On the generation/decay of the storm‐enhanced density plumes: Role of the convection flow and field‐aligned ion flow

Storm‐enhanced density (SED) plumes are prominent ionospheric electron density increases at the dayside middle and high latitudes. The generation and decay mechanisms of the plumes are still not clear. We present observations of SED plumes during six storms between 2010 and 2013 and comprehensively analyze the associated ionospheric parameters within the plumes, including vertical ion flow, field‐aligned ion flow and flux, plasma temperature, and field‐aligned currents, obtained from multiple instruments, including GPS total electron content (TEC), Poker Flat Incoherent Scatter Radar (PFISR), Super Dual Auroral Radar Network, and Active Magnetosphere and Planetary Electrodynamics Response Experiment. The TEC increase within the SED plumes at the PFISR site can be 1.4–5.5 times their quiet time value. The plumes are usually associated with northwestward E  ×  B flows ranging from a couple of hundred m s −1 to > 1 km s −1 . Upward vertical flows due to the projection of these E  ×  B drifts are mainly responsible for lifting the plasma in sunlit regions to higher altitude and thus leading to plume density enhancement. The upward vertical flows near the poleward part of the plumes are more persistent, while those near the equatorward part are more patchy. In addition, the plumes can be collocated with either upward or downward field‐aligned currents (FACs) but are usually observed equatorward of the peak of the Region 1 upward FAC, suggesting that the northwestward flows collocated with plumes can be either subauroral or auroral flows. Furthermore, during the decay phase of the plume, large downward ion flows, as large as ~200 m s −1 , and downward fluxes, as large as 10 14  m −2  s −1 , are often observed within the plumes. In our study of six storms, enhanced ambipolar diffusion due to an elevated pressure gradient is able to explain two of the four large downward flow/flux cases, but this mechanism is not sufficient for the other two cases where the flows are of larger magnitude. For the latter two cases, enhanced poleward thermospheric wind is suggested to be another mechanism for pushing the plasma downward along the field line. These downward flows should be an important mechanism for the decay of the SED plumes. Key Points Vertical plasma lifting leads to density increase during plume generation phase Large downward field‐aligned ion flow/flux seen during plume decay phase Complex‐induced plasma drifts seen indicating plumes' highly dynamic naturePeer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/1/StormB_tec_20121113.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/2/QuietTimeF_tec_20100821.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/3/StormD_tec_20120423.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/4/QuietTimeC_tec_20120928.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/5/SupplementaryMaterial_Figure3_quiet.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/6/QuietTimeE_tec_20110203.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/7/StormC_tec_20120930.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/8/StormA_tec_20130423.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/9/StormF_tec_20100803.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/10/jgra51348.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/11/SupplementaryMaterial_Figure4_quiet.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/12/QuietTimeA_tec_20130421.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/13/QuietTimeD_tec_20120429.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/14/QuietTimeB_tec_20121109.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/109661/15/StormE_tec_20110204.pd

Multi‐instrument observations of SED during 24–25 October 2011 storm: Implications for SED formation processes

We present multiple instrument observations of a storm‐enhanced density (SED) during the 24–25 October 2011 intense geomagnetic storm. Formation and the subsequent evolution of the SED and the midlatitude trough are revealed by global GPS vertical total electron content maps. In addition, we present high time resolution Poker Flat Incoherent Scatter Radar (PFISR) observations of ionospheric profiles within the SED. We divided the SED observed by PFISR into two parts. Both parts are characterized by elevated ionospheric peak height ( h m F 2 ) and total electron content, compared to quiet time values. However, the two parts of the SED have different characteristics in the electron temperature ( T e ), the F region peak density ( N m F 2 ), and convection flows. The first part of the SED is associated with enhanced T e in the lower F region and reduced T e in the upper F region and is collocated with northward convection flows. The N m F 2 was lower than quiet time values. The second part of the SED is associated with significantly increased N m F 2 , elevated T e at all altitudes and is located near the equatorward boundary of large northwestward flows. Based on these observations, we suggest that the mechanisms responsible for the formation of the two parts of the SED may be different. The first part is due to equatorward expansion of the convection pattern and the projection of northward convection flows in the vertical direction, which lifts the ionospheric plasma to higher altitudes and thus reduces the loss rate of plasma recombination. The second part is more complicated. Besides equatorward expansion of the convection pattern and large upward flows, evidences of other mechanisms, including horizontal advection due to fast flows, energetic particle precipitation, and enhanced thermospheric wind in the topside ionosphere, are also present. Estimates show that contribution from precipitating energetic protons is at most ~10% of the total F region density. The thermospheric wind also plays a minor role in this case. Key Points SED formation during 24–25 October 2011 geomagnetic storm studied PFISR observations within the SED shown Electric field plays a major role in the formation of SED in this stormPeer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/102626/1/jgra50711.pd

