wild ◽  
S. E. Milan ◽  
J. A. Davies ◽  
M. W. Dunlop ◽  
D. M. Wright ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Magnetic Reconnection ◽  
Local Magnetic Field ◽  
High Latitudes ◽  
Reconnection Rate ◽  
Flux Tubes ◽  
Dayside Magnetopause ◽  
Line Passing ◽  
Open Flux

Abstract. We present space- and ground-based observations of the signatures of magnetic reconnection during an interval of duskward-oriented interplanetary magnetic field on 25 March 2004. In situ field and plasma measurements are drawn from the Double Star and Cluster satellites during traversals of the pre-noon sector dayside magnetopause at low and high latitudes, respectively. These reveal the typical signatures of flux transfer events (FTEs), namely bipolar perturbations in the magnetic field component normal to the local magnetopause, enhancements in the local magnetic field strength and mixing of magnetospheric and magnetosheath plasmas. Further evidence of magnetic reconnection is inferred from the ground-based signatures of pulsed ionospheric flow observed over an extended interval. In order to ascertain the location of the reconnection site responsible for the FTEs, a simple model of open flux tube motion over the surface of the magnetopause is employed. A comparison of the modelled and observed motion of open flux tubes (i.e. FTEs) and plasma flow in the magnetopause boundary layer indicates that the FTEs observed at both low and high latitudes were consistence with the existence of a tilted X-line passing through the sub-solar region, as suggested by the component reconnection paradigm. While a high latitude X-line (as predicted by the anti-parallel description of reconnection) may have been present, we find it unlikely that it could have been responsible for the FTEs observed in the pre-noon sector under the observed IMF conditions. Finally, we note that throughout the interval, the magnetosphere was bathed in ULF oscillations within the solar wind electric field. While no one-to-one correspondence with the pulsed reconnection rate suggested by the ground-based observation of pulsed ionospheric flow has been demonstrated, we note that similar periodicity oscillations were observed throughout the solar wind-magnetosphere-ionosphere system. These findings are consistent with previously proposed mechanisms of solar wind modulation of the dayside reconnection rate.

scholarly journals The location and rate of dayside reconnection during an interval of southward interplanetary magnetic field

2003 ◽  
Vol 21 (7) ◽  
pp. 1467-1482 ◽  
Author(s):  
M. Pinnock ◽  
G. Chisham ◽  
I. J. Coleman ◽  
M. P. Freeman ◽  
M. Hairston ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Polar Cap ◽  
Reconnection Rate ◽  
Comprehensive Description ◽  
Total Potential ◽  
Radar Network ◽  
Dayside Magnetopause ◽  
Magnetic Field Model ◽  
Magnetopause Reconnection

Abstract. Using ionospheric data from the SuperDARN radar network and a DMSP satellite we obtain a comprehensive description of the spatial and temporal pattern of day-side reconnection. During a period of southward interplanetary magnetic field (IMF), the data are used to determine the location of the ionospheric projection of the dayside magnetopause reconnection X-line. From the flow of plasma across the projected X-line, we derive the reconnection rate across 7 h of longitude and estimate it for the total length of the X-line footprint, which was found to be 10 h of longitude. Using the Tsyganenko 96 magnetic field model, the ionospheric data are mapped to the magnetopause, in order to provide an estimate of the extent of the reconnection X-line. This is found to be ~ 38 RE in extent, spanning the whole dayside magnetopause from dawn to dusk flank. Our results are compared with previously reported encounters by the Equator-S and Geotail spacecraft with a reconnecting magnetopause, near the dawn flank, for the same period. The SuperDARN observations allow the satellite data to be set in the context of the whole magnetopause reconnection X-line. The total potential associated with dayside reconnection was ~ 150 kV. The reconnection signatures detected by the Equator-S satellite mapped to a region in the ionosphere showing continuous flow across the polar cap boundary, but the reconnection rate was variable and showed a clear spatial variation, with a distinct minimum at 14:00 magnetic local time which was present throughout the 30-min study period.Key words. Magnetospheric physics (magnetopause, cusp and boundary layers; magnetosphere-ionoshere interactions) – Space plasma physics (magnetic reconnection)

scholarly journals A numerical model of the ionospheric signatures of time-varying magneticreconnection: I. ionospheric convection

2004 ◽  
Vol 22 (1) ◽  
pp. 73-91 ◽  
Author(s):  
M. Lockwood ◽  
S. K. Morley
Keyword(s):  
Numerical Model ◽  
Time Varying ◽  
Plasma Convection ◽  
Reconnection Rate ◽  
Ionospheric Convection ◽  
Ionospheric Conductivity ◽  
Geomagnetic Tail ◽  
Dayside Magnetopause ◽  
Potential Applications ◽  
General Time

