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Journal articleHietala H, Trotta D, Fedeli A, et al., 2024,
Candidates for downstream jets at interplanetary shocks
, Monthly Notices of the Royal Astronomical Society, Vol: 531, Pages: 2415-2421, ISSN: 0035-8711Localized dynamic pressure enhancements arising from kinetic processes are frequently observed downstream of the Earth’s bow shock. These structures, called jets, modify their plasma surroundings and participate in particle energization. Here, we report the first observations of jet-like structures in a non-planetary shock environment: downstream of interplanetary shocks. We introduce an analysis approach suitable for such conditions and apply it to Wind spacecraft data. We present one event with a Mach number similar to the Earth’s bow shock as a benchmark, as well as two low Mach number, low beta shocks: a parameter range that is difficult to access at planets. The jet-like structures we find are tens of ion inertial lengths in size, and some are observed further away from the shock than in a limited magnetosheath. We find that their properties are similar to those of magnetosheath jets: in the frame of the shock these structures are fast, cold, and most have no strong magnetic field variations. All three interplanetary shocks feature foreshock activity, but no strongly compressive waves. We discuss the implications, these findings have for the proposed jet formation mechanisms.
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Journal articleKrupar V, Kruparova O, Szabo A, et al., 2024,
Radial Variations in Solar Type III Radio Bursts
, ASTROPHYSICAL JOURNAL LETTERS, Vol: 967, ISSN: 2041-8205 -
Journal articleJebaraj IC, Agapitov O, Krasnoselskikh V, et al., 2024,
Acceleration of Electrons and Ions by an "Almost" Astrophysical Shock in the Heliosphere
, ASTROPHYSICAL JOURNAL LETTERS, Vol: 968, ISSN: 2041-8205 -
Journal articleFuselier SA, Petrinec SM, Reiff PH, et al., 2024,
Global-scale processes and effects of magnetic reconnection on the geospace environment
, Space Science Reviews, Vol: 220, ISSN: 0038-6308Recent multi-point measurements, in particular from the Magnetospheric Multiscale (MMS)spacecraft, have advanced the understanding of micro-scale aspects of magnetic reconnection. In addition, the MMS mission, as part of the Heliospheric System Observatory, combined with recent advances in global magnetospheric modeling, have furthered the understanding of meso- and global-scale structure and consequences of reconnection. Magneticreconnection at the dayside magnetopause and in the magnetotail are the drivers of the globalDungey cycle, a classical picture of global magnetospheric circulation. Some recent advances in the global structure and consequences of reconnection that are addressed hereinclude a detailed understanding of the location and steadiness of reconnection at the dayside magnetopause, the importance of multiple plasma sources in the global circulation, andreconnection consequences in the magnetotail. These advances notwithstanding, there areimportant questions about global reconnection that remain. These questions focus on howmultiple reconnection and reconnection variability fit into and complicate the Dungey Cyclepicture of global magnetospheric circulation.
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Journal articleEastwood JP, Brown P, Magnes W, et al., 2024,
The Vigil magnetometer for operational space weather services from the Sun-Earth L5 point
, Space Weather, Vol: 22, ISSN: 1539-4956Severe space weather has the potential to cause significant socio-economic impact and it is widely accepted that mitigating this risk requires more comprehensive observations of the Sun and heliosphere, enabling more accurate forecasting of significant events with longer lead-times. In this context, it is now recognized that observations from the L5 Sun-Earth Lagrange point (both remote and in situ) would offer considerable improvements in our ability to monitor and forecast space weather. Remote sensing from L5 allows for the observation of solar features earlier than at L1, providing early monitoring of active region development, as well as tracking of interplanetary coronal mass ejections through the inner heliosphere. In situ measurements at L5 characterize the solar wind's geoeffectiveness (particularly stream interaction regions), and can also be ingested into heliospheric models, improving their performance. The Vigil space weather mission is part of the ESA Space Safety Program and will provide a real-time data stream for space weather services from L5 following its anticipated launch in the early 2030s. The interplanetary magnetic field is a key observational parameter, and here we describe the development of the Vigil magnetometer instrument for operational space weather monitoring at the L5 point. We summarize the baseline instrument capabilities, demonstrating how heritage from science missions has been leveraged to develop a low-risk, high-heritage instrument concept.
