The reconstruction of Mercury’s internal magnetic field enables us to take a look into the inner heart of Mercury. In view of the BepiColombo mission, Mercury’s magnetosphere is simulated using a hybrid plasma code, and the
multipoles of the internal magnetic field are estimated from the virtual spacecraft data using three distinct reconstruction methods: the truncated singular value decomposition, the Tikhonov regularization and Capon’s minimum variance projection. The study shows that a precise determination of Mercury’s internal field beyond the octupole up to the dotriacontapole (fifth degree of the multipole expansion) is possible. Especially, Capon’s method provides the most accurate inversion result compared to the Tikhonov regularization and the truncated singular value decomposition.

How to cite: Töpfer, S., Oertel, I., Schiron, V., Narita, Y., Glassmeier, K.-H., Heyner, D., Kolhey, P., and Motschmann, U.: Reconstruction of Mercury’s internal magnetic field beyond the octupole, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-1159, https://doi.org/10.5194/egusphere-egu23-1159, 2023.

At least four spacecraft are essential to investigate physical processes in space plasmas. CLUSTER was the first four-spacecraft mission orbiting the Earth, during its life time the size of the tetrahedron has been adjusted between hundred to thousands of kilometers accordingly to various scientific objectives. The size of MMS, the second four-spacecraft mission, is smaller. In the barycentric formalism [1, chapter 14] reciprocal vectors of the tetrahedron play a prominent role for estimating field gradients and analysing the propagation of waves or discontinuities. The method of least squares [1, chapter 12] underlines also the importance of the reciprocal vectors and both methods are identical  for four spacecraft [1, chapter 15], nevertheless, meanwhile the barycentric approach is restricted to four spacecraft, the least squares approach is applicable to any number N of spacecraft, and more, weighted least squares offer a possibility of optimization. Generalized reciprocal vectors for N spacecraft with arbitrary weights have been defined [2] and it was announced [3] that gradients of fields estimated from CLUSTER or MMS observations could be improved by an appropriate choice of weights ; this is wrong, we hereby demonstrate that for N=4 the estimated gradient of a vector field is independant of the weights. This unfortunate false announcement was due to a programming error: an erratum has been recently presented [4]. Discriminating between synchronous and asynchronous measurements by the constellation helps clarifying the tools and their uses. Synchronous data which gather observations of the same vector field by all spacecraft at the same time are used to estimate the spatial gradient of the field, meanwhile asynchronous data gathering observations of the same field made by the spacecraft at different times are used to estimate wave vectors or the propagation of discontinuities. The generalized synchronous position tensor R1, built from the vertices of the constellation, is introduced to analyze synchronous data, meanwhile the generalized asynchronous position tensor R2, built from the couples of vertices of the constellation, is introduced to analyze asynchronous data. It worth noticing that the synchronous analysis can be optimized only for N > 4 and by contrast the asynchronous analysis for any number N of spacecraft. The corresponding generalized synchronous and asynchronous reciprocal vectors q are defined by applying the inverses Q1 and Q2 of R1 and R2 to the position vectors, and their properties are demonstrated. We also give in tensor form the estimated gradient of a vector field satisfying the solenoidal condition, initially given by components in[1, chapter 12] and we discuss briefly the aliasing of waves by the constellation, initially adressed for a tetrahedron in [1, chapter 14].

References

• Analysis Methods for Multi-Spacecraft Data, ISSI Scientific Report SR-001, Eds. G. Paschmann and P.W. Daly, 1998.
• Multi-Spacecraft Analysis Methods Revisited, ISSI Scientific Report SR-008, Eds. G. Paschmann and P.W. Daly, 2008.
• Chanteur, G.M., Abstract D3.2-0004-18 Optimal Field Gradients Derived From Multi-Spacecraft Observations, Scientific Assembly Abstracts, p1243, COSPAR 2018 Pasadena, California, USA.
• Chanteur, G.M., CLUSTER 22nd Birthday Workshop, November 7- 11, 2022, ESOC, Darmstadt, Germany

How to cite: Chanteur, G. M.: Reciprocal Vectors of an Arbitrary Constellation of Spacecraft for Estimating Gradients and Wave Vectors, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-4486, https://doi.org/10.5194/egusphere-egu23-4486, 2023.

