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No study has assessed the durability of pulmonary vein isolation (PVI) with radiofrequency (RF) and cryoballoon (CB) in patients with persistent atrial fibrillation. These data are especially lacking for those with significantly diseased left atria (LA). The goals of this study were to assess PVI durability in patients with significant LA disease and to compare reconnection rates between RF and CB. Forty-four patients (mean age 63 years; 34 (77%) male; median time since atrial fibrillation diagnosis 22.5 months; median indexed LA volume 36 mL/m2) were randomized 1:1 to RF or CB PVI. A redo procedure using ultra-high-density electroanatomic mapping was mandated at 2 months, where PV reconnections were identified and reisolated. Thirty-eight patients underwent both procedures (CB n = 17; RF n = 21). Index RF procedures were longer (median 158 minutes vs 97 minutes; P <.001) but required less fluoroscopy (9.5 minutes vs 23 minutes; P <.001). At the index RF procedure, a median of 47% of LA myocardium had voltage < 0.5 mV, suggesting that half of the mapped LA comprised scar. PV reconnection was observed in 73 of 152 PVs (48.0%) and was more frequent with CB (58.8%) than with RF (39.3%) (P =.022). Reconnection of at least 1 PV was detected in >75% of patients. Significantly more ablation was required during the redo procedure to reisolate PVs in the CB arm (median 10.8 minutes vs 1.2 minutes; P <.001). PVI durability may be poor in those with significant LA scarring and dilatation, even with modern thermal ablation technologies. RF resulted in significantly better PVI durability than did CB in this complex population. [ABSTRACT FROM AUTHOR]

• The adjustment of a restored sand-gravel bed stream was monitored over 3 years. • Observed a net deposition response of 64.3 ± 32.1 m3. • Relative pool volume and morphological complexity were not improved by restoration. • Grain size was similar to pre-restoration but substrate diversity increased. • Backwaters were a sink for fine sediment, organic matter and phosphorous. Restoration is applied to reinstate geomorphic processes and complexity in degraded streams, but case studies of responses remain rare. A 236 m long reach of the Logie Burn, a straightened sand-gravel bed stream in north-east Scotland was restored by reconnecting its pre-modification channel to improve habitat and reduce nutrient transfer. Morphological, sedimentary and retention (wood, phosphorous and organic matter) responses were monitored over 3 years. Monitoring over 2 years was also conducted in a nearby control reach. A net deposition response of 64.3 ± 32.1 m3, a near two-fold enlargement of channel cross section area and a reduction of bed slope from 0.0008 m m−1 to 0.00014 m m−1 were observed in the restored reach over 3 years. The control reach in contrast was relatively stable. After 3 years, relative pool volume and morphological complexity were similar to the control reach and its pre-restoration state. Substrate diversity (Shannon-Wiener index: H') after an initial increase, declined but at the end of the monitoring period was higher (H' = 1.26) than the control reach (H' = 1) and pre-restoration reach (H' = 0.8). Following restoration, the median sediment size (D 50) of the majority of the restored main channel reduced from 3.4 mm to 1.5 mm – a similar value to pre-restoration (D 50 = 1.6 mm) – reflecting the net deposition response although the overall grain size distribution was not statistically different. No relationship between geomorphically effective flows and morphological change was found reflecting geomorphic sensitivity due to the reconnection work and wood recruitment mainly driven by tree collapse in response to channel readjustment. The retention of organic matter (OM) and total phosphorous (TP) did not increase in the main channel but did within the backwaters which also exhibited a statistically significant fining response. Overall, these results suggest that the physical habitat improvement value of the scheme so far has been limited but the creation of the backwaters may have increased the capacity of the reach to retain nutrients and fine sediment. [ABSTRACT FROM AUTHOR]

Abstract Previous studies have shown that dynamic pressure impacts (e.g., shocks initiating CME storms) with southward IMF promptly lead to strong auroral nightside activity and concurrent poleward expansion (indicating strong nightside reconnection), and strong enhancements in convection and currents. Here we use a combination of ground-based ASI and radar observations to further describe this response, to address what is driving the strong activity, and to suggest similar driving in other situations. Consistent with some previous studies, we find that shock driven auroral activity and poleward expansion resembles a substorm, but starts from an already broad MLT sector without much subsequent azimuthal expansion and without classical brightening of the equatorward-most arc. We furthermore find a large enhancement of meso-scale ionospheric polar cap flows heading towards the nightside separatrix immediately after shock impact. Recent studies have shown that such enhanced flows often cross the separatrix leading to plasma sheet flow bursts, poleward boundary intensifications (PBIs), streamers, and poleward motion of the polar cap boundary from reconnection. Thus these flow enhancements, which must extend outward along field lines from the ionosphere, are an attractive candidate as the driver for the almost immediate strong auroral, current, and reconnection activity resulting from shock impact. We also discuss and present some evidence that this phenomenon may be more general, leading to similar oval responses without a shock impact, including during and following the expansion phase of some substorms. These suggestions could lead to some possibly fundamental questions, such as when do polar cap convection enhancements lead to a substorm growth phase versus leading directly to strong polar expansion of, and strong activity along, the auroral oval field line region? Highlights • Immediate strong auroral, current, reconnection activity results from shock impact. • Shock driven aurora resembles substorm expansion; broader, from poleward boundary. • Enhanced meso-scale polar cap flows towards nightside separatrix after shock impact. • Above enhanced flows attractive candidate for driver of immediate strong responses. [ABSTRACT FROM AUTHOR]

Background: The reconnection of left atrial-pulmonary vein (LA-PV) conduction after the initial procedure of pulmonary vein (PV) isolation is not rare, and is one of the main cause of atrial fibrillation (AF) recurrence after PV isolation.Objective: We investigated feasibility of a new ultrahigh-resolution mapping system using a 64-pole small basket catheter for the identification of LA-PV conduction gaps.Methods: This prospective study included 31 consecutive patients (20 with persistent AF) undergoing a second ablation after a PV isolation procedure with LA-PV reconnected conduction at any of the 4 PVs. An LA-PV map was created using the mapping system, and ablation was performed at the estimated gap location.Results: The propagation map identified 54 gaps from 39 ipsilateral PV pairs, requiring manual electrogram reannotation for 23 gaps (43%). Gaps at the anterior and carinal regions of left and right ipsilateral PVs required manual electrogram reannotation more frequently than the other regions. The voltage map could identify the gap only in 19 instances (35%). Electrophysiological properties of the gaps (multiple gaps in the same ipsilateral PVs, conduction time, velocity, width, and length) did not differ between those needing and not needing manual electrogram reannotation. During the gap ablation, either the activation sequence alteration or elimination of PV potentials was observed using a circular catheter placed in the PV, suggesting that all the identified gaps were correct.Conclusion: This new electroanatomic mapping system visualized all the LA-PV gaps in patients undergoing a second AF ablation. [ABSTRACT FROM AUTHOR]

