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Conference paperHorner G, Gryspeerdt E, 2022,
Investigating the evolution of tropical cirrus clouds from deep convection
<jats:p>&lt;p&gt;Tropical convective clouds, particularly their large cirrus outflows, play an important role in modulating the energy balance of the Earth&amp;#8217;s atmosphere. Understanding the evolution of these clouds, and how they change in response to anthropogenic emissions is therefore important to understand past and future climate change. Previous work has focused on tracking individual convective cores and their evolution into anvil cirrus and subsequent thin cirrus clouds in satellite data.&lt;/p&gt;&lt;p&gt;In this work we have introduced a novel approach to investigating the evolution of tropical convective clouds by creating a &amp;#8216;Time Since Convection&amp;#8217; (TSC) dataset. Using reanalysis windspeeds, the time since the air at each location last experienced a convective event (as defined by the presence of a deep convective core) is calculated. Used in conjunction with data from the DARDAR and CERES products, we can build a composite picture of the radiative and microphysical properties of the clouds as a function of their time since convection.&lt;/p&gt;&lt;p&gt;As with previous studies, we find that cloud properties are a strong function of time since convection, with decreases in the optical thickness, cloud top height, and cloud fraction over time. These changes in in cloud properties also have a significant radiative impacts, with the longwave and shortwave component of the cloud radiative effect also being a strong function of time since convection. In addition, using the DARDAR product, a combination of CloudSat radar and the CALIPSO lidar measurements, we build composite cross sections of convective clouds, characterising their vertical evolution and how it is influenced by external meteorological and initial conditions flagged in the TSC dataset.&lt;/p&gt;</jats:p>
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Journal articleTeixeira J, Burton C, Kelley DI, et al., 2022,
Representing socio-economic factors in INFERNO using the Human Development Index
<jats:p>&lt;p&gt;INFERNO human fire ignitions and fire suppression functions excluded the representation of socio-economic factors (aside population density) that can affect anthropogenic behaviour regarding fire ignitions. To address this, we implement a socio-economic factor in the fire ignition and suppression parametrisation in INFERNO based on an Human Development Index (HDI) term. The HDI is calculated based on three indicators designed to capture the income, health, and education dimensions of human development. Therefore, we assume this leads to a representation where if there is more effort in improving human development, there is also investment on higher fire suppression by the population. Including this representation of socio-economic factors in INFERNO we were able to reduce large positive biases that were found for the regions of Temperate North America, Central America, Europe and Southern Hemisphere South America without significant impact to other regions, improving the model performance at a regional level and better representing processes that drive fire behaviour in the Earth System.&lt;/p&gt;</jats:p>
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Journal articlePisa D, Soucek J, Santolik O, et al., 2022,
Observations of the Time Domain Sampler receiver from the Radio and Plasma Wave instrument during the Solar Orbiter Earth flyby&#160;
<jats:p>&lt;p&gt;On November 27, 2021, Solar Orbiter completed its only flyby of Earth on its way to the following Sun&amp;#8217;s encounter in March 2022. Although this fast flyby was performed primarily to decrease the spacecraft&amp;#8217;s velocity and change orbit to get closer to the Sun, the Radio and Plasma Wave (RPW) instrument had the opportunity to perform high cadence measurements in the Earth&amp;#8217;s magnetosphere. We review the main observation of the Time Domain Sampler (TDS) receiver, a part of the RPW instrument, made during this flyby at frequencies below 200 kHz. The TDS receiver operated in a high cadence mode providing us with the regular waveform snapshot with 62 ms length every ten seconds for two electric components. Besides the regular captures, we have got more than five hundred onboard classified snapshots and the statistical products with a sixteen-second cadence. Before entering the terrestrial magnetosphere around 02:30UT, the spacecraft wandered through the foreshock region, registering intense bursts of Langmuir waves. After the bowshock crossing, Solar Orbiter was for more than two hours in the morning sector of the magnetosphere, recording various plasma wave modes. The closest approach was reached at 04:30UT above North Africa at an altitude of 460 km. Then the spacecraft continued into the Earth&amp;#8217;s tail and entered the magnetosheath around 13:00UT. After 15:00UT, the Solar Orbiter crossed the bowshock, and bursts of Langmuir waves were detected again pointing out to the deep downstream foreshock region. Further from the Earth, intense Auroral Kilometric Radiation (AKR) at frequencies above 100 kHz was also detected.&lt;/p&gt;</jats:p>