Abstract. This paper presents a numerical model for predicting the evolution of the pattern of ionospheric convection in response to general time-dependent magnetic reconnection at the dayside magnetopause and in the cross-tail current sheet of the geomagnetic tail. The model quantifies the concepts of ionospheric flow excitation by Cowley and Lockwood (1992), assuming a uniform spatial distribution of ionospheric conductivity. The model is demonstrated using an example in which travelling reconnection pulses commence near noon and then move across the dayside magnetopause towards both dawn and dusk. Two such pulses, 8min apart, are used and each causes the reconnection to be active for 1min at every MLT that they pass over. This example demonstrates how the convection response to a given change in the interplanetary magnetic field (via the reconnection rate) depends on the previous reconnection history. The causes of this effect are explained. The inherent assumptions and the potential applications of the model are discussed. Key words. Ionosphere (ionosphere-magnetosphere interactions; plasma convection) – Magnetospheric physics (magnetosphere-ionosphere interactions; solar wind-magnetosphere interactions)

Recent ionospheric observations relating to solar-wind-magnetosphere coupling

1989 ◽  
Vol 328 (1598) ◽  
pp. 93-105 ◽  
Keyword(s):  
Solar Wind ◽  
Interplanetary Medium ◽  
Spatial Scales ◽  
Driving Mechanism ◽  
Reconnection Rate ◽  
Dayside Magnetopause ◽  
Solar Wind Flow ◽  
High Latitude Ionosphere ◽  
Low Altitude ◽  
Statistical Surveys

Simultaneous observations in the high-latitude ionosphere and in the near-Earth interplanetary medium have revealed the control exerted by the interplanetary magnetic field and the solar wind flow on field-perpendicular convection of plasma in both the ionosphere and the magnetosphere. Previous studies, using statistical surveys of data from both low-altitude polar-orbiting satellites and ground-based radars and magnetometers, have established that magnetic reconnection at the dayside magnetopause is the dominant driving mechanism for convection. More recently, ground-based data and global auroral images of higher temporal resolution have been obtained and used to study the response of the ionospheric flows to changes in the interplanetary medium. These observations show that ionospheric convection responds rapidly (within a few minutes) to both increases and decreases in the reconnection rate over a range of spatial scales, as well as revealing transient enhancements which are also thought to be related to magnetopause phenomena. Such results emphasize the potential of ground-based radars and other remotesensing instruments for studies of the Earth’s interaction with the interplanetary medium.

scholarly journals Geospace plume and its impact on dayside magnetopause reconnection rate

2021 ◽  
Author(s):  
Ying Zou ◽  
Brian M. Walsh ◽  
Xueling Shi ◽  
Larry Lyons ◽  
Jiang Liu ◽  
...  
Keyword(s):  
Reconnection Rate ◽  
Dayside Magnetopause ◽  
Magnetopause Reconnection

scholarly journals Dayside magnetopause reconnection and flux transfer events: BepiColombo earth-Flyby observations

2021 ◽  
Author(s):  
Weijie Sun ◽  
James A. Slavin ◽  
Rumi Nakamura ◽  
Daniel Heyner ◽  
Karlheinz J. Trattner ◽  
...  
Keyword(s):  
Flux Rope ◽  
Radial Component ◽  
High Plasma ◽  
Reconnection Rate ◽  
Transfer Event ◽  
Guide Field ◽  
Dayside Magnetopause ◽  
Flux Ropes ◽  
Theoretical Predictions ◽  
Flux Transfer

Abstract. This study analyzes the flux transfer event (FTE)-type flux ropes and magnetic reconnection around the dayside magnetopause during BepiColombo’s Earth flyby. The magnetosheath corresponds to a high plasma β (~ 8) and the IMF has a significant radial component. Six flux ropes are identified. The motion of flux rope together with the maximum magnetic shear model suggests that the reconnection X-line swipes BepiColombo near the magnetic equator due to an increase of the radial IMF. The flux rope with the highest flux content contains a clear coalescence signature, i.e., two smaller flux ropes merging, supporting theoretical predictions the flux content of flux ropes can grow through coalescence. The secondary reconnection associated with coalescence exhibits a large normalized guide field and a reconnection rate comparable to the reconnection rate measured at the magnetopause (~ 0.1).

Flux Rope Acceleration and Enhanced Magnetic Reconnection Rate

2003 ◽  
Author(s):  
C.Z. Cheng ◽  
Y. Ren ◽  
G.S. Choe ◽  
Y.-J. Moon
Keyword(s):  
Magnetic Reconnection ◽  
Flux Rope ◽  
Reconnection Rate

The Effect of Solar Wind Mach Numbers on the Occurrence Rate of Flux Transfer Events at the Dayside Magnetopause

2019 ◽  
Vol 46 (8) ◽  
pp. 4106-4113 ◽  
Author(s):  
C. Chen ◽  
T. R. Sun ◽  
C. Wang ◽  
Z. H. Huang ◽  
B. B. Tang ◽  
...  
Keyword(s):  
Solar Wind ◽  
Occurrence Rate ◽  
Flux Transfer Events ◽  
Dayside Magnetopause ◽  
Mach Numbers ◽  
Flux Transfer
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