We explore relationship between the interplanetary magnetic field configuration and the direction of the solar wind flow analyzing few substorm onset lists, produced by different methods over the few years.  We investigate the impact of upstream conditions, such as the interplanetary magnetic field (IMF) configuration and  the changing direction of the solar wind flow on the occurrence of substorms by using substorm onset lists between time1-time2. Large directional changes in the solar wind flow can result in large-scale windsock motions and current sheet thinnings forcing magnetic reconnection to occur in magnetospheric tail, which consequently can lead to substorm onset. Magnetic reconnection is a process, which can explain fast and energetic releases of plasmas in the tail during southward oriented IMF, leading to energetic substorms. However, it is more difficult to explain substorms which are associated with northward oriented IMF. Here we aim to analyse substorms associated with northward oriented IMF with the additional challenge to understand whether the substorm onsets are externally triggered by some upstream conditions or internally initiated by some instabilities in the magnetotail, observed for example during northward oriented interplanetary magnetic field i.e. in the time when there is no significant flux transfer. For our analysis we use concurrent OMNI data of solar wind, substorm databases, Geotail, THEMIS satellite data and ground base data.

How to cite: Saxonbergová, D. and Vörös, Z.: A statistical study: Relations Between the Directional Changes in Solar Wind Flow and Magnetotail Response, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-6231, https://doi.org/10.5194/egusphere-egu23-6231, 2023.

Flux Transfer Events (FTEs) are transient phenomena generated at the dayside magnetopause as a result of magnetic reconnection. FTEs have a significant role in the transfer of momentum and energy into the magnetosphere. We study here, in a multifluid framework, how the energy is converted within FTEs and their surrounding plasma. In particular we investigate how the plasma gains or loses kinetic energy through electric and/or pressure gradient terms. We also investigate the terms that control how the internal energy of the plasma is gained or dissipated through the pressure work term. Using observations from Magnetospheric MultiScale (MMS), we perform a statistical study based on an existing FTE catalog (Fargette et al., 2020). We analyze FTEs with or without internal current sheets. We discuss the contribution of the different terms in the energy conversion process separately for ions and electrons and as a function of location within the FTE. We analyze and compare the results found for FTEs’ intervals with magnetosheath intervals (Wang et al. 2021), taking into account their locations, using probability distribution functions of the various energy terms measured in each interval. This work contributes to a better understanding of energy conversion processes associated with FTEs at the magnetopause.

How to cite: Dahani, S., Lavraud, B., Génot, V., Toledo-Redondo, S., Kieokaew, R., Fargette, N., Gershman, D., Giles, B., Torbert, R., and Burch, J.: Energy Conversion Associated with Flux Transfer Events at Earth’s Magnetopause, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-7257, https://doi.org/10.5194/egusphere-egu23-7257, 2023.

The presence of a velocity shear layer in a plasma can lead to the development of the Kelvin-Helmholtz instability (KHI). KHI is characterised by the growth of waves that roll up to form non-linear vortices. An example of such velocity shear layer is found at either flank of Earth's magnetopause, where KHI acts a driver of mass and energy transfer from the solar wind into the magnetosphere. Within the rolled-up vortices, kinetic length scales may be attained, allowing vortex-induced magnetic reconnection and kinetic-scale diffusion to operate. In the present study, we have considered the realistic case of a density/temperature jump across the magnetopause and modelled the development of the KHI using a local hybrid-Vlasov simulation with the Vlasiator code. For a case with a northward directed magnetic field, we find that an enhanced ion heat flux arises at vortex boundaries whose thickness approaches the ion gyroscale. Furthermore, the direction of the heat flux vector closely follows the direction of the vortex boundary tangent vector. As such, this signature could provide observational evidence of ion diffusion occurring within KHI, and also information on vortex boundary geometry with single spacecraft data. To validate our results, we compare our simulation run with data from the Magnetospheric Multiscale Mission.

How to cite: Tarvus, V., Turc, L., Zhou, H., Cozzani, G., Ganse, U., Pfau-Kempf, Y., Alho, M., Battarbee, M., Dubart, M., George, H., Horaites, K., Suni, J., Tesema, F., Zaitsev, I., and Palmroth, M.: Ion heat flux associated with the Kelvin-Helmholtz instability in a non-uniform plasma: Numerical hybrid-Vlasov results, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-8390, https://doi.org/10.5194/egusphere-egu23-8390, 2023.