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Journal articleLaker R, Horbury T, Matteini L, et al., 2022,
On the Deflections of Switchbacks
<jats:p>&lt;p&gt;Following their presence during Parker Solar Probe&amp;#8217;s (PSP) first encounter, switchbacks have become an active area of research with several proposed mechanisms for their formation. Many of these theories have testable predictions, although it is not trivial to compare simulation results with in-situ data from PSP. For example, there is some debate regarding the deflection direction of switchbacks, with some theories predicting a consistent magnetic deflection in the +T direction in the RTN coordinate system. Such arguments are largely focussed on the first two PSP encounters, as these are the most studied encounters in the literature. We examine the deflection direction of switchbacks for the first eight PSP encounters, with the aim to clear up any ambiguity regarding this property of switchbacks. Much like the earlier results of Horbury et al. 2020 (during the first encounter) we find that switchbacks tend to deflect in the same direction for hours at a time. Although there is some consistency in deflection direction within an individual encounter, crucially we find that there is no preferred deflection direction across all the encounters. We speculate about the cause of these results and what implications they may have for switchback formation theories.&lt;/p&gt;</jats:p>
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Journal articlePal S, Kilpua E, Good S, et al., 2022,
Eruption and Interplanetary Evolution of a Stealth Streamer-blowout CME Observed at ~0.5 AU&#160;
<jats:p>&lt;p&gt;The orbit of the Parker Solar Probe (PSP) during the 5th encounter with the Sun presented an opportunity for a multi-observation analysis including the observations of Sun-Earth Connection Coronal and Heliospheric Investigation (SECCHI) coronagraphs and Large Angle and Spectrometric Coronagraph (LASCO) coronagraphs. Streamer-blowout coronal mass ejections (SBO-CMEs) are the dominant CME population during solar minimum. With the aid of extrapolated coronal fields and remote observations of the off-limb low corona, we study the initiation of an SBO-CME preceded by consecutive CME eruptions following a multi-stage sympathetic breakout scenario. The suprathermal electron pitch-angle distributions (PADs) and magnetic field observations by PSP suggest that draping of interplanetary magnetic field lines about the CME caused a curvature in the adjacent heliospheric current sheet, initiated magnetic reconnection with the CME flux rope about ~45 hours before it encountered PSP, and eroded ~38% of its initial poloidal magnetic flux at ~0.5 AU. This study covering inner heliospheric observation and analysis of SBO-CME magnetic content provides important implications for the origin of twisted magnetic field lines in SBO-CME flux ropes as the flux rope is not perturbed much by the interplanetary propagation. Also, the multi-spacecraft observations allowed us to estimate the distances where reconnection between the flux rope and its surroundings may be initiated.&amp;#160;&lt;/p&gt;</jats:p>
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Journal articleDesai R, Eastwood J, Eggington J, et al., 2022,
Magnetospheric compressions, magnetopause shadowing and the last-closed-drift-shell
<jats:p>&lt;p&gt;Fluxes in the outer radiation belt can vary by orders of magnitude in response to solar wind driving conditions. Magnetopause shadowing, where electron and proton drift paths intersect the magnetopause boundary, is a fundamental loss process which operates on sub-day timescales and can result in rapid loss across the outer radiation belt. Accurate characterisation of this is therefore required to fully account for outer radiation belt dynamics and to avoid unrealistic fluxes impacting long-term forecasts. In this paper we utilise particle simulations of the radiation belts integrated within evolving global MHD simulations, to provide high-resolution high-fidelity simulations of the phenomenon of magnetopause shadowing. We model a variety of magnetopause compression scenarios corresponding to extreme cases of interplanetary shock impacts, and gradual increases in solar wind dynamic pressure. We thus constrain how time-dependent topological variation of the magnetospheric fields results in a complex interplay of open and closed particle drift paths, and examine the role of the electric field in modulating escaping particles trajectories as well as corresponding prompt injections into the inner magnetosphere.&lt;/p&gt;</jats:p>
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Journal articleWoolley T, Matteini L, Horbury TS, et al., 2022,
