Search

Two sounding rockets, designated TRICE‐2, were launched on 8 December 2018 into the northern cusp region. The two rockets were designated the high‐ and low‐flyers, respectively, and launched 2 min apart to investigate cusp structures, specifically their spatial or temporal nature. 2 hr prior to the cusp encounter by the TRICE‐2 rockets, the MMS satellites, located in the magnetopause boundary layer, observed switching ion beams under very similar IMF conditions as later observed by TRICE‐2. The observed ion beam switch in the boundary layer defined the location of the primary dayside X‐line. Both, TRICE‐2 and MMS, also observed the signatures of multiple X‐lines at the magnetopause, overlapping ion‐energy dispersions in the cusp and counterstreaming ion beams in the magnetopause boundary layer, respectively. In addition to the TRICE‐2 cusp observations, ionospheric convection patterns from the SuperDARN radar are used to explain the vastly different cusp ion signatures observed by the TRICE‐2 rockets. While the high‐flyer rocket progressed north through the center of the cusp, the low‐flyer rocket drifted off to the east and crossed into the dusk convection cell, traveling perpendicular to the ionospheric convection direction before reaching the poleward oriented section of the convection cell also observed by the high‐flyer counterpart. Key Points: TRICE‐2 cusp ion dispersions are explained using the different magnetic foot points of the rockets through the ionospheric convection cellsTRICE‐2 cusp crossing occurred 2 hr after an MMS magnetopause crossing during similar IMF conditionsOverlapping cusp ion energy dispersions result from multiple magnetopause reconnection locations in agreement with MMS observations [ABSTRACT FROM AUTHOR]

The launch of the Twin Rockets to Investigate Cusp Electrodynamics‐2 (TRICE‐2) took place on the morning of 08 December 2018. The two rockets of this campaign each sampled the low‐altitude Northern Hemisphere cusp region at approximately the apex of each rocket's trajectory (1,042 and 757 km for the High flyer and Low flyer, respectively). Ion and electron electrostatic analyzers (ESAs) on board each rocket measured in situ particle populations throughout the flights. Energy‐flux spectrograms of ions and electrons from each ESA clearly show the passage of each rocket through the cusp region. This work examines the locations of these entrance/exit points in relation to cusp models as provided in and compiled from the published literature, along with a discussion of model variables that have been optimized to best fit the cusp region boundary sampling locations by TRICE‐2. The results of this study set the stage for understanding the upcoming NASA Small Explorer Tandem Reconnection and Cusp Electrodynamics Reconnaissance Satellites orbital plane intersections with (i.e., "trajectory cuts" through) the cusp region. Key Points: The low‐altitude cusp region was directly sampled by instruments onboard the two Twin Rockets to Investigate Cusp Electrodynamics‐2 rocketsCusp models have been compiled from published studies, with free parameters representing the low‐latitude boundary layer and mantleCusp model free parameters have been optimized to best match the observed cusp region location [ABSTRACT FROM AUTHOR]

Magnetospheric Multiscale (MMS) observations during an extended crossing of the Earth's dayside magnetopause show evidence of multiple reconnections at the boundary. This crossing occurred when the Interplanetary Magnetic Field (IMF) was southward and had a significant BY component. Approximately 2 hr after this crossing, the Twin Rocket Investigation of Cusp Electrodynamics‐2 rockets were launched into the northern hemisphere cusp and observed overlapping cusp ion injections. These overlapping injections are also evidence of multiple reconnections at the magnetopause. Observations more than 2 hr apart do not constitute conjunction between the spacecraft and the rockets. However, the IMF conditions during the magnetopause crossing and the cusp traversal were very similar. Therefore, had the magnetopause crossings and cusp traversals occurred at the same time, the observations would have been similar. Thus, these two events illustrate the link between multiple reconnections at the magnetopause and overlapping cusp ion injections. Plain Language Summary: Magnetic reconnection is a fundamental process in plasmas that interconnects magnetic field lines on either side of a current layer and converts magnetic energy into particle energy. It is the primary process that interconnects the magnetic field of the Sun with the magnetic field of the Earth at the current layer interface called the magnetopause. Ions and electrons from the solar wind follow these interconnected field lines into the Earth's magnetospheric cusps. Magnetic reconnection at the magnetopause occurs along long lines, called X‐lines. This paper discusses observations at the magnetopause and in the cusp that indicate that there are actually multiple X‐lines at the magnetopause and these multiple X‐lines produce a specific signature in the cusp called overlapping ion injections. Key Points: Magnetospheric multiscale observations often show evidence of multiple reconnection at the magnetopauseTwin Rocket Investigation of Cusp Electrodynamics‐2 observations of overlapping cusp ion injections are also evidence of multiple reconnections at the magnetopauseThere is a strong link between multiple reconnections at the magnetopause and overlapping cusp ion dispersions [ABSTRACT FROM AUTHOR]