The energy of particles in the Earth's magnetosphere changes significantly when the configuration of the magnetic field lines suddenly changes from stretched to more dipolar (dipolarization). Energy changes can be caused by variation in electric fields,  due to the generation of electrostatic waves, etc. The presence of heavy ions at the heights of the magnetosphere significantly changes the physics of the processes since, in addition to changing the main characteristics of the plasma (temperature, pressure, Alfven velocity thickness of the current/plasma layer), the conditions and rate of development of instabilities (in particular, the Kelvin-Helmholtz instability) and the nature of turbulent processes will change as well.

In this work, the change of ion and electron fluxes is considered and the peculiarities of resonant interaction of charged particles with electromagnetic fluctuations during the dipolarizations are determined.

The data from the Cluster-II mission spacecraft (magnetic field measurements from ferroelectrode magnetometers (FGM) and energetic particle fluxes from RAPID spectrometers) were used for the analysis. The analysis of individual events is carried out, and a statistical consideration of changes in particle fluxes during magnetic field dipolarizations for 2001–2015 is presented.

Among the features of proton fluxes for individual events, an non-correlation between flux changes in different energy channels is recorded (example, the flux at 27 keV is approximately constant, and is peaks in higher energy ranges). Thus, we have a selective non-adiabatic acceleration of a part of a proton spectrum depending on energy. The change of the spectral index for different energy channels and components was studied.

The values of the power of magnetic field oscillations at gyrofrequencies for different ion types obtained by epoch superposition method showed that resonant interactions of ions with low-frequency electromagnetic waves are more significant for "heavier" components. Therefore the ions can effectively be accelerated by the interaction with these waves during the dipolarization.

This work was supported by the grant no. 97742 of the Volkswagen Foundation (VW-Stiftung), the Royal Society International Exchanges Scheme 2021 IES\R1\211177, and BF/30-2021.

How to cite: Kozak, L., Petrenko, B., Kronberg, E., Akhmetshyn, R., and Ballai, I.: Wave-particle interactions in the Earth magnetotail during dipolarization, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-8439, https://doi.org/10.5194/egusphere-egu23-8439, 2023.

The Interstellar Boundary Explorer (IBEX) mission continues to provide energetic neutral atom (ENA) observations of the heliosphere and Earth’s magnetosphere from a global perspective and including spatial, temporal, and energy information. Due to its orbit, IBEX routinely observes the magnetosphere from a side-viewing vantage point, with a field-of-view that is nearly perpendicular to the day-night plane. This enables the construction of composite ENA images at different energies (0.5 – 6.0 keV) for convected solar wind conditions, which provides global insights into different magnetospheric plasma regions and processes.

Earth’s plasma sheet plays a crucial role in the global circulation of plasma throughout the magnetosphere. The structure of the plasma sheet is driven by a combination of effects including interplanetary magnetic field (IMF) and solar wind conditions, internal magnetospheric processes, and Earth’s dipole tilt angle.

This work examines the structure of the plasma sheet in the X-Z geocentric ecliptic plane (GSE) using ENA images from IBEX. The thickness and extent of the plasma sheet is compared for conditions of prolonged northward and southward IMF. We report on a North-South asymmetry in the plasma sheet that is related to the IMF orientation and is driven by a combination of dayside magnetic reconnection effects and high dipole tilt. Results provide evidence of dayside reconnection driving plasma sheet dynamics.

How to cite: Dayeh, M. A., Starkey, M. J., Petrinec, S. M., Fuselier, S. A., Sokół, J. M., Ogasawara, K., Szalay, J. R., McComas, D. J., Zirnstein, E. J., and Schwadron, N. A.: Asymmetry in the Terrestrial Plasma Sheet Driven by Dayside Dynamics, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-9371, https://doi.org/10.5194/egusphere-egu23-9371, 2023.