Linking In-situ Magnetic and Density Structures in the Low Latitude Slow Solar Wind to Solar Origins
<jats:p>&lt;p&gt;To date, Parker Solar Probe has completed ten solar encounters and measured a wealth of in-situ data down to heliocentric distances of ~13 solar radii. This data provides a novel opportunity to investigate the near-Sun environment and understand the young slow solar wind. Typically, the slow solar wind observed in the inner heliosphere is split into an Alfvenic and a non-Alfvenic component. The Alfvenic slow wind is thought to originate from overexpanded coronal hole field lines, whereas the non-Alfvenic slow wind could originate from active regions, transient events, or reconnection at the tips of helmet streamers. In this work, we find structures associated with non-Alfvenic slow wind in the low latitude wind measured by Parker Solar Probe. We identify at least two distinct types of structure using magnetic field magnitude, electron pitch angle distributions, and electron number density. After statistically analysing these structures, with a focus on their plasma properties, shape, and location with respect to the heliospheric current sheet, we link them to solar origins. We find structures that are consistent with the plasma blobs seen previously in remote sensing observations.&lt;/p&gt;</jats:p>
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Journal articleMaffei S, Livermore P, Mound J, et al., 2022,
The future evolution of the auroral zones
<jats:p>&lt;p&gt;The auroral zones indicate the locations on the Earth&amp;#8217;s surface where, on average, it is most likely to spot aurorae as a consequence of increased solar activity. The shape of the auroral zones and, similarly, the geographical locations most vulnerable to extreme space weather events are modulated by the geomagnetic field of internal origin. As the latter evolves in time, the formers will be subject to variations on the same timescales.&lt;/p&gt;&lt;p&gt;From available geomagnetic field forecasts (which provide an estimate of the future evolution of the geomagnetic field of internal origin) we derive AACGM latitudes and estimate the future evolution of the auroral zones. The novel aspect of this technique is that we make use of all available Gauss coefficients to produce the forecasts, while the majority of present techniques estimate the location of the auroral zones based on the dipolar coefficients only. Our results show that, while the shift of the geomagnetic dipole axis has a first order contribution, higher order Gauss coefficients contribute significantly to the location and shape of the auroral zones.&lt;/p&gt;&lt;p&gt;The same technique is then extended to estimate the future location of the geographical location that would be, on average, most exposed to extreme space weather event. We find that the space-weather related risk will not change significantly for the UK over the next 50 years. For the Canadian provinces of Quebec and Ontario, however, we predict a significant increase in the risk associated to extreme solar activity.&lt;/p&gt;</jats:p>
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Journal articleBen-Yami M, Oetjen H, Brindley H, et al., 2022,
Emissivity retrievals with FORUM's end-to-end simulator: challenges and recommendations
, Atmospheric Measurement Techniques, Vol: 15, Pages: 1755-1777, ISSN: 1867-1381Spectral emissivity is a key property of the Earth's surface, of which only very few measurements exist so far in the far-infrared (FIR) spectral region, even though recent work has shown that the FIR is important for accurate modelling of the global climate. The European Space Agency's 9th Earth Explorer, FORUM (Far-infrared Outgoing Radiation Understanding and Monitoring) will provide the first global spectrally resolved measurements of the Earth's top-of-the-atmosphere (TOA) spectrum in the FIR. In clear-sky conditions with low water vapour content, these measurements will provide a unique opportunity to retrieve spectrally resolved FIR surface emissivity. In preparation for the FORUM mission with an expected launch in 2027, this study takes the first steps towards the development of an operational emissivity retrieval for FORUM by investigating the sensitivity of the emissivity product of a full spectrum optimal estimation retrieval method to different physical and operational parameters. The tool used for the sensitivity tests is the FORUM mission's end-to-end simulator. These tests show that the spectral emissivity of most surface types can be retrieved for dry scenes in the 350–600 cm−1 region, with an absolute uncertainty ranging from 0.005 to 0.01. In addition, the quality of the retrieval is quantified with respect to the precipitable water vapour content of the scene, and the uncertainty caused by the correlation of emissivity with surface temperature is investigated. Based on these investigations, a road map is recommended for the development of the operational emissivity product.