PFISR observation of intense ion upflow fluxes associated with an SED during the 1 June 2013 geomagnetic storm

The Earth’s ionosphere plays an important role in supplying plasma into the magnetosphere through ion upflow/outflow, particularly during periods of strong solar wind driving. An intense ion upflow flux event during the 1 June 2013 storm has been studied using observations from multiple instruments. When the open‐closed field line boundary (OCB) moved into the Poker Flat incoherent scatter radar (PFISR) field of view, divergent ion fluxes were observed by PFISR with intense upflow fluxes reaching ~1.9 × 1014 m−2 s−1 at ~600 km altitude. Both ion and electron temperatures increased significantly within the ion upflow, and thus, this event has been classified as a type 2 upflow. We discuss factors contributing to the high electron density and intense ion upflow fluxes, including plasma temperature effect and preconditioning by storm‐enhanced density (SED). Our analysis shows that the significantly enhanced electron temperature due to soft electron precipitation in the cusp can reduce the dissociative recombination rate of molecular ions above ~400 km and contributed to the density increase. In addition, this intense ion upflow flux event is preconditioned by the lifted F region ionosphere due to northwestward convection flows in the SED plume. During this event, the OCB and cusp were detected by DMSP between 15 and 16 magnetic local times, unusually duskward. Results from a global magnetohydrodynamics simulation using the Space Weather Modeling Framework have been used to provide a global context for this event. This case study provides a more comprehensive mechanism for the generation of intense ion upflow fluxes observed in association with SEDs.Key PointsA more comprehensive mechanism for the generation of intense ion upflow fluxes observed in association with SEDs has been providedNorthwestward convection flows lift the F region ionosphere within SED and provide seed population for intense ion upflow fluxesSignificantly elevated electron temperature reduces recombination rate contributing to density increasePeer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/136519/1/jgra53328.pdfhttps://deepblue.lib.umich.edu/bitstream/2027.42/136519/2/jgra53328_am.pd

Earth's ion upflow associated with polar cap patches: global and in-situ observations

We report simultaneous global monitoring of a patch of ionization and in situ observation of ion upflow at the center of the polar cap region during a geomagnetic storm. Our observations indicate strong fluxes of upwelling O+ ions originating from frictional heating produced by rapid antisunward flow of the plasma patch. The statistical results from the crossings of the central polar cap region by Defense Meteorological Satellite Program F16–F18 from 2010 to 2013 confirm that the field-aligned flow can turn upward when rapid antisunward flows appear, with consequent significant frictional heating of the ions, which overcomes the gravity effect. We suggest that such rapidly moving patches can provide an important source of upwelling ions in a region where downward flows are usually expected. These observations give new insight into the processes of ionosphere-magnetosphere coupling