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Journal articleArcher M, Pilipenko V, Li B, et al., 2024,
Magnetopause MHD surface wave theory: progress & challenges
, Frontiers in Astronomy and Space Sciences, Vol: 11, ISSN: 2296-987XSharp boundaries are a key feature of space plasma environments universally, with their wave-like motion (driven by pressure variations or flow shears) playing a key role in mass, momentum, and energy transfer. This review summarises magnetohydrodynamic surface wave theory with particular reference to Earth’s magnetopause, due to its mediation of the solar-terrestrial interaction. Basic analytic theory of propagating and standing surface waves within simple models are presented, highlighting many of the typically-used assumptions. We raise several conceptual challenges to understanding the nature of surface waves within a complex environment such as a magnetosphere, including the effects of magnetic topology and curvilinear geometry, plasma inhomogeneity, finite boundary width, the presence of multiple boundaries, turbulent driving, and wave nonlinearity. Approaches to gain physical insight into these challenges are suggested. We also discuss how global simulations have proven a fruitful tool in studying surface waves in more representative environments than analytic theory allows. Finally, we highlight strong interdisciplinary links with solar physics which might help the magnetospheric community. Ultimately several upcoming missions provide motivation for advancing magnetopause surface wave theory towards understanding their global role in filtering, accumulating, and guiding turbulent solar wind driving.
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Journal articleKilpua EKJ, Good S, Ala-Lahti M, et al., 2024,
Permutation entropy and complexity analysis of large-scale solar wind structures and streams
, ANNALES GEOPHYSICAE, Vol: 42, Pages: 163-177, ISSN: 0992-7689 -
Journal articleOpgenoorth HJ, Robinson R, Ngwira CM, et al., 2024,
Earth’s geomagnetic environment—progress and gaps in understanding, prediction, and impacts
, Advances in Space Research, ISSN: 0273-1177Understanding of Earth’s geomagnetic environment is critical to mitigating the space weather impacts caused by disruptive geoelectric fields in power lines and other conductors on Earth’s surface. These impacts are the result of a chain of processes driven by the solar wind and linking Earth’s magnetosphere, ionosphere, thermosphere and Earth’s surface. Tremendous progress has been made over the last two decades in understanding the solar wind driving mechanisms, the coupling mechanisms connecting the magnetically controlled regions of near-Earth space, and the impacts of these collective processes on human technologies on Earth’s surface. Studies of solar wind drivers have been focused on understanding the responses of the geomagnetic environment to spatial and temporal variations in the solar wind associated with Coronal Mass Ejections, Corotating Interaction Regions, Interplanetary Shocks, High-Speed Streams, and other interplanetary magnetic field structures. Increasingly sophisticated numerical models are able to simulate the magnetospheric response to the solar wind forcing associated with these structures. Magnetosphere-ionosphere-thermosphere coupling remains a great challenge, although new observations and sophisticated models that can assimilate disparate data sets have improved the ability to specify the electrodynamic properties of the high latitude ionosphere. The temporal and spatial resolution needed to predict the electric fields, conductivities, and currents in the ionosphere is driving the need for further advances. These parameters are intricately tied to auroral phenomena—energy deposition due to Joule heating and precipitating particles, motions of the auroral boundary, and ion outflow. A new view of these auroral processes is emerging that focuses on small-scale structures in the magnetosphere and their ionospheric effects, which may include the rapid variations in current associated with geomagnetically indu
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Conference paperStephenson P, Galand M, Deca J, et al., 2024,
Cooling of Electrons in a Weakly Outgassing Comet
<jats:p>The plasma instruments, Mutual Impedance Probe (MIP) and Langmuir Probe (LAP), part of the Rosetta Plasma Consortium (RPC), onboard the Rosetta mission to comet 67P revealed a population of cold electrons (</jats:p>
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Journal articleProvan G, Bradley T, Bunce E, et al., 2024,
Saturn&#8217;s nightside ring current during Cassini&#8217;s Grand Finale