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Journal articleSaboya E, Zazzeri G, Graven H, et al., 2022,
Continuous CH4 and delta(CH4)-C-13 measurements in London demonstrate under-reported natural gas leakage
, Atmospheric Chemistry and Physics, Vol: 22, Pages: 3595-3613, ISSN: 1680-7316Top-down greenhouse gas measurements can be used to independently assess the accuracy of bottom-up emission estimates. We report atmospheric methane (CH4) mole fractions and δ13CH4 measurements from Imperial College London from early 2018 onwards using a Picarro G2201-i analyser. Measurements from March 2018 to October 2020 were compared to simulations of CH4 mole fractions and δ13CH4 produced using the NAME (Numerical Atmospheric-dispersion Modelling Environment) dispersion model coupled with the UK National Atmospheric Emissions Inventory, UK NAEI, and a global inventory, the Emissions Database for Global Atmospheric Research (EDGAR), with model spatial resolutions of ∼ 2, ∼ 10, and ∼ 25 km. Simulation–measurement comparisons are used to evaluate London emissions and the source apportionment in the global (EDGAR) and UK national (NAEI) emission inventories. Observed mole fractions were underestimated by 30 %–35 % in the NAEI simulations. In contrast, a good correspondence between observations and EDGAR simulations was seen. There was no correlation between the measured and simulated δ13CH4 values for either NAEI or EDGAR, however, suggesting the inventories' sectoral attributions are incorrect. On average, natural gas sources accounted for 20 %–28 % of the above background CH4 in the NAEI simulations and only 6 %–9 % in the EDGAR simulations. In contrast, nearly 84 % of isotopic source values calculated by Keeling plot analysis (using measurement data from the afternoon) of individual pollution events were higher than −45 ‰, suggesting the primary CH4 sources in London are actually natural gas leaks. The simulation–observation comparison of CH4 mole fractions suggests that total emissions in London are much higher than the NAEI estimate (0.04 Tg CH4 yr−1) but close to, or slightly lo
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Journal articleReville V, Fargette N, Rouillard AP, et al., 2022,
Flux rope and dynamics of the heliospheric current sheet Study of the Parker Solar Probe and Solar Orbiter conjunction of June 2020
, Astronomy and Astrophysics: a European journal, Vol: 659, Pages: 1-14, ISSN: 0004-6361Context. Solar Orbiter and Parker Solar Probe jointly observed the solar wind for the first time in June 2020, capturing data from very different solar wind streams: calm, Alfvénic wind and also highly dynamic large-scale structures.Context. Our aim is to understand the origin and characteristics of the highly dynamic solar wind observed by the two probes, particularly in the vicinity of the heliospheric current sheet (HCS).Methods. We analyzed the plasma data obtained by Parker Solar Probe and Solar Orbiter in situ during the month of June 2020. We used the Alfvén-wave turbulence magnetohydrodynamic solar wind model WindPredict-AW and we performed two 3D simulations based on ADAPT solar magnetograms for this period.Results. We show that the dynamic regions measured by both spacecraft are pervaded by flux ropes close to the HCS. These flux ropes are also present in the simulations, forming at the tip of helmet streamers, that is, at the base of the heliospheric current sheet. The formation mechanism involves a pressure-driven instability followed by a fast tearing reconnection process. We further characterize the 3D spatial structure of helmet streamer born flux ropes, which appears in the simulations to be related to the network of quasi-separatrices.