On December 08, 2018 the Twin Rocket Investigation of Cusp Electrodynamics 2 (TRICE 2) mission was successfully launched. The mission consisted of two sounding rockets, each carrying a payload capable of measuring electron and ion distributions, electric and magnetic fields, and plasma waves occurring in the northern magnetospheric cusp. This study highlights the ion and wave observations obtained by TRICE 2 in the cusp and observations from the magnetospheric multiscale (MMS) spacecraft at the low‐latitude magnetopause two hours prior to the TRICE 2 traversal of the cusp. Within the cusp, typical ion cusp features were observed, that is, energy‐latitude dispersion of injected magnetosheath plasma. However, a lower energy population was also measured near the equatorward edge of the cusp on open field lines. Pitch‐angle distributions of the low‐energy ions suggest that this population was magnetospheric in origin, and not from ionospheric upflows. Data from MMS show that counterstreaming ions were present in the outer magnetosphere and low‐latitude boundary layer at similar energies to those observed by TRICE 2 in the cusp. Correlations between the low‐energy ions within the cusp and broadband extremely low frequency waves suggest that the low‐energy magnetospheric ions that filled the flux tube may have undergone wave‐particle interactions. These interactions may cause pitch‐angle scattering of low‐energy magnetospheric ions closer to the loss cone, thereby allowing them to precipitate into the cusp and be measured by the TRICE 2 sounding rockets. Key Points: Low‐energy ions measured near the equatorward edge of the cusp by TRICE 2 are locally mirroring and propagating toward the ionosphereA similar counter‐streaming ion population is observed at the magnetopause by MMS two hours prior to the TRICE 2 cusp traversalIon and wave data in the cusp suggest wave‐particle interactions are pitch angle scattering low‐energy magnetospheric ions [ABSTRACT FROM AUTHOR]

During the Twin Rockets to Investigate Cusp Electrodynamics (TRICE‐2) High‐Flyer rocket's passage through the cusp the high frequency (HF) radio wave receiver observed three intervals of banded upper‐hybrid (UH) waves. The bands begin at the UH frequency (∼1.2–1.3 MHz), descending to as low as 1.1 MHz, with amplitudes of hundreds of mV/m. The spacing of the bands are ∼4.5–6 kHz and the number of bands ranges from 3 to 10. Simultaneously, the very low frequency (VLF) radio wave receiver observed lower‐hybrid (LH) waves with amplitudes ranging from 1 to 10 mV/m and frequencies of 4.5–6 kHz. Slight variations of the spacings of the bands in the UH waves were closely correlated with variations in the LH peak frequencies. Two possible wave‐wave interactions are explored to explain this phenomenon: decay of an UH wave into a lower frequency UH wave and a LH wave, and coalescence of independent UH waves and LH waves that spawn UH waves. Using a dispersion relation calculator with electron and ion distribution functions based off those observed by the particle instruments suggests that UH waves, and to a lesser degree LH waves, can be excited by linear instabilities. Kinematic analysis of the waves dispersion relations and the wave matching conditions show that wave‐wave interactions linking UH and LH modes are possible through either decay or coalescence. This analysis along with comparisons of the energy densities of the waves, and the ratio of their occupation numbers suggest that the decay process is more likely than coalescence. Key Points: Modulated upper‐hybrid (UH) waves coincided with enhanced power near the local lower‐hybrid (LH) frequencyThe spacings of the banded UH waves are correlated with the frequency of the peak spectral density near the LH peaksKinematic constraints and energy densities of wave modes suggest wave‐wave process is plausible, with decay more likely than coalescence [ABSTRACT FROM AUTHOR]