Polar cap arcs are often called sun-aligned arcs. Satellite observations reveal that polar cap arcs join together at the cusp and are actually cusp aligned. Strong ionospheric plasma velocity shears, thus field aligned currents, were associated with polar arcs and they were likely caused by Kelvin–Helmholtz waves around the low-latitude magnetopause under a northward IMF B z . The magnetic field lines around the magnetopause join together in the cusp region so are the field aligned currents and particle precipitation. This explains why polar arcs are cusp aligned. [ABSTRACT FROM AUTHOR]

On March 23, 2002, Cluster satellites recorded an event, which has been interpreted as reconnection, during an outward crossing near the dawn side cusp region in the Northern Hemisphere. The event showed a large perturbation in the magnetic normal component, inconsistent with a one-dimensional reconnection layer configuration, and causing a poor result in a minimum magnetic variance analysis. The utilization of the plasma velocity or electric field data significantly improves the boundary normal analyses. Through the comparison between observational data and local three-dimensional MHD simulations, it is demonstrated that this perturbation is likely an indication of a strong boundary modulation by a KH wave. The event is used to examine several established and new boundary normal analysis methods. [ABSTRACT FROM AUTHOR]

Background: Limited data exist on procedural and biophysical indicators of pulmonary vein (PV) isolation durability after the cryoballoon ablation of atrial fibrillation (AF).Objective: The aim of this study was to investigate the procedural and biophysical characteristics associated with late PV reconnection (PVR) and durable PV isolation (PVI) after cryoablation using the currently available second-generation cryoballoon.Methods: Data from 435 PVs targeted in 112 consecutive patients who underwent a repeat procedure 14 ± 3 months after an index cryoablation of AF were examined.Results: Altogether, 111 PVs (25.5%) in 71 patients (63.4%) demonstrated PVR, whereas 324 PVs (74.5%) exhibited PVI. The number and duration of cryoballoon applications did not differ between PVR and PVI. However, the time to PV isolation (time to effect) was considerably shorter (39.1 ± 11.7 seconds vs 67.6 ± 19.7 seconds; P < .001), the balloon temperature at time to effect was significantly warmer (-32.1°C ± 7.8°C vs -39.4°C ± 5.8°C; P < .001), the balloon nadir temperature was slightly cooler (-48.7°C ± 4.6°C vs -47.8°C ± 2.9°C; P = .034), and the total thaw time (56.5 ± 25.4 seconds vs 34.8 ± 9.1 seconds; P < .001) and interval thaw times at 0°C (iTT0; 14.8 ± 10.9 seconds vs 7.1 ± 2.0 seconds; P < .001) and 15°C (54.2 ± 25.4 seconds vs 33.3 ± 9.1 seconds; P < .001) were notably longer with PVI than with PVR. However, only a time to effect of ≤60 seconds and an iTT0 of ≥10 seconds emerged as significant predictors of PV isolation durability. Consequently, in a multivariate model, presence of both criteria predicted <1% and their mere absence ~75% likelihood of PVR.Conclusion: A time to effect of ≤60 seconds and an iTT0 of ≥10 seconds significantly predict PV isolation durability after the cryoballoon ablation of AF. If both criteria are met, the likelihood of PV reconnection may be exceedingly low. [ABSTRACT FROM AUTHOR]

We present a study of the impact of the December 7, 2003 fast forward interplanetary (IP) shock on the distant tail of the Earth׳s magnetosphere. Using the data from the several spacecraft located in the solar wind/magnetosheath upstream to the Earth, we monitor a propagation of the IP shock from the L1 point to the magnetosphere. A behavior of the far magnetotail is inferred from the Wind observations at X GSM ≈ − 230 R E . Shortly after the shock arrival, Wind crossed consequentially southern and northern lobes and observed a flux rope and the tailward fast plasma flow (≈780 km/s) within the plasmasheet. Moreover, a change of the solar wind V Z component across the shock creates a huge kink of the tail magnetosphere that propagates down the tail with the IP shock. [ABSTRACT FROM AUTHOR]

Abstract: A three-dimensional adaptive magnetohydrodynamic (MHD) model is used to investigate the energy flow from the solar wind to the magnetosphere in response to sudden turnings of the interplanetary magnetic field (IMF) on 5 June 1998. During this dynamic period, the size of magnetospheric cavity and the energy input fluctuated enormously. Due to the positive earth dipole tilt angle during the event, the distribution of energy transfer between northern and southern hemispheres of magnetopause is asymmetrical, with most energy transferred in the north hemisphere sunward of . The electromagnetic and mechanical energy inputs increase rapidly after the arrival of an interplanetary shock, while the electromagnetic energy rises much more slowly after IMF turns from north to south. With a nearly invariable component of IMF, under southward IMF the most electromagnetic energy is transferred near the plane anti-parallel to IMF clock angle, the most significant mechanical energy input occurs in the polar cusp of north hemisphere. In contrast, for northward IMF the electromagnetic energy is mostly transferred near the plane perpendicular to IMF clock angle, mechanical transferred energy occurs near equatorial plane of dayside magnetopause. Analyzing the distribution of the Poynting flux we show that the high-latitude reconnection causes different types of electromagnetic energy transfers into the magnetosphere during northward IMF especially with a large component. It is also shown that the traditional energy transfer parameters from solar wind conditions do not include any of residual or hysteresis effects; therefore sometimes they do not reflect the right response to the solar wind variations. [Copyright &y& Elsevier]

Background: Pulmonary vein (PV) isolation has become the mainstay acute procedural end point for paroxysmal atrial fibrillation (AF) ablation. Objective: To examine the incidence of conduction recovery in the PVs in patients without clinical recurrence of AF after paroxysmal AF ablation. Methods: From August 2008 to March 2011, 392 patients with drug-refractory PAF underwent catheter ablation in our center, a wide area circumferential ablation approach guided with a circular mapping catheter was performed with the intended endpoint of entrance block in all PVs. 276 (70.4%) of them were free from recurrence at one year follow-up, and 32 of them were enrolled to assess the incidence of PV reconnection. Forty-three patients with clinical recurrence after ablation were analyzed for comparison. The regions of gap were mapped and characterized in all of the reconnected PVs. Results: Among patients without recurrence, recovery of PV conduction was observed in 29 of 32 (90.6%) patients: 10/32 (31.2%) reconnection in 4 veins, 7/32 (21.9%) in 3 veins, 10/32 (31.2%) in 2 veins, and 2/32 (6.2%) in 1 vein. No anatomic propensity was seen because reconnection was evenly distributed throughout all veins (left superior pulmonary vein 21, left inferior pulmonary vein 20, right superior pulmonary vein 19, and right inferior pulmonary vein 23). When compared to patients with recurrence, no significant differences were seen in the proportion of patients with reconnection (P = 1.0) or in left atrium-PV intervals (73.4 ± 43.3 ms vs 61.9 ± 31.8 ms; P > .05). Conclusion: A high incidence of PV reconnection was similarly observed in patients with and without recurrence of AF, suggesting that sustained PV isolation may not be required for freedom from clinical recurrence of AF. [Copyright &y& Elsevier]