<jats:p>During Cassini&#8217;s Grand Finale proximal orbits, the spacecraft traversed the nightside magnetotail to ~21 Saturn radii. &#160;Clear signatures of Saturn&#8217;s equatorial current sheet are observed in the magnetic field data. &#160;An axisymmetric model of the ring current is fitted to these data, amended to taken into account the tilt of the current layer by solar wind forcing, its teardrop-shaped nature and the magnetotail and magnetopause fringing fields. &#160;Variations in ring current parameters are examined in relation to external driving of the magnetosphere by the solar wind, and internal driving by the two planetary period oscillations (PPOs) and compared with dawn and dayside regimes. &#160;The relative phasing of the PPOs determines the ring current&#8217;s response to solar wind conditions. During solar wind compressions when the PPOS are in antiphase, magnetospheric storms are triggered and a thick partial ring current is formed on the nightside, dominated by hot plasma injected by tail reconnection.&#160; However, during solar wind compressions when the PPOs are in phase, the magnetosphere shows only a &#8216;minor&#8217; response and a partial ring current is not observed. During solar wind rarefactions an equatorial &#8216;magnetodisc&#8217; configuration is observed in the dayside/dawn/nightside regions, with similar total currents flowing at these local times. &#160;This partial ring current should close partly via magnetopause currents and possibly via field-aligned currents into the ionosphere. &#160;During very quiet intervals of prolonged solar wind rarefaction, a thin current sheet with an enhanced current density is formed, indicative of a ring current dominated by cool, dense, Enceladus water group ions.</jats:p>
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Conference paperStephenson P, Galand M, Deca J, et al., 2024,
Forming a cold electron population at a weakly outgassing comet
<jats:p>The Rosetta Mission rendezvoused with comet 67P/Churyumov-Gerasimenko in August 2014 and escorted it for two years along its orbit. The Rosetta Plasma Consortium (RPC) was a suite of instruments, which observed the plasma environment at the spacecraft throughout the escort phase. The Mutual Impedance Probe (RPC/MIP; Wattieaux et al, 2020; Gilet et al., 2020) and Langmuir Probe (RPC/LAP; Engelhardt et al., 2018), both part of RPC, measured the presence of a cold electron population within the coma.Newly born electrons, generated by ionisation of the neutral gas, form a warm population within the coma at ~10eV. Ionisation is either through absorption of extreme ultraviolet photons or through collisions of energetic electrons with the neutral molecules. The cold electron population is formed by cooling the newly born, warm electrons via electron-neutral collisions. Assuming the radial outflow of electrons, the cold population was only expected at comet 67P close to perihelion, where outgassing rate from the nucleus was at its highest (Q > 1028 s-1). However, cold electrons were observed until the end of the Rosetta mission at 3.8au when the outgassing was weak (Q</jats:p>
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Conference paperRothkaehl H, Andre N, Auster U, et al., 2024,
Dust, Field and Plasma instrument onboard ESA&#8217;s Comet Interceptor &#160;mission
<jats:p>The main goal of ESA&#8217;s F-1 class Comet Interceptor mission is to characterise, for the first time, a long period comet; preferably a dynamically-new or an interstellar object. The main spacecraft, will have its trajectory outside of the inner coma, whereas two sub-spacecrafts will be targeted inside the inner coma, closer to the nucleus. The flyby of such a comet &#160;will offer unique multipoint measurement opportunity to study the comet's dusty and ionised environment in ways exceeding that of the previous cometary missions, including Rosetta.&#160;The Dust Field and Plasma (DFP) instruments located on both the main spacecraft A and on the sub-spacecraft B2, is a combined experiment dedicated to the in situ, multi-point study of the multi-phased ionized and dusty environment in the coma of the target and &#160;its interaction with the surrounding space environment and the Sun.&#160;The DFP instruments will be present in different configurations on the Comet Interceptor spacecraft A and B2. To enable the measurements on spacecraft A, the DFP is composed of 5 sensors; Fluxgate magnetometer DFP-FGM-A, Plasma instrument with nanodust and E-field measurements capabilities DFP-COMPLIMENT, Electron spectrometer DFP-LEES, Ion and energetic neutrals spectrometer DFP-SCIENA &#160;and Dust detector DFP-DISC. On board of spacecraft B2 the DFP is composed of 2 sensors: Fluxgate magnetometer DFP-FGM-B2 and Cometary dust detector DFP-DISC.&#160;The DFP instrument will measure magnetic field, the electric field, plasma parameters (density, temperature, speed), the distribution functions of electrons, ions and energetic neutrals, spacecraft potential, mass, number and spatial density of cometary dust particles and the dust impacts. &#160;&#160;The full set of DFP sensors will allow to model the comet plasma environment and its interaction with the solar wind. It will also allow to describe