Auroral whistler‐mode radio emissions called saucers are of fundamental interest because they require an unusually stationary emission process in the dynamic auroral environment, and it is a mystery how that can happen in this or similar conditions elsewhere in geospace. The Cusp Alfvén and Plasma Electrodynamics Rocket (CAPER‐2), launched into the cusp, obtained the first rocket measurements of a large‐scale, multiple‐armed dayside saucer, similar to those observed by the DEMETER satellite, with the addition of particle measurements and ground‐based measurements. Analysis of saucer shapes, directional measurements using waveforms, and ground‐based data show that, accounting for estimated uncertainties, these originate at altitudes ∼4,000 km within the cusp, the eastern side of which is penetrated by the rocket ∼100 s after the saucers are encountered. On‐board particle instruments show dispersed electron bursts in the cusp, Alfvénically accelerated at altitudes at or above the saucer sources. Plain Language Summary: Electrons, precipitating down Earth's high‐latitude magnetic field lines, emit radio waves at angles to the background magnetic field, depending on frequency. When spacecrafts traverse through a region close to the source, they observe descending and ascending frequency signatures referred to as saucers. This research focused on rocket measurements of large‐scale, multiarmed saucers on the dayside. Using ray‐tracing software and hodogram analysis of the electric field waveforms combined with ground‐based measurements, we were able to determine the source location of the saucers to be in the magnetic field's cusp at altitudes near 4,000 km. Additionally, particle measurements on‐board the rocket showed time dispersed bursts of electrons typically associated with Alfvénic acceleration, which can be traced back to a source height that is equal to or above the source heights of the observed saucers. This is the first time that dayside large‐scale saucers have been associated with the cusp. Key Points: First observation of large‐scale dayside saucers from a sounding rocketThe saucers are estimated to originate at ∼4,000 km on cusp field lines to within estimated uncertaintiesDispersed electrons observed in the cusp were accelerated at altitudes at or above the saucer signal source region [ABSTRACT FROM AUTHOR]

The FIELDS instrumentation suite on the Magnetospheric Multiscale (MMS) mission provides comprehensive measurements of the full vector magnetic and electric fields in the reconnection regions investigated by MMS, including the dayside magnetopause and the night-side magnetotail acceleration regions out to 25 Re. Six sensors on each of the four MMS spacecraft provide overlapping measurements of these fields with sensitive cross-calibrations both before and after launch. The FIELDS magnetic sensors consist of redundant flux-gate magnetometers (AFG and DFG) over the frequency range from DC to 64 Hz, a search coil magnetometer (SCM) providing AC measurements over the full whistler mode spectrum expected to be seen on MMS, and an Electron Drift Instrument (EDI) that calibrates offsets for the magnetometers. The FIELDS three-axis electric field measurements are provided by two sets of biased double-probe sensors (SDP and ADP) operating in a highly symmetric spacecraft environment to reduce significantly electrostatic errors. These sensors are complemented with the EDI electric measurements that are free from all local spacecraft perturbations. Cross-calibrated vector electric field measurements are thus produced from DC to 100 kHz, well beyond the upper hybrid resonance whose frequency provides an accurate determination of the local electron density. Due to its very large geometric factor, EDI also provides very high time resolution (∼1 ms) ambient electron flux measurements at a few selected energies near 1 keV. This paper provides an overview of the FIELDS suite, its science objectives and measurement requirements, and its performance as verified in calibration and cross-calibration procedures that result in anticipated errors less than 0.1 nT in B and 0.5 mV/m in E. Summaries of data products that result from FIELDS are also described, as well as algorithms for cross-calibration. Details of the design and performance characteristics of AFG/DFG, SCM, ADP, SDP, and EDI are provided in five companion papers. [ABSTRACT FROM AUTHOR]