Background: Pulmonary vein isolation by cryoballoon ablation is an accepted method of treating atrial fibrillation. Little data exist regarding factors affecting late electrical reconnection of pulmonary veins following cryoballoon ablation. Objective: To investigate factors determining pulmonary vein reconnection in patients undergoing repeat catheter ablation for recurrent atrial fibrillation following cryoballoon ablation. Methods: Fifty-one consecutive patients undergoing repeat catheter ablation for recurrent atrial fibrillation following initial cryoballoon ablation underwent retrospective assessment of initial cryoablation characteristics, including balloon and vein sizes, venogram occlusion score, balloon freezing time from 0 to −30°C, nadir temperature, and balloon warming time from −30 to +15°C, recorded during the initial cryoballoon procedure. Results: Of 199 veins assessed, 91 had reconnected (1.8 per patient). Balloon warming time (odds ratio [OR] 3.21; 95% confidence interval [CI] 2.00–5.13; P < .0001), nadir temperature (OR 1.94; 95% CI 1.42–2.66; P < .0001), vein occlusion score (OR 1.74; 95% CI 1.29–2.34; P = .0003), and balloon freezing time (OR 1.58; 95% CI 1.03–2.42; P = .037) predicted pulmonary vein reconnection. On multivariate analysis, balloon warming time (OR 3.71; 95% CI 2.2–6.24; P ≤ .0001), pulmonary vein size (OR 1.63; 95% CI 1.08–2.43; P = .020), and vein occlusion score (OR 1.48; 95% CI 1.06–2.08; P = .021) remained statistically significant independent predictors of pulmonary vein reconnection. The receiver operating characteristic for the multivariate model yielded an area under the curve of 0.82. Conclusions: Balloon warming time, vein occlusion score, and pulmonary vein size predict pulmonary vein reconnection. Balloon warming time was the most important predictive factor, and the manipulation of balloon warming may be a novel therapeutic strategy for improving outcomes of cryoballoon ablation for atrial fibrillation. [Copyright &y& Elsevier]

Abstract: The whistler-mode waves and electron temperature anisotropy play a key role prior to and during magnetic reconnection. On August 21, 2002, the Cluster spacecrafts encountered a quasi-collisionless magnetic reconnection event when they crossed the plasma sheet. Prior to the southward turning of magnetospheric magnetic field and high speed ion flow, the whistler-mode waves and positive electron temperature anisotropy are simultaneously observed. Theoretic analysis shows that the electrons with positive temperature anisotropy can excite the whistler-mode waves via cyclotron resonances. Using the data of particles and magnetic field, we estimated the whistler-mode wave growth rate and the ratio of whistler-mode growth rate to wave frequency. They are 0.0016fce (Electron cyclotron frequency) and 0.0086fce , respectively. Therefore the whistler-mode waves can grow quickly in the current sheet. The combined observations of energetic electron beams and waves show that after the southward turning of magnetic field, energetic electrons in the reconnection process are accelerated by the whistler-mode waves. [Copyright &y& Elsevier]

Abstract: We review recent experience from the Cluster, Double Star, and THEMIS missions for lessons that apply to the upcoming Magnetospheric Multiscale Mission (MMS) being developed for launch in 2014. On global scales, simulation and statistical studies lead to mean configurations of dayside reconnection, implying specific relative alignments of the inflow magnetic fields and X-line, with implications for MMS operations designed to maximize the number of close encounters with the diffusion region. At intermediate MHD-to-ion scales, reconstruction of features created by one or two X-lines have developed to the point where data from a cluster of spacecraft can determine their temporal trends and the approximate three-dimensional X-line structure. Recent petascale particle-in-cell (PIC) simulations of reconnection encompass three spatial dimensions with excellent resolution, and make striking predictions of electron scale physics that creates complex interacting flux ropes under component reconnection. High time resolution measurements from MMS will determine the detailed electron scale kinetics embedded within the global and MHD–ion scale contexts. These developments will lead to the refinement of our three-dimensional multiscale picture of reconnection, yielding improved understanding of the global, MHD, and local physics controlling the onset or quenching, variability, and mean rate of reconnection. This in turn will enable improved predictability of the structural features created by transient reconnection, and their space weather consequences. [Copyright &y& Elsevier]

Abstract: So-called plasmoids are most fundamental signatures of geomagnetic substorms, and precise measurements of magnetic fields have been obtained by in situ satellite observations. Hence, in understanding substorm phenomena, it is essential to clarify the physical mechanism of plasmoid dynamics. The present paper studies on the basis of the spontaneous fast reconnection model how a large-scale plasmoid is generated and propagates in weakly sheared current sheets. It is demonstrated that the basic structure and dynamics of the plasmoid, generated by the fast reconnection, are both qualitatively and quantitatively in good agreement with actual satellite observations. In particular, magnetic field lines inside the generated plasmoid deviate from a helical geometry. [Copyright &y& Elsevier]

Abstract: We study the dependence of Mercury''s magnetospheric magnetic field structure on the interplanetary magnetic field (IMF). Special attention is paid to the case of radial IMF. Mercury is the smallest planet in the solar system and it does not have a substantial atmosphere or ionosphere. Mercury is the closest planet to the Sun, and it possesses a week intrinsic magnetic field. Due to these circumstances, IMF plays a major role in the hermean magnetospheric dynamics. Using a paraboloidal model of Mercury''s magnetosphere, we study the magnetospheric magnetic field topology for different orientations of IMF including examples representative of the first MESSENGER''s flyby. Variations in IMF lead to variations in the Mercury''s magnetospheric magnetic field structure, which in turn, lead to changes in the distribution of open and closed magnetic field lines. Comparison with the much better investigated Earth''s magnetosphere is fulfilled for clarifying the physical processes (mainly reconnection) existent in the hermean magnetosphere. We also consider the cases when MESENGER, being the Mercury''s orbiter, observed flux transfer events (FTEs) in the hermean magnetosphere. When the radial IMF component (B IMFx) is significant, which is character to the Mercury, the quasi-neutral line is placed in one of the cusps (depending on the sign of B IMFx). The FTE generation at Mercury can be connected with this line, similarly to the case of southward IMF at Earth, when FTEs arise at the dayside magnetopause at the quasi-neutral line. We show examples of observations supporting this result for Mercury. [Copyright &y& Elsevier]