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Journal articleUkhorskiy AY, Sorathia KA, Merkin VG, et al., 2022,
Cross-scale energy cascade powered by magnetospheric convection
, SCIENTIFIC REPORTS, Vol: 12, ISSN: 2045-2322- Author Web Link
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- Citations: 2
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Journal articleDesai M, Mitchell DG, McComas DJ, et al., 2022,
Suprathermal ion energy spectra and anisotropies near the heliospheric current sheet crossing observed by the Parker Solar Probe during encounter 7
, The Astrophysical Journal: an international review of astronomy and astronomical physics, Vol: 927, Pages: 1-12, ISSN: 0004-637XWe present observations of ≳10–100 keV nucleon−1 suprathermal (ST) H, He, O, and Fe ions associated with crossings of the heliospheric current sheet (HCS) at radial distances of <0.1 au from the Sun. Our key findings are as follows: (1) very few heavy ions are detected during the first full crossing, the heavy-ion intensities are reduced during the second partial crossing and peak just after the second crossing; (2) ion arrival times exhibit no velocity dispersion; (3) He pitch-angle distributions track the magnetic field polarity reversal and show up to ∼10:1 anti-sunward, field-aligned flows and beams closer to the HCS that become nearly isotropic farther from the HCS; (4) the He spectrum steepens either side of the HCS, and the He, O, and Fe spectra exhibit power laws of the form ∼E−4–E6; and (5) maximum energies EX increase with the ion's charge-to-mass (Q/M) ratio as ${E}_{X}/{E}_{H}\propto {({Q}_{X}/{M}_{X})}^{\delta }$, where δ ∼ 0.65–0.76, assuming that the average Q states are similar to those measured in gradual and impulsive solar energetic particle events at 1 au. The absence of velocity dispersion in combination with strong field-aligned anisotropies closer to the HCS appears to rule out solar flares and near-Sun coronal-mass-ejection-driven shocks. These new observations present challenges not only for mechanisms that employ direct parallel electric fields and organize maximum energies according to E/Q but also for local diffusive and magnetic-reconnection-driven acceleration models. Reevaluation of our current understanding of the production and transport of energetic ions is necessary to understand this near-solar, current-sheet-associated population of ST ions.
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Journal articleSioulas N, Velli M, Chhiber R, et al., 2022,
Statistical Analysis of Intermittency and its Association with Proton Heating in the Near-Sun Environment
, ASTROPHYSICAL JOURNAL, Vol: 927, ISSN: 0004-637X- Author Web Link
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- Citations: 8
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Journal articleLarosa A, Dudok de Wit T, Krasnoselskikh V, et al., 2022,
Langmuir-Slow Extraordinary Mode Magnetic Signature Observations with Parker Solar Probe
, ASTROPHYSICAL JOURNAL, Vol: 927, ISSN: 0004-637X- Author Web Link
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- Citations: 4
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Journal articleMozer FS, Bale SD, Cattell CA, et al., 2022,
Core Electron Heating by Triggered Ion Acoustic Waves in the Solar Wind
, ASTROPHYSICAL JOURNAL LETTERS, Vol: 927, ISSN: 2041-8205- Author Web Link
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- Citations: 4
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Journal articleReville V, Velli M, Panasenco O, et al., 2022,
The Role of Alfven Wave Dynamics on the Large-scale Properties of the Solar Wind: Comparing an MHD Simulation with <i>Parker Solar Probe</i> E1 data (vol 246. 24, 2020)
, ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 259, ISSN: 0067-0049 -
Journal articleWang S, Toumi R, 2022,
On the intensity decay of tropical cyclones before landfall
, Scientific Reports, Vol: 12, ISSN: 2045-2322It remains unclear how tropical cyclones (TCs) decay from their ocean lifetime maximum intensity (LMI) to landfall intensity (LI), yet this stage is of fundamental importance governing the socio-economic impact of TCs. Here we show that TCs decay on average by 25% from LMI to LI. A logistic decay model of energy production by ocean enthalpy input and surface dissipation by frictional drag, can physically connect the LMI to LI. The logistic model fits the observed intensity decay as well as an empirically exponential decay does, but with a clear physical foundation. The distance between locations of LMI and TC landfall is found to dominate the variability of the decay from the LMI to LI, whereas environmental conditions are generally less important. A major TC at landfall typically has a very large LMI close to land. The LMI depends on the heating by ocean warming, but the LMI location is also important to future landfall TC intensity changes which are of socio-economic importance.