The Electric and Magnetic Field Instrument and Integrated Science (EMFISIS) investigation on the NASA Radiation Belt Storm Probes (now named the Van Allen Probes) mission provides key wave and very low frequency magnetic field measurements to understand radiation belt acceleration, loss, and transport. The key science objectives and the contribution that EMFISIS makes to providing measurements as well as theory and modeling are described. The key components of the instruments suite, both electronics and sensors, including key functional parameters, calibration, and performance, demonstrate that EMFISIS provides the needed measurements for the science of the RBSP mission. The EMFISIS operational modes and data products, along with online availability and data tools provide the radiation belt science community with one the most complete sets of data ever collected. [ABSTRACT FROM AUTHOR]

Measurements of shear Alfvén waves are used to test the predictions of a variety of different electron collision operators, including several Krook collision operators as well as a Lorentz collision operator. New expressions for the collisional warm-plasma dielectric tensor resulting from the use of the fully magnetized collisional Boltzmann equation are presented here. Theoretical predictions for the parallel phase velocity and damping as a function of perpendicular wave number k⊥ are derived from the dielectric tensor. Laboratory measurements of the parallel phase velocity and damping of shear Alfvén waves were made to test these theoretical predictions in both the kinetic (vte≪vA) and inertial (vte≫vA) parameter regimes and at several wave frequencies (ω<ωci). Results show that, in the inertial regime, the best match between measurements and theory occur when any of the Krook operators are used to describe electron collisions. In contrast, the best agreement in the kinetic regime is found when collisions are completely ignored. [ABSTRACT FROM AUTHOR]

Human cytomegalovirus (CMV) infection is normally controlled effectively by the immune response, including CD4+ T cells. Large numbers of these cells are present in healthy seropositive individuals but their loss in immunosuppression leads to reactivation and disease. Tracking such responses in vivo is hampered by poor definition of their peptide targets. In this study, we defined the key targets of the peptide-specific CD4+ T cell responses to the CMV pp65 protein using functional assays and a peptide library. Despite a good deal of interindividual variation in the numbers of peptides recognized, responses to CMV pp65 were strikingly targeted at three key epitopes. A response to one or more of these three key peptides was seen in all individuals tested ( P < 0·0001) and this finding was tested and reproduced in a second independent population. The most common response identified was that to a DR53 restricted epitope, aa281–295. HLA-DR1 restricted CMV pp65-specific populations, although reproducibly detected, were of low frequency ex vivo. However, it was possible to detect and phenotype these cells using an enrichment protocol and this revealed them to have ‘effector memory’ status although, in contrast to CD8+ T cell responses, these were CD45RA–. These data suggest that CD4+ T cell responses to CMV can be identified reliably using a pool of just three peptides. This simple approach will provide a robust and reliable as well as economic method for tracking peptide specific populations in health and disease. [ABSTRACT FROM AUTHOR]

Ever since emphasis for noise control in the community has become greater, noise codes, both simple and complex, have emerged from states and municipalities. Most 'simple' codes are based on A-weighted standards while the 'complex' codes are based on octave band or statistical criteria. Montgomery County, Maryland's noise code has become effective relatively recently. Based on an A-weighted sound pressure level measurement, it attempts to provide a means for quantitatively determining noise violations. This paper presents the background of the development of the code and the code requirements. It will be shown that the A-weighted code and its development may not be as simple as one would expect. [ABSTRACT FROM AUTHOR]

An A-weighted community noise code was developed for Montgomery County. The code requires a single number noise measurement for enforcement. This paper describes the procedure used and the experience of the County in enforcement since the code became enforceable. Although no legal tests have come up since the code became effective (1 October 1976), it appears that there may be some trouble should it come to court. Description of these possible problems will be discussed. [ABSTRACT FROM AUTHOR]