Asymmetric Magnetosphere Deformation Driven by Hot Flow Anomaly(ies)

We present a case study of a large deformation of the magnetopause on November 26, 2008. The investigation is based on observations of five THEMIS spacecraft located at the dawn flank in the magnetosphere and magnetosheath, on Cluster measurements at the dusk magnetosheath, and is supported by ACE solar wind monitoring. The main revelation of our study is that the interaction of the IMF discontinuity with the bow shock creates either one very elongated hot flow anomaly (HFA) or a pair of them that is (are) simultaneously observed at both flanks. Whereas the dusk HFA is weak and does not cause observable deformation of the magnetopause, the pressure variations connected with the dawn HFA lead to a magnetopause displacement by approx. = 5 R(sub E) outward from its nominal position. This is followed by a rapid inward motion of the magnetopause approx. = 4 R(sub E) inward with respect to the model location. The surface deformation is so large that the outermost THEMIS spacecraft was in the magnetosphere, whereas the spacecraft located 9 R(sub E) inbound entered into the magnetosheath at the same time. The whole event lasted about 5 minutes

Long-term variations in solar wind parameters, magnetopause location, and geomagnetic activity over the last five solar cycles

We use both solar wind observations and empirical magnetopause models to reconstruct time series of the magnetopause standoff distance for nearly five solar cycles. Since the average annual interplanetary magnetic field (IMF) Bz is about zero, and the annual IMF cone angle varies between 54.0° and 61.2°, the magnetopause standoff distance on this time scale depends mostly on the solar wind dynamic pressure. The annual IMF magnitude well correlates with the sunspot number (SSN) with a zero time lag, while the annual solar wind dynamic pressure (Pdyn) correlates reasonably well with the SSN but with 3 years time lag. At the same time, we find an anticorrelation between Pdyn and SSN in cycles 20–21 and a correlation in cycles 22–24 with 2 years time lag. Both the annual solar wind density and velocity well correlate with the dynamic pressure, but the correlation coefficient is higher for density than for velocity. The 11‐year solar cycles in the dynamic pressure variations are superimposed by an increasing trend before 1991 and a decreasing trend between 1991 and 2009. The average annual solar wind dynamic pressure decreases by a factor of three from 1991 to 2009. Correspondingly, the predicted standoff distance in Lin et al.’s (2010) magnetopause model increases from 9.7 RE in 1991 to 11.6 RE in 2009. The annual SSN, IMF magnitude and magnetospheric geomagnetic activity indices display the same trends as the dynamic pressure. We calculate extreme solar wind parameters and magnetopause standoff distance in each year using daily values and find that both extremely small and large standoff distances during a solar cycle preferably occur at solar maximum r0061ther than at solar minimum

Super fast plasma streams as drivers of transient and anomalous magnetospheric dynamics

Abstract. We present multi spacecraft measurements in the magnetosheath (MSH) and in the solar wind (SW) by Interball, Cluster and Polar, demonstrating that coherent structures with magnetosonic Mach number up to 3 – Supermagnetosonic Plasma Streams (SPS) – generate transient and anomalous boundary dynamics, which may cause substantial displacements of the magnetospheric boundaries and the riddling of peripheral boundary layers. In this regard, for the first time, we describe a direct plasma penetration into the flank boundary layers, which is a candidate for being the dominant transport mechanism for disturbed MSH periods. Typically SPS's have a ram pressure exceeding by several times that of the SW and lead to long-range correlations between processes at the bow shock (BS) and at the magnetopause (MP) on one side and between MSH and MP boundary layers on the other side. We demonstrate that SPS's can be observed both near the BS and near the MP and argue that they are often triggered by hot flow anomalies (HFA), which represent local obstacles to the SW flow and can induce the SPS generation as a means for achieving a local flow balance. Finally, we also discuss other causes of SPS's, both SW-induced and intrinsic to the MSH. SPS's appear to be universal means for establishing a new equilibrium between flowing plasmas and may also prove to be important for astrophysical and fusion applications

What is the solar wind frame of reference?

Various solar wind ion species move with different speeds and theoretical considerations as well as limited observations in a region close to the Sun show that heavy solar wind ions tend to flow faster than protons, at least in less-aged fast solar wind streams. The solar wind flow carries the frozen-in interplanetary magnetic field (IMF) and this situation evokes three related questions: (i) what is the proper solar wind speed, (ii) is this speed equal to the speed of the dominant component, whatever that may be, and (iii) what is the speed of the magnetic field? We show that simple theoretical considerations based on the MHD approximation as well as on the dynamics of charged particles in electric and magnetic fields suggest that the IMF velocity of motion (de Hoffmann–Teller (HT) velocity) would be deliberated as the velocity appropriate for solar wind studies. Our analysis based on the Wind, Helios, ACE, and SOHO observations of differential streaming of solar wind populations shows that their energy is conserved in the HT frame. On the other hand, the noise and temporal resolution of the data do not allow us to decide whether the total momentum is also conserved in this frame

Predictors of Renal Outcomes in Sclerotic Class Anti-Neutrophil Cytoplasmic Antibody Glomerulonephritis

Background: The prognostic value of the anti-neutrophil cytoplasmic antibody (ANCA) associated glomerulonephritis (GN) classification has been demonstrated in several cohorts with sclerotic class having the worst renal outcome. Relevant published data on factors predicting outcomes in sclerotic ANCA GN is limited. Methods: Sclerotic ANCA GN patients were recruited from 5 centers worldwide for this retrospective cohort study. We describe the clinical characteristics of this cohort and evaluate predictors of 1-year glomerular filtration rate (GFR) and end-stage renal disease (ESRD). Kidney function at 12 months as measured by Modification of Diet in Renal Disease estimated GFR (eGFR) was modeled by simple and multiple linear regression analyses. We used Cox proportional hazards regression modeling to evaluate ESRD-free survival. Results: Of the 50 patients, 92% were Caucasian and 60% male with a mean age of 61 years. While 72% had renal limited disease, 82% were MPO ANCA positive. Kidney biopsies contained a median of 20 (interquartile range [IQR] 15–34) glomeruli with 96% showing moderate to severe interstitial fibrosis. Overall, 96% of patients received immunosuppressive drug therapy and 16% received plasmapheresis. Treatment response was achieved in all but 1 patient. The median (IQR) eGFR at entry was 14.5 (9–19) mL/min/1.73 m2. Over a median (IQR) follow-up of 33.5 (17–82) months, 26 patients reached ESRD. Ten patients died with 6 of the deaths occurring within the first year of diagnosis. The hazard of progression to ESRD was significantly higher in those with lower GFR at study entry (p = 0.003) and with higher degree of tubular atrophy (p = 0.043). Conclusions: Renal recovery is rare among sclerotic ANCA GN patients requiring dialysis at entry and 12% of patients died in the first year. Entry GFR and tubular atrophy were significant predictors of GFR at 12 months and renal survival in patients with sclerotic class ANCA GN