Abstract: Magnetospheric substorms manifest a fundamental disturbance in geospace. Understanding of substorm progression is essential for solar terrestrial physics and space weather research. The auroral streamer and the bursty bulk flows (BBFs) were simultaneously observed by the IMAGE/WIC and the Cluster in the midtail (X∼−16R E ), whose footprint was near the auroral streamer, respectively, during a substorm on September 14, 2004. The auroral poleward boundaries (APBs) are 2∼3° MLAT lower than the open–closed field line boundaries (OCBs) during the growth phase. After the expansion onset, streamer elongated poleward, and the location of APBs became coincident with OCBs. These observations are consistent with the scenario that substorm activations start from plasma sheet reconnection of closed field lines during growth phase; in the expansion phase the open field line in the lobes are involved in reconnection in tail. [Copyright &y& Elsevier]

Abstract: The large scale dynamics of the cusp ionosphere is directly controlled by the solar wind and the orientation of the interplanetary magnetic field. The IMF BY controlled east–west movement of the poleward moving forms (PMAFs), separating from the cusp, is consistent with the magnetic tension pull of newly opened flux, which is a key feature tying the auroral phenomenon of PMAFs to flux transfer events (FTEs) at the magnetopause. The central region of an FTE is a mesoscale flow channel, bounded by a pair of Birkeland current sheets on each flank. Systematic observations by EISCAT Svalbard Radar, meridian scanning photometers and all-sky imagers have provided us further insight into key processes of the cusp ionosphere such as how FTEs/PMAFs control ion upflow events, and how transient magnetopause reconnection processes segment a stream of high density solar EUV plasma into polar cap patches at the polar cap boundary. We have found a close causal relationship between formation of plasma patches and onset of scintillation by a previously unrecognized process. We have discovered a new category of flow channels, reversed flow channel events (RFEs) that may appear related to a signature of Birkeland currents arcs, and may be signature of the MI-coupling/inverted V rather than mapping directly to the magnetopause. This review paper concentrates on a niche of cusp studies made by high-resolution radar and optical measurements. [Copyright &y& Elsevier]

Abstract: We present results from a 2.5 dimensional hybrid code simulation for the evolution of flux transfer events (FTEs) during intervals of due southward interplanetary magnetic field (IMF) orientation. The structures invariably form between pairs of reconnection lines, often remaining nearly stationary on the subsolar magnetopause before their motion begins. Although a few structures move sunward, ultimately coalescing with others, most eventually accelerate antisunward, reaching velocities many times greater than the sound speed in the magnetosheath but only about one Alfvén speed greater than the ambient magnetosheath flow. At these velocities, slow mode wakes (but not shocks) marked by density enhancements and magnetic field strength decreases extend outward from the structures into the magnetosheath. Upon encountering the cusps, the structures decelerate, undergo reconnection, and are destroyed. [Copyright &y& Elsevier]

Abstract: In this paper, we study multiwavelength observations of an M6.4 flare in Active Region NOAA 11045 on 7 February 2010. The space- and ground-based observations from STEREO, SoHO/MDI, EIT, and Nobeyama Radioheliograph were used for the study. This active region rapidly appeared at the north-eastern limb with an unusual emergence of a magnetic field. We find a unique observational signature of the magnetic field configuration at the flare site. Our observations show a change from dipolar to quadrapolar topology. This change in the magnetic field configuration results in its complexity and a build-up of the flare energy. We did not find any signature of magnetic flux cancellation during this process. We interpret the change in the magnetic field configuration as a consequence of the flux emergence and photospheric flows that have opposite vortices around the pair of opposite polarity spots. The negative-polarity spot rotating counterclockwise breaks the positive-polarity spot into two parts. The STEREO-A 195Å and STEREO-B 171Å coronal images during the flare reveal that a twisted flux tube expands and erupts resulting in a coronal mass ejection (CME). The formation of co-spatial bipolar radio contours at the same location also reveals the ongoing reconnection process above the flare site and thus the acceleration of non-thermal particles. The reconnection may also be responsible for the detachment of a ring-shaped twisted flux tube that further causes a CME eruption with a maximum speed of 446km/s in the outer corona. [Copyright &y& Elsevier]

Abstract: Recently, automated segmentation of retinal vessels in optic fundus images has been an important focus of much research. In this paper, we propose a multi-scale method to segment retinal vessels based on a weighted two-dimensional (2D) medialness function. The results of the medialness function are first multiplied by the eigenvalues of the Hessian matrix. Next, centerlines of vessels are extracted using noise reduction and reconnection procedures. Finally, vessel radii are estimated and retinal vessels are segmented. The proposed method is evaluated and compared with several recent methods using images from the DRIVE and STARE databases. [Copyright &y& Elsevier]

Abstract: A new type of polar cap aurora, dawn–dusk aligned polar cap aurora (DDAPCA), was detected during the exceptionally intense January 21, 2005 substorm (AE max=3504nT). The DDAPCA was located at very high latitude (>85°MLAT) in the polar cap region. As the interplanetary magnetic field (IMF) GSM By component rotated from a positive to a negative value, the DDAPCA tilt angle relative to the dawn–dusk direction rotated anticlockwise and reached ∼45°. It is speculated that the DDAPCA arises from the formation of an X-line in the distant (>80R E) tail due to polar cap magnetic field reconnection under unusually high solar wind compression conditions. [Copyright &y& Elsevier]