A. M. Benedito Nunes (co-first author), J. Gamper (co-first author), M. Friel, J. W. Gjerloev, S.C. Chapman

The Newcomb-Benford Law (NBL) prescribes the probability distribution of the first digit of variables under conditions including aggregation. It will not apply where there is strong truncation or a cut-off. We apply it to space weather relevant magnetic field observations and indices for the first time. In upstream solar wind magnetic field OMNI HRO IMF observations we show that the NBL detects the improvement in data quality with the availability of the WIND and later, ACE spacecraft after 1995, in addition to IMP8. The SMR geomagnetic index averages over multiple ground magnetometer time-series and follows the NBL to a consistent high precision across changing solar activity and a ten-fold increase in the number of constituent stations. The AE and SME indices select the extremal signals from a set of stations. AE, which is mostly based on the same stations throughout its record, follows the NBL to a consistent high precision and with weak but statistically significant variation, it follows the NBL less well during relatively strong solar cycle maxima compared to solar minima. Both the number of constituent stations and the station type comprising SME has changed over the SME record. First, in 1996 the number of available stations increased tenfold, but the station type remained homogeneous. The NBL is followed to a consistent high precision through this period, up to 2006. Beyond 2006, new station types are introduced into the composition of SME and this can be seen in an approximately factor of two drop in the precision with which the NBL is followed. Subsequently, the SME record follows the NBL to varying precision which tracks the inclusion and omission of different types of magnetometer in the record. As the use of composite indices becomes more widespread across the geosciences, the NBL may therefore provide a generic 'data flag' to indicate when the constituent raw data, calibration or sampling method has changed.

How to cite: Benedito Nunes, A., Gamper, J., Friel, M., Gjerloev, J., and Chapman, S.: Newcomb-Benford Law characterization of solar wind magnetic field and geomagnetic indices, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-9727, https://doi.org/10.5194/egusphere-egu23-9727, 2023.

We search for ESA’s Cluster and NASA’s MMS missions’ simultaneous observations of the Earth’s magnetosheath (MSH) region. Visual inspection of Cluster quicklook plots is used to determine Cluster-MSH crossings. Next, MMS quicklook plots are inspected, and the MMS-MSH crossings which overlap in time with the Cluster-MSH intervals from step 1, are catalogued. We find 117 simultaneous crossings in 2017-2021. Our overall goal is to investigate the correlation between the properties of the magnetosheath and the bow shock (BS) characteristics. Thus, for each one of the MSH intervals in our catalogue, we determine the BS characteristics. The Earth’s bow shock can be classified as either quasi-parallel or quasi-perpendicular, depending on the angle between the interplanetary magnetic field (IMF) and bow shock normal direction. We use OMNI data to determine the IMF direction, and we estimate the BS normal direction using two approaches: (1) from magnetic field measurements using minimum variance analysis and (2) from a bow shock model using solar wind data as input. We will present our catalogue of simultaneous Cluster-MMS magnetosheath crossings, and also our estimates for the BS type associated with each crossing.

How to cite: Munteanu, C., Teodorescu, E., and Echim, M.: Cluster and MMS simultaneous observations of the Earth’s magnetosheath region in 2017-2021, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-11179, https://doi.org/10.5194/egusphere-egu23-11179, 2023.

Ultra-low frequency (ULF) waves in the Earth’s magnetosphere are commonly observed in space as well as on the ground stations. Located between the magnetosphere and the earth’s surface, the lower-thermosphere-ionosphere region is expected to be abundant in ULF waves. Transverse Alfven waves are of interest since they have one-dimensional nature along the magnetic field lines with radial variation in their characteristic frequencies. We have conducted three-dimensional magnetohydrodynamic wave simulations to investigate ULF observations by various types of low-Earth orbit (LEO) satellites. Virtual spacecraft are embedded in our model to measure electromagnetic wave signals as they move at different altitudes and latitudes. Our results present that the waveform and frequency of transverse waves change significantly when they are observed in low Earth orbit. Since the majority of LEO satellites lay in polar orbit, they traverse different field lines at relatively high speeds. Thus, fast movement through Alfven speed gradient along the spacecraft trajectory alters the frequency of transverse Alfven waves. It is worth noting that the observed frequency by virtual satellites in low-Earth orbit becomes ~8 times higher than the original frequency. It indicates that frequency distortion from LEO satellite observations can cause serious differences between ground-based and satellite observations. We suggest validating ULF wave observations in low-Earth orbit using a series of spacecraft such as the CubeSat constellation can improve the robustness of electromagnetic field measurements in LEO.