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Conference paperBenseguane S, Guilbert-Lepoutre A, Lasue J, et al., 2024,
A new take on the formation and evolution of circular depressions at the surface of 67P/Churyumov-Gerasimenko
<jats:p>&#160;IntroductionSome of the comets visited by spacecraft missions display some circular depressions at their surface: 81P/Wild 2 (Brownlee et al. 2004), 9P/Tempel 1 (Belton et al. 2013), 103P/Hartley 2 (Bruck Syal et al. 2013), 67P/C-G (Vincent et al. 2015). For 67P, they consist of circular holes, half holes or cliffs, with a size range of tens of meters to a few hundreds of meters (Ip et al. 2016). Owing to the high precision of the shape model obtained from the Rosetta/OSIRIS images (Preusker et al. 2015, Sierks et al. 2015), it is possible to investigate the thermal processing of 67P&#8217;s surface in relation to the formation and evolution of these features (Mousis et al. 2015, Vincent et al. 2015, Guilbert-Lepoutre et al. 2016).&#160;&#160;MethodsWe aim to investigate the formation and evolution of 67P&#8217;s circular depressions (or pits, thereafter) by thermally-induced processes (for instance sublimation and amorphous water ice crystallization) on its current orbit. In a departure from the aforementioned studies, we consider a high-resolution shape model of the nucleus, which allows to study several facets for each pit: at the bottom, and on the walls. For each facet, the complete thermal environment is considered, including self-heating and shadowing, either by neighboring facets or due to the complex global morphology of the comet. We compute the illumination, self-heating and shadowing conditions for 125k facets during a full orbit, with a time step of ~8 min, then use these conditions as an input of a 1D thermal evolution model for each facet. The model includes standard features: heat conduction, phase transitions, gas diffusion, erosion, dust mantling (De Sanctis et al. 2005, 2010, Lasue et al. 2008). Various initial setups have been considered, and many tests were conducted to assess the influence of each parameter. The behaviour of 30 circular depressions (pits, half pits and cliffs) was stud
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Journal articleCohen CMS, Leske RA, Christian ER, et al., 2024,
Observations of the 2022 September 5 Solar Energetic Particle Event at 15 Solar Radii
, ASTROPHYSICAL JOURNAL, Vol: 966, ISSN: 0004-637X -
Journal articleZank GP, Zhao L-L, Adhikari L, et al., 2024,
Characterization of Turbulent Fluctuations in the Sub-Alfvénic Solar Wind
, ASTROPHYSICAL JOURNAL, Vol: 966, ISSN: 0004-637X -
Journal articleGuo X, Wang L, Li W, et al., 2024,
Evolution of Electron Acceleration by Corotating Interaction Region Shocks at 1 au
, ASTROPHYSICAL JOURNAL LETTERS, Vol: 966, ISSN: 2041-8205 -
Journal articlePerkins O, Kasoar M, Voulgarakis A, et al., 2024,
A global behavioural model of human fire use and management: WHAM! v1.0
, Geoscientific Model Development, Vol: 17, Pages: 3993-4016, ISSN: 1991-959XFire is an integral ecosystem process and a major natural source of vegetation disturbance globally. Yet at the same time, humans use and manage fire in diverse ways and for a huge range of purposes. Therefore, it is perhaps unsurprising that a central finding of the first Fire Model Intercomparison Project was simplistic representation of humans is a substantial shortcoming in the fire modules of dynamic global vegetation models (DGVMs). In response to this challenge, we present a novel, global geospatial model that seeks to capture the diversity of human–fire interactions. Empirically grounded with a global database of anthropogenic fire impacts, WHAM! (the Wildfire Human Agency Model) represents the underlying behavioural and land system drivers of human approaches to fire management and their impact on fire regimes. WHAM! is designed to be coupled with DGVMs (JULES-INFERNO in the current instance), such that human and biophysical drivers of fire on Earth, and their interactions, can be captured in process-based models for the first time. Initial outputs from WHAM! presented here are in line with previous evidence suggesting managed anthropogenic fire use is decreasing globally and point to land use intensification as the underlying reason for this phenomenon.