Abstract: During the last decade, a debate arose regarding the timing and pattern of the last reconnection of the Black Sea “Lake” with the global ocean. On a geochemical basis, the radiocarbon age of Black Sea “Lake” surface water, during the time of reconnection, was determined to be ∼8400 14C a. BP. Despite the potential bias induced by the hard water effect in lakes, the reconnection age was calibrated without any reservoir age correction, which led to an estimate of ∼9400 cal a. BP. Since knowledge for the actual calendar age has important hydrologic implications that would provide new insights regarding the mechanism of reconnection, determining the actual calendar age for the last reconnection remains important. Based upon modeling experiments and micropaleontological reconstructions, the Black Sea “Lake” reconnection occurred in two steps, as follows: 1) Initial Marine Inflow (IMI) followed by 2) a period of increasing basin salinity that led to the Disappearance of Lacustrine Species (DLS). In order to better define the actual calendar age for the last reconnection, a review of the sedimentary expressions of the IMI and DLS boundaries was performed in order to correlate them throughout the Black Sea sedimentary environments. This correlation reconciles the apparent inconsistency in the published radiocarbon dataset, and provides the atmospheric radiocarbon age of the last reconnection, which represents the reference for reservoir age calculations and which can be directly calibrated. We determine reservoir ages for the water column, as well as the reconnection calendar age to be 9000 cal a. BP. At the reconnection with the global ocean, Black Sea “Lake” reservoir ages were non-negligible and water-depth-dependent, consistent with a weak water column stratification during the Early Holocene. The calibrated age of Initial Marine Inflow (9000 cal a. BP) implies that the former Bosphorus sill was shallower by ∼10 m than is commonly assumed in the literature. Compared to the sedimentary context of the Sakarya coastal plain, this result suggests that the level of the isolated Black Sea was below the former Bosphorus sill depth at the time of the last reconnection. Furthermore, a lag of ∼900 yr between Initial Marine Inflow and the Disappearance of Lacustrine Species indicates that approximately ten centuries were needed to establish the currently observed two-way flow exchange with the global ocean. [Copyright &y& Elsevier]

Abstract: The ACB search-coil magnetometer for Cross-Scale will measure three components of the AC magnetic field up to 4kHz, and one component up to 100kHz. Turbulent and coherent magnetic field fluctuations in that frequency range play an important role in the acceleration, scattering, and thermalisation of particles. ACB will, together with the other instruments of the Cross-Scale wave consortium, allow to address the key science objectives associated with plasma waves. Here, we list some of the important issues, based on the experience drawn from Cluster, and describe the instrument. [Copyright &y& Elsevier]

Abstract: The properties of plasmas (in space) are fundamentally governed by both ‘cross-scale’ coupling and comparative temporal behaviour operating over the micro-, meso-, and (MHD-) fluid regimes: for example, under conditions of turbulence, during magnetic reconnection and in shocks and other plasma boundaries. These themes map to a number of related and overlapping, phenomena, where known phenomena play different roles in each theme. Detailed understanding of fundamental plasma processes therefore requires analysis of both theoretical models (to distinguish the collisionless from the collisional regimes) and multi-scale measurements (suitable to address issues of stationarity). In particular, the investigation of phenomena requires analysis techniques which can distinguish and quantify temporal behaviour and the multi-scale spatial behaviour. The analysis of existing, multi-point data sets has led to a number of data co-ordination methods, such as the four spacecraft analysis tools developed for cluster, and we consider examples here. Advanced analysis concepts may be investigated with suitable considerations of measurement quality:adequate sampling of phenomena (for example, to extract the necessary information on the mechanisms operating) requires suitable spacecraft configurations and directly relates to the measurement quality achievable. A particular issue is how to resolve temporal behaviour across the spatial regimes, so that the data set is suitably coordinated. With the addition of theoretical modelling (in the context of particular phenomena) both the space and laboratory plasma regimes may be compared and we give an example of nonlinear wave coupling across spatial scales in this context. [Copyright &y& Elsevier]

Abstract: We present a THEMIS study of a dipolarization front associated with a bursty bulk flow (BBF) that was observed in the central plasma sheet sequentially at X=−20.1, −16.7, and −11.0R E . Simultaneously, the THEMIS ground network observed the formation of a north–south auroral form and intensification of westward auroral zone currents. Timing of the signatures in space suggests earthward propagation of the front at a velocity of 300km/s. Spatial profiles of current and electron density on the front reveal a spatial scale of 500km, comparable to an ion inertial length and an ion thermal gyroradius. This kinetic-scale structure traveled a macroscale distance of 10R E in about 4min without loss of coherence. The dipolarization front, therefore, is an example of space plasma cross-scale coupling. THEMIS observations at different geocentric distances are similar to recent particle-in-cell simulations demonstrating the appearance of dipolarization fronts on the leading edge of plasma fast flows in the vicinity of a reconnection site. Dipolarization fronts, therefore, may be interpreted as remote signatures of transient reconnection. [Copyright &y& Elsevier]

Abstract: By analyzing trajectories of solid hydrogen tracers in superfluid 4He, we identify tens of thousands of individual reconnection events between quantized vortices. We characterize the dynamics by the minimum separation distance between the two reconnecting vortices both before and after the events. Applying dimensional arguments, this separation has been predicted to behave asymptotically as , where is the quantum of circulation. The major finding of the experiments and their analysis is strong support for this asymptotic form with as the dominant controlling feature, although there are significant event to event fluctuations. At the three-parameter level the dynamics may be about equally well-fit by two modified expressions: (a) an arbitrary power-law expression of the form and (b) a correction-factor expression . The measured frequency distribution of is peaked at the predicted value , although the half-height values are and 0.80 and there is marked variation in all fitted quantities. Accepting (b) the amplitude has mean values of and half height values of 0.8 and 1.6 while the distribution is peaked close to with a half-height range of −0.9 s−1 to 1.5 s−1. In light of possible physical interpretations we regard the correction-factor expression (b), which attributes the observed deviations from the predicted asymptotic form to fluctuations in the local environment and in boundary conditions, as best describing our experimental data. The observed dynamics appear statistically time-reversible, which suggests that an effective equilibrium has been established in quantum turbulence on the time scales (≤0.25 s) investigated. We discuss the impact of reconnection on velocity statistics in quantum turbulence and, as regards classical turbulence, we argue that forms analogous to (b) could well provide an alternative interpretation of the observed deviations from Kolmogorov scaling exponents of the longitudinal structure functions. [Copyright &y& Elsevier]

Abstract: This paper focuses on a particular group of food commodities, associated with the wider turn to ‘alternative food networks’, that are described as ‘naturally embedded food products’ (NEFPs). These are commodities (specifically meats and cheeses) that utilise grassland biodiversity as an input into production to positively influence, in various ways, the final qualities of the commodity. Building on the geographical literature on commodity circuits and analysing data derived from NEFP promotional materials and focus groups with urban and rural residents in the UK, the paper interrogates the geographical knowledges that are deployed by producers in the promotion of NEFPs and how these knowledges are accommodated and contested by consumers as they bring their own geographical knowledges to the interpretation of these commodities. The paper undertakes this task in order to problematise the extent to which alternative food networks in general and NEFPs in particular are bringing about a reconnection of producers and consumers and, concomitantly, a defetishisation of food, as is claimed for them by many of their policy and academic proponents. In the process the paper reveals how the food commodities associated with alternative food networks entail the creation of new and rival fetishes paradoxically as a result of efforts to ‘thicken connections’ between the production and consumption of food. [Copyright &y& Elsevier]