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Journal articleTrofimov H, Post P, Gryspeerdt E, et al., 2022,
Meteorological conditions favorable for strong anthropogenic aerosol impacts on clouds
, Journal of Geophysical Research: Atmospheres, Vol: 127, ISSN: 2169-897XShip-track-like polluted cloud tracks provide a direct way to study aerosol-cloud interactions. Here, we study environmental conditions favorable for pollution tracks' formation. We study polluted cloud tracks forming downwind of localized anthropogenic air pollution hot spots of Norilsk and Cherepovets in Russia and Thompson in Canada. Polluted cloud tracks form on 20%–37% of days with liquid-phase clouds. The large-scale atmospheric circulation largely determines the occurrence of track-favoring conditions. Tracks tend to form in clean and thin clouds under stable and dry conditions that are more often associated with anticyclonic large-scale flow in the studied locations.
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Journal articleChen L-J, Halekas J, Wang S, et al., 2022,
Solitary Magnetic Structures Developed From Gyro-Resonance With Solar Wind Ions at Mars and Earth
, GEOPHYSICAL RESEARCH LETTERS, Vol: 49, ISSN: 0094-8276- Author Web Link
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- Citations: 2
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Journal articleMostafavi P, Allen RC, McManus MD, et al., 2022,
Alpha-Proton Differential Flow of the Young Solar Wind: Parker Solar Probe Observations
, ASTROPHYSICAL JOURNAL LETTERS, Vol: 926, ISSN: 2041-8205- Author Web Link
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- Citations: 6
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Journal articleZank GP, Zhao L-L, Adhikari L, et al., 2022,
Turbulence in the Sub-Alfvenic Solar Wind
, ASTROPHYSICAL JOURNAL LETTERS, Vol: 926, ISSN: 2041-8205- Author Web Link
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- Citations: 26
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Journal articleVasko IY, Alimov K, Phan T, et al., 2022,
Kinetic-scale Current Sheets in the Solar Wind at 1 au: Scale-dependent Properties and Critical Current Density
, ASTROPHYSICAL JOURNAL LETTERS, Vol: 926, ISSN: 2041-8205- Author Web Link
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- Citations: 9
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Journal articleShi C, Zhao J, Malaspina DM, et al., 2022,
Multiband Electrostatic Waves below and above the Electron Cyclotron Frequency in the Near-Sun Solar Wind
, ASTROPHYSICAL JOURNAL LETTERS, Vol: 926, ISSN: 2041-8205- Author Web Link
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- Citations: 4
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Journal articleRodriguez L, Barnes D, Hosteaux S, et al., 2022,
Comparing the heliospheric cataloging, analysis, and techniques service (HELCATS) manual and automatic catalogues of coronal mass ejections using solar terrestrial relations observatory/heliospheric Imager (STEREO/HI) Data
, Solar Physics: a journal for solar and solar-stellar research and the study of solar terrestrial physics, Vol: 297, ISSN: 0038-0938We present the results of a comparative study between automatic and manually compiled coronal mass ejection (CME) catalogues based on observations from the Heliospheric Imagers (HIs) onboard NASA’s Solar Terrestrial Relations Observatory (STEREO) spacecraft. Using the Computer Aided CME Tracking software (CACTus), CMEs are identified in HI data using an automatic feature-detection algorithm, while the Heliospheric Imagers Catalogue (HICAT) includes CMEs that are detected by visual inspection of HI images. Both catalogues were compiled as part of the EU FP7 Heliospheric Cataloguing, Analysis and Techniques Service (HELCATS) project (www.helcats-fp7.eu). We compare observational parameters of the CMEs from CACTus to those listed in HICAT, such as CME frequency, position angle (PA), and PA-width. We also compare CACTus-derived speeds to speeds derived from applying geometric modelling to the majority of