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Journal articleToledo-Redondo S, Lee JH, Vines SK, et al., 2024,
Statistical Observations of Proton-Band Electromagnetic Ion Cyclotron Waves in the Outer Magnetosphere: Full Wavevector Determination
, JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 129, ISSN: 2169-9380 -
Journal articleDe Keyser J, Edberg NJT, Henri P, et al., 2024,
In situ plasma and neutral gas observation time windows during a comet flyby: Application to the Comet Interceptor mission
, PLANETARY AND SPACE SCIENCE, Vol: 244, ISSN: 0032-0633 -
Journal articleLewis ZM, Beth A, Galand M, et al., 2024,
Constraining ion transport in the diamagnetic cavity of comet 67P
, Monthly Notices of the Royal Astronomical Society, Vol: 530, Pages: 66-81, ISSN: 0035-8711The European Space Agency Rosetta mission escorted comet 67P for a 2-yr section of its six and a half-year orbit around theSun. By perihelion in 2015 August, the neutral and plasma data obtained by the spacecraft instruments showed the comet hadtransitioned to a dynamic object with large-scale plasma structures and a rich ion environment. One such plasma structure isthe diamagnetic cavity: a magnetic field-free region formed by interaction between the unmagnetized cometary plasma andthe impinging solar wind. Within this region, unexpectedly high ion bulk velocities have been observed, thought to have beenaccelerated by an ambipolar electric field. We have developed a 1D numerical model of the cometary ionosphere to constrainthe impact of various electric field profiles on the ionospheric density profile and ion composition. In the model, we includethree ion species: H2O+, H3O+, and NH+4 . The latter, not previously considered in ionospheric models including acceleration, isproduced through the protonation of NH3 and only lost through ion–electron dissociative recombination, and thus particularlysensitive to the time-scale of plasma loss through transport. We also assess the importance of including momentum transferwhen assessing ion composition and densities in the presence of an electric field. By comparing simulated electron densities toRosetta Plasma Consortium data sets, we find that to recreate the plasma densities measured inside the diamagnetic cavity nearperihelion, the model requires an electric field proportional to r−1 of around 0.5–2 mV m−1 surface strength, leading to bulk ionspeeds at Rosetta of 1.2–3.0 km s−1.
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Journal articleZhou Y, He F, Archer MO, et al., 2024,
Spatial evolution characteristics of plasmapause surface wave during a geomagnetic storm on 16 July 2017
, Geophysical Research Letters, Vol: 51, ISSN: 0094-8276Boundary dynamics are crucial for the transport of energy, mass, and momentum in geospace. The recently discovered plasmapause surface wave (PSW) plays a key role in the inner magnetosphere dynamics. However, a comprehensive investigation of spatial variations of the PSW remains absent. In this study, we elucidate the spatial characteristics of a PSW through observations from multiple spacecrafts in the magnetosphere. Following the initiation of the PSW, quasi-periodic injections of energetic ions, rather than electrons, are suggested to serve as energy source of the PSW. Based on the distinct wave and particle signatures, we categorize the PSW into four regions: seed region, growth region, stabilization region and decay region, spanning from nightside to afternoon plasmapause. These findings advance our understanding of universal boundary dynamics and contribute to a deeper comprehension of the pivotal roles of surface waves in the energy couplings within the magnetosphere-plasmasphere-ionosphere system.
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ReportZachariah M, Kimutai J, Barnes C, et al., 2024,
Heavy precipitation hitting vulnerable communities in the UAE and Oman becoming an increasing threat as the climate warms
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Journal articleSparks N, Toumi R, 2024,
The Imperial College Storm model (IRIS) dataset
, Scientific Data, Vol: 11, ISSN: 2052-4463Assessing tropical cyclone risk on a global scale given the infrequency of landfalling tropical cyclones (TC) and the short period of reliable observations remains a challenge. Synthetic tropical cyclone datasets can help overcome these problems. Here we present a new global dataset created by IRIS, the ImpeRIal college Storm model. IRIS is novel because, unlike other synthetic TC models, it only simulates the decay from the point of lifetime maximum intensity. This minimises the bias in the dataset. It takes input from 42 years of observed tropical cyclones and creates a 10,000 year synthetic dataset of wind speed which is then validated against the observations. IRIS captures important statistical characteristics of the observed data. The return periods of the landfall maximum wind speed are realistic globally.