Abstract: Recent Cluster observations have strongly supported the existence of meso-scale structure in the magnetotail current sheet. In our study, a magnetohydrodynamic simulation event study exhibited current sheet behavior comparable to that seen in the Cluster observations. Geotail and DoubleStar observations also show that the simulation is providing a realistic representation of the magnetosphere during the period of interest; that is, when the current sheet evidently becomes bifurcated. The magnetohydrodynamic simulation allows us to place the local observations into a global contest. It shows that the observations can be explained in terms of localized reconnection tailward of the Cluster location and the formation of a flux rope nearby. The simulation also features wave-like structure across the current sheet. [Copyright &y& Elsevier]

Abstract: This paper reviews quantitative analysis results of the energy transfer and dissipation processes in the GUMICS-4 global MHD simulation. Reconnection power dissipating magnetic energy, dynamo power transferring energy from plasma to the field, and energy flux transport across the magnetopause surface are all examined separately and shown to yield consistent results. This is used to argue that magnetic reconnection is the process controlling the energy transfer, even though it is not localized near the reconnection line. The most important factors controlling the reconnection efficiency are the interplanetary magnetic field (IMF) orientation and the solar wind speed, while the IMF magnitude and solar wind density play a lesser role. During northward IMF, the reconnection efficiency is larger for high speed and low IMF than for low speed and high IMF magnitude, even though the solar wind electric field in both cases is the same. Moreover, increasing pressure by increasing density has a different effect from equal increase of pressure by increasing the solar wind speed. Comparison with statistical observational results shows that the simulation results are in qualitative agreement with the observations, which significantly increases our confidence in interpreting the simulation results. [Copyright &y& Elsevier]

Abstract: We address the problem of interacting relativistic current sheets in self-consistent kinetic plasma simulations within the framework of the Particle-In-Cell model. The interaction is enforced in head-on collisions of up to 10 current sheets at relativistic bulk speeds. The simulations are motivated by the general problem of Poynting flux dissipation in ‘striped wind’ configurations presumably governing the relativistic outflows pervasive in pulsar winds and gamma-ray bursts. We identify the generation of non-thermal particles and formation of a stable power-law shape in the particle energy distributions f(γ) dγ ∝ γ −s dγ. In 1D, a spectral index s ∼2 is observed and attributed to a stochastic Fermi-type acceleration mechanism. In 2D, the generic index of s ∼3–4 is retained as in previous simulations of individual current sheets. Whereas in 2D the high energy cut-off is constrained by the limited dissipation of magnetic energy, in 1D the process converts the bulk motion of current sheets towards directed particle momentum of an exclusive class of non-thermal particles. [Copyright &y& Elsevier]

Abstract: The analysis of simultaneous observations of 128 cases of high-latitude magnetic impulse events (MIEs), as well as geomagnetic pulsations in the Pc1–2 band observed in the area of the dayside cusp, was carried out. We investigated magnetograms from the Mirny Observatory, Antarctica. As a result of the examination, three groups of impulses were identified: (1) impulses accompanied by impulsive bursts of intervals of pulsations with rising periods (IPRPs)-type geomagnetic pulsations—16% of all events, (2) impulses accompanied by impulsive bursts of the Pi1B type (bursts of irregular magnetic pulsations)—48% of all events, and (3) impulses which were not accompanied by geomagnetic pulsations within a high-frequency band—36% of all events. It was found that the maximum frequency of occurrence of the impulses accompanied by impulsive bursts of the IPRP and Pi1B types was observed between 1200 and 1300MLT. The events of the first two groups were observed predominantly when Bz>0. It was shown that the filling frequency of impulsive bursts that accompany the occurrence of impulses depends on the amplitude of the bursts. The maximum frequency of the occurrence of impulses which were not accompanied by impulsive bursts is between 1000 and 1100MLT. The events of the third group were observed predominantly when Bz<0. In most cases, the occurrence of impulsive bursts coincided with the leading edge of the MIE. It is supposed that the MIE generation is stimulated by intensification of the plasma turbulence level at the dayside magnetopause in consequence of modulation instability development or reconnection processes. [Copyright &y& Elsevier]

Abstract: This paper presents both rigorous results and physical theory on the breakdown of magnetic flux conservation for ideal plasmas by nonlinear effects. Our analysis is based upon an effective equation for magnetohydrodynamic (MHD) modes at length scales , with smaller scales eliminated, as in renormalization-group methodology. We prove that flux conservation can be violated at an instant of time for an arbitrarily small length scale , and in the absence of any nonideality, but only if at least one of three necessary conditions is satisfied. These conditions are (i) nonrectifiability of advected loops, (ii) unbounded velocity or magnetic fields, (iii) singular current sheets and vortex sheets that both exist and intersect in sets of large enough dimension. This result gives analytical support to and rigorous constraints on theories of fast turbulent reconnection. Mathematically, our theorem is analogous to Onsager’s result on energy dissipation anomaly in hydrodynamic turbulence. As a physical phenomenon, the breakdown of magnetic flux conservation in ideal MHD is similar to the decay of magnetic flux through a narrow superconducting ring, by phase-slip of quantized flux lines. The effect should be observable both in numerical MHD simulations and in laboratory plasma experiments at moderately high magnetic Reynolds numbers. [Copyright &y& Elsevier]

Abstract: The scant data from the historic Mariner-10 flybys indicate that the Hermean and terrestrial magnetospheres have many similarities. However, Mercury’s differences, e.g., the absence of an ionosphere, high sodium content, small dimension, and the stronger forcing by the solar wind, make it likely that processes of lesser importance at Earth play a more major role at Mercury. In addition, the proximity of Mercury in time and space to the onset of solar events, places the magnetosphere in a heretofore unexplored environment. [Copyright &y& Elsevier]

Abstract: This review summarizes the magnetotail current sheet observations by the Cluster spacecraft during July–October 2001. Due to four-point measurements and the tetrahedron configuration of the spacecraft constellation we are able to separate spatial and temporal variations and to estimate gradients and characteristic scales of structures in the current sheet. We discuss the following topics: (i) magnetotail current sheet flapping, (ii) the structure of the current sheet, and (iii) magnetotail reconnection. [Copyright &y& Elsevier]