How to cite: Choi, J., Lee, D.-H., Min, K., Yoon, K., and Park, J. U.: Validating in-situ measurements of ULF Waves in Low Earth Orbit, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-12182, https://doi.org/10.5194/egusphere-egu23-12182, 2023.

In situ observations revealed both linear and non-linear signatures of the kinetic (electron) ballooning-interchange instability (BICI) operating in the Earth’s magnetotail, which appear to drive auroral beads and pseudo-breakups in the ionosphere. Observation of the magnetotail configurations with inversed gradient of the vertical magnetic field, which is believed to drive the BICI is challenged by sparse spacecraft coverage. We use the adapted modeling based on in situ spacecraft observations, and low-altitude particle observations to extract some information on such magnetotail configurations. We present two in situ events with both linear and non-linear BICI development signatures and compare the magnetotail configurations during the two events using the two methods.

How to cite: Panov, E. V., Kubyshkina, M. V., Sergeev, V. A., Nakamura, R., and Baumjohann, W.: Magnetotail configurations during ballooning-interchange instability signatures, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-12541, https://doi.org/10.5194/egusphere-egu23-12541, 2023.

On 28th of August 2018 at 5:30 UT, MMS and Cluster were located in the magnetotail at about 16 earth radii (RE). They both suddenly crossed plasma interfaces. Located near the post midnight sector, Cluster transitioned from a cold plasma sheet to a hot plasma sheet associated with a quasi-parallel earthward flow 800 km/s whereas MMS, located at 4 RE duskward of Cluster, transitioned from a similar cold plasma sheet to the lobe region via a very short period in a hot plasma sheet associated with a vortex-like signature. At 05:50 UT MMS returned to a hot plasma sheet and also detected a quasi-parallel earthward flow ~ 400 km/s and increased energetic ion and electron fluxes. We use measurements from both missions during this conjunction to describe the possible large scale dynamics of the magnetotail as well as some associated kinetic processes. Energetic particle (>50keV) measurements from the two missions are compared. Furthermore, at ion scales, we investigate the possible role of ion fire-hose instability in the plasma flow reduction. At electron scales, we analyze fast and slow non linear electrostatic waves propagating tailward which are detected in the so called electron boundary layer as well as in the hot plasma sheet. We discuss their possible generation mechanisms and link with the large scale dynamics of the magnetotail.

How to cite: Le Contel, O., Retino, A., Chust, T., Steinvall, K., Alqeeq, S., Baraka, M., Canu, P., Fontaine, D., Mirioni, L., Dandouras, I., Carr, C., Toledo-Redondo, S., Fazakerley, A., Doss, N., Daly, P., Kiehas, S., Nakamura, R., Khotyaintsev, Y., Wilder, F., and Ahmadi, N. and the Joint Cluster/MMS team: Study of kinetic processes based on MMS/Cluster joint measurements in the vicinity of the plasma sheet boundary layer, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-12580, https://doi.org/10.5194/egusphere-egu23-12580, 2023.

Models of the geospace plasma environment have been proceeding towards more realistic descriptions of the solar wind—magnetosphere interaction, from gas-dynamic to MHD and hybrid ion-kinetic models such as the state-of-the-art Vlasiator model. Advances in computational capabilities have enabled global simulations of detailed physics, with some inroads to electron physics made with eVlasiator, specifically, in a meridional 2D+3V simulation.

In this work we present preliminary results from eVlasiator, an offshoot of the Vlasiator model, showing results from a global 3D+3V kinetic electron geospace simulation. Previous work in a spatially 2D environment has shown, despite truncation of some electron physics and use of ion-scale spatial resolution, that realistic electron distribution functions are obtainable within the magnetosphere. This work examines the differences between the spatially 2D and the new spatially 3D results, and describe these in relation to MMS observations. Electron precipitation to the upper atmosphere from these velocity distributions is estimated.