Polar cap patch transportation beyond the classic scenario

We report the continuous monitoring of a polar cap patch, encompassing its creation, and a subsequent evolution that differs from the classic behavior. The patch was formed from the storm-enhanced density plume, by segmentation associated with a subauroral polarization stream generated by a substorm. Its initial antisunward motion was halted due to a rapidly changing of interplanetary magnetic field (IMF) conditions from strong southward to strong eastward with weaker northward components, and the patch subsequently very slowly evolved behind the duskside of a lobe reverse convection cell in afternoon sectors, associated with high-latitude lobe reconnection, much of it fading rapidly due to an enhancement of the ionization recombination rate. This differs from the classic scenario where polar cap patches are transported across the polar cap along the streamlines of twin-cell convection pattern from day to night. This observation provides us new important insights into patch formation and control by the IMF, which has to be taken into account in F region transport models and space weather forecasts

Multiresolution Modeling of High-Latitude Ionospheric Electric Field Variability and Impact on Joule Heating Using SuperDARN Data.

The most dynamic electromagnetic coupling between the magnetosphere and ionosphere occurs in the polar upper atmosphere. It is critical to quantify the electromagnetic energy and momentum input associated with this coupling as its impacts on the ionosphere and thermosphere system are global and major, often leading to considerable disturbances in near-Earth space environments. The current general circulation models of the upper atmosphere exhibit systematic biases that can be attributed to an inadequate representation of the Joule heating rate resulting from unaccounted stochastic fluctuations of electric fields associated with the magnetosphere-ionosphere coupling. These biases exist regardless of geomagnetic activity levels. To overcome this limitation, a new multiresolution random field modeling approach is developed, and the efficacy of the approach is demonstrated using Super Dual Auroral Radar Network (SuperDARN) data carefully curated for the study during a largely quiet 4-hour period on February 29, 2012. Regional small-scale electrostatic fields sampled at different resolutions from a probabilistic distribution of electric field variability conditioned on actual SuperDARN LOS observations exhibit considerably more localized fine-scale features in comparison to global large-scale fields modeled using the SuperDARN Assimilative Mapping procedure. The overall hemispherically integrated Joule heating rate is increased by a factor of about 1.5 due to the effect of random regional small-scale electric fields, which is close to the lower end of arbitrarily adjusted Joule heating multiplicative factor of 1.5 and 2.5 typically used in upper atmosphere general circulation models. The study represents an important step toward a data-driven ensemble modeling of magnetosphere-ionosphere-atmosphere coupling processes

Formation of Storm Enhanced Density (SED) during Geomagnetic Storms: Observation and Modeling Study

Ionospheric density often exhibits significant variations, which affect the propagation of radio signals that pass through or are reflected by the ionosphere. One example of these effects is the loss of phase lock and range errors in Global Navigation Satellite Systems (GNSS) signals. Because our modern society increasingly relies on ground-toground and ground-to-space communications and navigation, understanding the sources of the ionospheric density variation and monitoring its dynamics during space weather events have great importance. Storm-enhanced density (SED) is one of the most prominent ionospheric density structures that can have significant space weather impact. In this presentation, we present multi-instrument observations and modeling results of the SED events, focusing on the formation processes. Formation and the subsequent evolution of the SED and the mid-latitude trough are revealed by global GPS vertical total electron content (VTEC) maps. High time resolution Poker Flat Advanced Modular Incoherent Scatter Radar (PFISR) observations are used to reveal the ionospheric characteristics within the SED when available. In addition, field-aligned current data from Active Magnetosphere and Planetary Electrodynamics Response Experiment (AMPERE) and large-scale convection flow pattern measured by the Super Dual Auroral Radar Network (SuperDARN) will also be used to provide large-scale context. Based on these observations, we will discuss the role of energetic particle precipitation, enhanced thermospheric wind, and enhanced convection flows, including subauroral polarization streams (SAPS), in creating the SED. In the modeling part, we use the Global Ionosphere Thermosphere Model (GITM) to study the SED formation. Various high-latitude drivers, such as the potential patterns from the Weimer model, outputs from the Assimilative Mapping of Ionospheric Electrodynamics (AMIE) and the Hot Electron Ion Drift Integrator Model (HEIDI) are used to drive GITM. Effects of different drivers as well as different physical processes on creating SEDs are assessed