Abstract: The past half century has been characterized by the birth of space plasma physics and its rise to maturity which has led into a certain mood of satisfaction and partial saturation with its achievements. Indeed, on the global scale our knowledge about the magnetosphere, the solar wind from the Sun out to its boundaries, even of the conditions on the surface and in the atmosphere of the Sun and the Sun’s interior has to a high degree become complete. The degree of completion is indeed such that it allows predicting up to a certain precision their behavior. New names like solar seismology, solar meteorology, and space weather have been coined indicating the transition of some of the sub-field of Space Plasma Physics into the domain of an industry of monitoring and predicting in the interest of the needs of a general society. This is an entirely healthy evolution of a scientific field that is on the path of completion. Still there is a large number of questions which should and can hopefully be answered by space plasma theory. Some of them will be listed here in view of what has been achieved and in which direction future theory could proceed in order to contribute to their resolution when addressing the already operating and the new and upcoming space missions like Cluster, the planned Magnetospheric Multi-Scale mission MMS and others, respectively, most of which are designed to become multi-spacecraft enterprizes and also in view of the new theoretical and computational techniques and methods that have been developed during the past decades. These directions reach from the detailed understanding of the processes in the solar atmosphere and solar wind through the detailed physics of the formation of collisionless shocks, magnetosheaths and turbulence, the microphysics of reconnection and particle acceleration, and the substorm mechanism to the detailed understanding of planetary magnetospheres, the outer heliosphere with its heliospheric termination shock, heliosheath and boundary layer. All this research though already in flow has by far not been completed yet. It requires new efforts as it implies resolution of the smallest though still non-atomic scales, but it has high implications for the understanding of the processes in space plasma and, in extension, of processes in the remote astrophysical systems which can be understood only by observation of their radiation in all wavebands. [Copyright &y& Elsevier]

Abstract: We present and discuss observations of a region in the high-latitude near-Earth outer magnetosphere when over a distance of 9R E – from GSM [0.83R E, 1.6R E, 8.5R E] to [−0.957R E, 10.175R E, 12.738R E] – Interball-1 observed multiple alternative changes in plasma characteristics: hot plasma sheet population is replaced by a region of mixed magnetosheath – plasma sheet population with the presence of ionospheric ions and vice versa. In the ‘mixed’ region, both ion populations were nearly stagnant, their velocity rarely exceeded 50km/s and plasma-sheet electrons were absent. Most of the time interplanetary magnetic field (IMF) clock angle was less than 90°, rotating to more than 270° at the end of the interval, IMF B x being positive and dominating. A flux transfer event was registered near the magnetopause. Plasma characteristics suggest that observations took place at the high-latitude boundary of the near-Earth plasma sheet on closed field lines. We suggest that the mixed regions are formed on filed lines first reconnected to the magnetosheath magnetic field, then draped and convected duskward and tailward and secondary reconnected and closed. [Copyright &y& Elsevier]

Abstract: We apply a theoretical model to describe the behavior of nightside flux transfer events (NFTEs) measured by Cluster satellites in the Earth magnetotail. Based on the Cagniard–deHoop method we calculate the magnetic field and plasma flow time series observed by a satellite. Our aim is to solve an inverse problem to obtain the reconnection rate from the measured plasma data. The ill-posed inverse problem is treated with the method of regularization, since the solution of the Cagniard–deHoop method is given in the form of a convolution integral, which is well known in the theory of inverse problems. This method is applied to Cluster measurements from September 8th, 2002, where a series of Earthward propagating 1-min scale magnetic field and plasma flow variations were observed outside of the plasma sheet, which are consistent with the theoretical picture of NFTEs. Estimations of the satellite position with respect to the reconnection site and of the Alfvén velocity are made because they are necessary parameters for the model. The reconnection rate is found to be in the range of 1–2mV/m and the reconnection site at about 29R e tailwards. [Copyright &y& Elsevier]

Abstract: In understanding the structure of an MHD-scale Kelvin–Helmholtz (KH) vortex, magnetic reconnection within the vortex must not be neglected. Here, we have performed two-dimensional two-fluid simulations including finite electron inertial effects to investigate this issue. An MHD-scale velocity shear is set up and evolution of MHD-scale KH mode is followed with in-plane magnetic component taken into account. In this study, we focus on three basic cases with different initial magnetic configuration. In all cases, when the Alfven Mach number of the shear is strong enough, magnetic reconnection occurs spontaneously within the vortex by the electron inertial effects. The critical Alfven Mach number for the reconnection is found to depend on the initial magnetic configuration. [Copyright &y& Elsevier]

Abstract: On 7 December 2000, Cluster made an extended outbound radial traversal of the duskside magnetopause boundary layer. The long duration of the crossing, during which Cluster spent several hours within 2R E of the nominal magnetopause, allows us to deconvolve the structure of this boundary layer in its dependence on interplanetary parameters. We present evidence that as the interplanetary magnetic field (IMF) changed in discontinuous jumps from southward to northward, the magnetic topology of the boundary layer evolved from open to closed. Reconnection signatures, including enhanced flows observed locally at Cluster and ion energy dispersion signatures observed by FAST near Cluster’s magnetic footpoint, appeared while the IMF was southward. When the IMF turned nearly due northward, Cluster observed 75-s (Pc 4) oscillations which we attribute to the Kelvin–Helmholtz instability. [Copyright &y& Elsevier]

Abstract: The influence of the Hall-term on the width of the magnetic islands of the tearing-mode is examined. We applied the center manifold (CMF) theory to a magnetohydrodynamic (MHD)-system. The MHD-system was chosen to be incompressible and includes in addition to viscosity the Hall-term in Ohm’s law. For certain values of physical parameters the corresponding center manifold is two-dimensional and therefore the original partial differential equations could be reduced to a two-dimensional system of ordinary ones. This amplitude equations exhibit a pitchfork-bifurcation which corresponds to the occurrence of the tearing-mode. Eigenvalue-problems and linear equations due to the center manifold reduction were solved numerically with the Arpack++-library. An important result of this analysis is the growth of the tearing mode island width by increasing the Hall-parameter, a feature which has been observed in recent numerical simulations of collisionless reconnection. [Copyright &y& Elsevier]

We investigated the structure of magnetic field lines in a tokamak with reversed magnetic shear and non-symmetric perturbations by means of analytically derived area-preserving non-twist Poincaré maps. The maps are used to study magnetic island dimerization and the formation of a transport barrier in the chaotic layer of field lines. [Copyright &y& Elsevier]