How to cite: Alho, M., Battarbee, M., Kotipalo, L., Grandin, M., Pfau-Kempf, Y., Ganse, U., Cozzani, G., Bussov, M., Gordeev, E., Horaites, K., Kebede, F. T., Papadakis, K., Suni, J., Tarvus, V., Turc, L., Zaitsev, I., Zhou, H., and Palmroth, M.: Global simulation of geospace electrons: eVlasiator in 3D, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-13452, https://doi.org/10.5194/egusphere-egu23-13452, 2023.

Kinetic Alfvén wave (KAW) is the kinetic extension of shear Alfvén wave (SAW) where the perpendicular wavelength with respect to the magnetic field becomes comparable to the ion scale. It has been suggested theoretically that mode conversion from incident compressional waves to KAWs at the magnetopause leads to the plasma transport. Existence of KAWs has been identified from in-situ observations and shown to be closely related to the Hall field from magnetic reconnection. In this study, we investigate the properties of KAWs using the hybrid-Vlasov model Vlasiator. Local runs of tangential discontinuities with parameters relevant to Earth’s magnetopause are performed to look at the mode conversion from fast waves to Alfvén waves. Signatures of KAWs are identified from both local and global simulations, which provide insights into the nonlinear plasma transport process in the magnetosphere.

How to cite: Zhou, H., Turc, L., Cozzani, G., Zaitsev, I., Pfau-Kempf, Y., Horaites, K., Kebede, F., Battarbee, M., Alho, M., Grandin, M., Gordeev, E., Tarvus, V., Dubart, M., Suni, J., Papadakis, K., Ganse, U., and Palmroth, M.: Kinetic Alfvén waves from hybrid-Vlasov simulations, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-13756, https://doi.org/10.5194/egusphere-egu23-13756, 2023.

A COnstellation of Radiation BElt Survey (CORBES) program is proposed by the Sub-Group on Radiation Belt (SGRB) of TGCSS, COSPAR, which is in pursuit of the goal of SGRB, focusing on the implementation of a Small/CubeSats constellation mission for radiation belt exploration. Basing on a general review of the status quo of research on the Earth’s radiation belts dynamics and the unresolved scientific issues, the scientific object and observation requirements of CORBES are proposed. The CORBES program is expected to have a constellation of 10-plus small/ CubeSats to take an ultra-fast survey of the Earth’s radiation belt. The general science goal for CORBES is to investigate two groups of physical processes related to the radiation belts: wave-particle interactions and radial transport. This program is an international multilateral cooperation mission, an open and sharing data policy will be implemented. The data set of observations will be shared within the contributors of the constellation and the broad research community at large, then would be of great use for comprehensively understanding the dynamics of magnetospheric energetic populations and developing more standard models of the Earth’s radiation belts. Furthermore, from the application perspective, the ultra-fast survey of the radiation belt could serve as an important facility for monitoring space weather of the Earth as well.

How to cite: Yang, X., Dai, L., Wu, J., Li, W., Miyoshi, Y., Nakamura, R., Palmroth, M., Ebrahimi, M., Deng, L., and Li, Y.: Constellation of radiation belts survey (CORBES) a COSPAR small satellite constellation survey program for Earth’s radiation belt, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-7205, https://doi.org/10.5194/egusphere-egu23-7205, 2023.

We created a database of over 100 simulations of geomagnetic storms from the time interval from 2010 to 2019, using the Geospace configuration of the Space Weather Modeling Framework. With this data set, we explore and quantify the errors that arise from the uncertainties of the input solar wind data set that comes from the OMNI database, using global magnetic indices such as SYM-H, AL and Cross Polar Cap Potential as measures of the model output that can be directly compared with observations. Our results show that the method of propagation of the solar wind data from the spacecraft location near L1 to the bow shock nose causes errors that are much smaller than those arising from the limitations in modeling the solar wind – magnetosphere – ionosphere coupling processes during strong solar wind driving. We devise a method to quantify these uncertainties, which may become useful in understanding the output of global simulations. These results will be useful as well for research investigations of magnetospheric processes as well as for forecasting space weather.

How to cite: Al Shidi, Q., Pulkkinen, T., and Welling, D.: Uncertainty Quantification in Global Simulations: Solar Wind Propagation Effects, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-11764, https://doi.org/10.5194/egusphere-egu23-11764, 2023.