the HICAT CMEs, the results of which are listed in the HELCATS Heliospheric Imagers Geometric Catalogue (HIGeoCAT). We find that both CACTus and HICAT catalogues contain a similar number of events when we exclude events narrower than 20∘, which are not included in the HICAT catalogue but are found to be identified by CACTus. PA-distributions are strongly peaked around 90∘ and 270∘, with a slightly larger CME frequency northwards of the equatorial plane (particularly for the STEREO-A versions of both catalogues). The CME PA-widths in both HICAT and CACTus catalogues peak at approximately 60∘. Manually derived speeds from HIGeoCAT and automatically derived speeds by CACTus correlate well for values lower than 1000 km s−1, in particular when CMEs are propagating close to the plane of the sky.
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Journal articleMozer FS, Bale SD, Kellogg PJ, et al., 2022,
An Improved Technique for Measuring Plasma Density to High Frequencies on the Parker Solar Probe
, ASTROPHYSICAL JOURNAL, Vol: 926, ISSN: 0004-637X- Author Web Link
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- Citations: 1
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Journal articleAgapitov V, Drake JF, Swisdak M, et al., 2022,
Flux Rope Merging and the Structure of Switchbacks in the Solar Wind
, ASTROPHYSICAL JOURNAL, Vol: 925, ISSN: 0004-637X- Author Web Link
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- Citations: 9
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Journal articleArcher M, Southwood D, Hartinger M, et al., 2022,
How a realistic magnetosphere alters the polarizations of surface, fast magnetosonic, and Alfvén waves
, Journal of Geophysical Research: Space Physics, Vol: 127, ISSN: 2169-9380System-scale magnetohydrodynamic (MHD) waves within Earth's magnetosphere are often understood theoretically using box models. While these have been highly instructive in understanding many fundamental features of the various wave modes present, they neglect the complexities of geospace such as the inhomogeneities and curvilinear geometries present. Here, we show global MHD simulations of resonant waves impulsively excited by a solar wind pressure pulse. Although many aspects of the surface, fast magnetosonic (cavity/waveguide), and Alfvén modes present agree with the box and axially symmetric dipole models, we find some predictions for large-scale waves are significantly altered in a realistic magnetosphere. The radial ordering of fast mode turning points and Alfvén resonant locations may be reversed even with monotonic wave speeds. Additional nodes along field lines that are not present in the displacement/velocity occur in both the perpendicular and compressional components of the magnetic field. Close to the magnetopause, the perpendicular oscillations of the magnetic field have the opposite handedness to the velocity. Finally, widely used detection techniques for standing waves, both across and along the field, can fail to identify their presence. We explain how all these features arise from the MHD equations when accounting for a non-uniform background field and propose modified methods that might be applied to spacecraft observations.
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Journal articleGetachew T, McComas DJ, Joyce CJ, et al., 2022,
PSP/IS⊙IS Observation of a Solar Energetic Particle Event Associated with a Streamer Blowout Coronal Mass Ejection during Encounter 6
, ASTROPHYSICAL JOURNAL, Vol: 925, ISSN: 0004-637X- Author Web Link
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- Citations: 2
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Journal articleBandyopadhyay R, Matthaeus WH, McComas DJ, et al., 2022,
Sub-Alfvenic Solar Wind Observed by the Parker Solar Probe: Characterization of Turbulence, Anisotropy, Intermittency, and Switchback
, ASTROPHYSICAL JOURNAL LETTERS, Vol: 926, ISSN: 2041-8205- Author Web Link
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- Citations: 21
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