The Mariner 10 observations of Mercury''s miniature magnetosphere collected during its close encounters in 1974 and 1975 are reviewed. Subsequent data analysis, re-interpretation and theoretical modeling, often influenced by new results obtained regarding the Earth''s magnetosphere, have greatly expanded our impressions of the structure and dynamics of this small magnetosphere. Of special interest are the Earth-based telescopic images of this planet''s tenuous atmosphere that show great variability on time scales of tens of hours to days. Our understanding of the implied close linkage between the sputtering of neutrals into the atmosphere due to solar wind and magnetospheric ions impacting the regolith and the resultant mass loading of the magnetosphere by heavy planetary ions is quite limited due to the dearth of experimental data. However, the influence of heavy ions of planetary origin (O+, Na+, K+, Ca+ and others as yet undetected) on such basic magnetospheric processes as wave propagation, convection, and reconnection remain to be discovered by future missions. The electrodynamic aspects of the coupling between the solar wind, magnetosphere and planet are also very poorly known due to the limited nature of the measurements returned by Mariner 10 and our lack of experience with a magnetosphere that is rooted in a regolith as opposed to an ionosphere. The review concludes with a brief summary of major unsolved questions concerning this very small, yet potentially complex magnetosphere. [Copyright &y& Elsevier]

The dawn–dusk magnetic field component (Bz) in the plasmoid resulting of magnetic reconnections have been observed GEOTAIL satellite. We have studied the effects by Bz component in the reconnection in geomagnetotail. This paper present the results of computer simulation about them. Our recent simulation apply the spontaneous fast reconnection model to the three-dimensional (3-D) plasmoid dynamics. Previous our original 3-D computational region (the first quadrant) is extended to the second quadrant and axis symmetry boundary conditions are used. Then, various initial values of dawn–dusk magnetic field component Bz can be possibly assumed. As a result in all our simulation cases: (1) a large-scale plasmoid evolves, and (2) it propagates down to the geomagnetic tail, (3) slow shocks and finite amplitude intermediate waves simultaneously stand along the resulting plasmoid boundary layer. We also found that in the plasmoid where north–south magnetic field component (By) changes its sign, Bz also has a considerably big value, Which is consistent with the satellite observation result. We propose that the spontaneous fast reconnection mechanism could be most applicable to substorms. [Copyright &y& Elsevier]

Supersonic and subsonic expansion acceleration mechanisms associated with spontaneous fast magnetic reconnection process are compared by two-dimensional magnetohydrodynamic (MHD) simulations and test fluid (non-charged) particle simulations. When the Petschek reconnection process is steadily established, the reconnection jet generated by a pair of slow shocks becomes either supersonic (Case 1) or subsonic (Case 2), depending on the upstream plasma condition. For Case 1, the jet generated by the slow shocks can be further accelerated by the adiabatic supersonic expansion process. Finally, the jet encounters a fast shock in front of the plasmoid. For Case 2, the jet generated by slow shocks can be further accelerated by the adiabatic subsonic expansion process. The acceleration of Case 1 is stronger than that of Case 2. In Case 2, a fast shock is not formed. In both cases, it is important that the propagation of the plasmoid is driven by slow shocks formed around the plasmoid itself, rather than the reconnection jet. [Copyright &y& Elsevier]

The solar wind is a magnetized flowing plasma that intersects the Earth''s magnetosphere at a velocity much greater than that of the compressional fast mode wave that is required to deflect that flow. A bow shock forms that alters the properties of the plasma and slows the flow, enabling continued evolution of the properties of the flow on route to its intersection with the magnetopause. Thus the plasma conditions at the magnetopause can be quite unlike those in the solar wind. The boundary between this “magnetosheath” plasma and the magnetospheric plasma is many gyroradii thick and is surrounded by several boundary layers. A very important process occurring at the magnetopause is reconnection whereby there is a topological change in magnetic flux lines so that field lines can connect the solar wind plasma to the terrestrial plasma, enabling the two to mix. This connection has important consequences for momentum transfer from the solar wind to the magnetosphere. The initiation of reconnection appears to be at locations where the magnetic fields on either side of the magnetopause are antiparallel. This condition is equivalent to there being no guide field in the reconnection region, so at the reconnection point there is truly a magnetic neutral or null point. Lastly reconnection can be spatially and temporally varying, causing the region of the magnetopause to be quite dynamic. [Copyright &y& Elsevier]

We describe how a local plasma structure can be changed by a transverse shear flow using numerical simulation to investigate the disturbance process near the magnetopause. The results show that magnetic field lines are bent by transverse shear flow disturbance near the current sheet region. There are multiple bipolar structures of the normal magnetic field in the numerical simulation. We term this new feature as K-point magnetic reconnection, realistic for discussing space observations. [Copyright &y& Elsevier]

Interaction of exoplanet with a host star in the triple star system is considered. Besides reconnection of the stellar and planetary magnetic fields (if they exist), the specific interaction of exoplanet with three stars leads to increased impact on the planetary environment and the host star astrosphere. Encounters with different kinds of corotation interaction regions from the stellar winds of the distant stars in the triple system affect the host-star's astrosphere. Just out of the astrosphere's boundary, dynamo can act for the rapidly rotating magnetic host star, because corotation, transferred along open field lines, brakes down there with possible generation of magnetic field. When several stars exist in the system, the effect of their CMEs and flare activities can summarize. Rotational synchronization between the host star and close-in exoplanet can intensify the coronal activity of the star. All these effects could lead to possible increase of magnetic field at the boundary of the host star astrosphere and inside it, which, consequently, will result in the enhanced cyclotron radio emission from such systems. • Triple star system with exoplanet can be a source of cyclotron radio emission. • Specific features of interaction between the distant stars' winds are CIRs and MIRs. • At the boundary of rapidly rotating magnetic star astrosphere the dynamo can act. [ABSTRACT FROM AUTHOR]

A variety of magnetospheric plasma populations have been proposed to impact solar wind-magnetosphere coupling. These magnetospheric populations could mass load the dayside magnetopause and include the plasmaspheric plume, plasma cloak, ion plasma sheet, and dayside ion outflow. Each has different densities, ion composition, and spatial/temporal occurrences at the dayside magnetopause which may coupling in different ways. These properties are reviewed as well as proposed mechanisms for impacting wave formation and magnetic reconnection. Broader discussion on control of solar wind-magnetosphere coupling governed by through local boundary physics or through the driving of the solar wind (local versus global control) is also considered. • Cold dense plasma can populate the outer magnetosphere under a variety of conditions. • Cold plasma originating from the inner-magnetosphere can dominate the mass density at the magnetopause. • Cold plasma can impact modes of solar wind-magnetosphere coupling such as boundary waves and magnetic reconnection. [ABSTRACT FROM AUTHOR]