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Journal articleBlackford K, Kasoar M, Burton C, et al., 2024,
INFERNO-peat v1.0.0: a representation of northern high latitude peat fires in the JULES-INFERNO global fire model
, Geoscientific Model Development, Vol: 17, Pages: 3063-3079, ISSN: 1991-959XPeat fires in the northern high latitudes have the potential to burn vast amounts of carbon-rich organic soil, releasing large quantities of long-term stored carbon to the atmosphere. Due to anthropogenic activities and climate change, peat fires are increasing in frequency and intensity across the high latitudes. However, at present they are not explicitly included in most fire models. Here we detail the development of INFERNO-peat, the first parameterization of peat fires in the JULES-INFERNO (Joint UK Land Environment Simulator INteractive Fire and Emission algoRithm for Natural envirOnments) fire model. INFERNO-peat utilizes knowledge from lab and field-based studies on peat fire ignition and spread to be able to model peat burnt area, burn depth, and carbon emissions, based on data of the moisture content, inorganic content, bulk density, soil temperature, and water table depth of peat. INFERNO-peat improves the representation of burnt area in the high latitudes, with peat fires simulating on average an additional 0.305×106 km2 of burn area each year, emitting 224.10 Tg of carbon. Compared to Global Fire Emissions Database version 5 (GFED5), INFERNO-peat captures ∼ 20 % more burnt area, whereas INFERNO underestimated burning by 50 %. Additionally, INFERNO-peat substantially improves the representation of interannual variability in burnt area and subsequent carbon emissions across the high latitudes. The coefficient of variation in carbon emissions is increased from 0.071 in INFERNO to 0.127 in INFERNO-peat, an almost 80 % increase. Therefore, explicitly modelling peat fires shows a substantial improvement in the fire modelling capabilities of JULES-INFERNO, highlighting the importance of representing peatland systems in fire models.
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Journal articleDing M, Ryabtsev AN, Kononov EY, et al., 2024,
Spectrum and energy levels of the low-lying configurations of Nd III
, ASTRONOMY & ASTROPHYSICS, Vol: 684, ISSN: 0004-6361 -
Journal articleColomban L, Kretzschmar M, Krasnoselkikh V, et al., 2024,
Quantifying the diffusion of suprathermal electrons by whistler waves between 0.2 and 1 AU with Solar Orbiter and Parker Solar Probe
, ASTRONOMY & ASTROPHYSICS, Vol: 684, ISSN: 0004-6361 -
Journal articleMathews J, Czaja A, 2024,
Oceanic maintenance of atmospheric blocking in wintertime in the North Atlantic
, CLIMATE DYNAMICS, ISSN: 0930-7575 -
Journal articleHellinger P, Verdini A, Montagud-Camps V, et al., 2024,
Anisotropy of plasma turbulence at ion scales: Hall and pressure-strain effects
, ASTRONOMY & ASTROPHYSICS, Vol: 684, ISSN: 0004-6361 -
Journal articleChawner H, Saboya E, Adcock KE, et al., 2024,
Atmospheric oxygen as a tracer for fossil fuel carbon dioxide: a sensitivity study in the UK
, Atmospheric Chemistry and Physics, Vol: 24, Pages: 4231-4252, ISSN: 1680-7316We investigate the use of atmospheric oxygen (O2) and carbon dioxide (CO2) measurements for the estimation of the fossil fuel component of atmospheric CO2 in the UK. Atmospheric potential oxygen (APO) – a tracer that combines O2 and CO2, minimizing the influence of terrestrial biosphere fluxes – is simulated at three sites in the UK, two of which make APO measurements. We present a set of model experiments that estimate the sensitivity of APO simulations to key inputs: fluxes from the ocean, fossil fuel flux magnitude and distribution, the APO baseline, and the exchange ratio of O2 to CO2 fluxes from fossil fuel combustion and the terrestrial biosphere. To estimate the influence of uncertainties in ocean fluxes, we compare three ocean O2 flux estimates from the NEMO–ERSEM, the ECCO–Darwin ocean model, and the Jena CarboScope (JC) APO inversion. The sensitivity of APO to fossil fuel emission magnitudes and to terrestrial biosphere and fossil fuel exchange ratios is investigated through Monte Carlo sampling within literature uncertainty ranges and by comparing different inventory estimates. We focus our model–data analysis on the year 2015 as ocean fluxes are not available for later years. As APO measurements are only available for one UK site at this time, our analysis focuses on the Weybourne station. Model–data comparisons for two additional UK sites (Heathfield and Ridge Hill) in 2021, using ocean flux climatologies, are presented in the Supplement. Of the factors that could potentially compromise simulated APO-derived fossil fuel CO2 (ffCO2) estimates, we find that the ocean O2 flux estimate has the largest overall influence at the three sites in the UK. At times, this influence is comparable in magnitude to the contribution of simulated fossil fuel CO2 to simulated APO. We find that simulations using different ocean fluxes differ from each other substantially. No single model estimate, or a model estimate that assumed zero oce
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Journal articleHuang J, Kasper JC, Larson DE, et al., 2024,
Parker Solar Probe Observations of High Plasma β Solar Wind from the Streamer Belt (vol 265, 47, 2023)
, ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 271, ISSN: 0067-0049
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