In order to improve the predictions of the ambient solar wind plasma at planets, moons, comets, and interplanetary spacecraft, we are conducting a multi-spacecraft investigation to study the spatial variation and temporal evolution of solar wind structures. Here we present our results on the spatial variation by investigating the impact of latitudinal spacecraft-target separation on extrapolation accuracy. Using ballistically propagated bulk velocity datasets of the ACE, STEREO A, Parker Solar Probe, and Solar Orbiter spacecraft, we perform statistical analyses and case studies. Our findings indicate that a separation of even a few degrees in latitude can introduce errors into propagation accuracy and needs to be taken into account when incorporating in-situ measurements into solar wind forecasting. We further investigate the role of the heliospheric current sheet in this phenomenon by utilizing coronal modeling. The results are useful in supporting out-of-ecliptic solar wind observations and for the improvement of propagation models.

Solar wind parameters at different locations in the inner heliosphere can be estimated using various solar wind extrapolation methods. The simple ballistic method extrapolates solar wind parameters from the point of measurement to a chosen heliospheric position by assuming that major solar wind structures are persistent and arrive relatively unaltered to the target position. The method considers the rotation period of the Sun while assuming a constant solar wind speed during radial propagation. We improve the simple ballistic model by considering the interaction between the slow and the fast solar wind with a pressure correction during the propagation. Instead of extrapolating from the position of a single spacecraft, we apply this pressure-corrected ballistic method to 2D speed maps of the solar source surface available from solar coronal models to determine the solar wind speed in the inner heliosphere in 3D, between latitudes of ±50°. We also take into account the effects of the solar differential rotation in our model. Our method is simple and fast, and it can be applied to different source surface datasets. The results of our model are validated with in situ data from the ACE spacecraft. We find that the pressure-corrected ballistic method can give accurate predictions of the solar wind in 3D.

The Rosetta spacecraft observed the temporal evolution of the ion populations within the ionosphere of comet 67P/Churyumov-Gerasimenko. A striking feature of the ion spectrum is represented by the so-called medium-energy ion peaks, which recurrently emerge from the low-energy ion background with their energy levels typically reaching 50 to 1000 eV before their energy gradually decreases, and they disappear from the measurements. These peaks are believed to be caused by space weather forcing, but there was no conclusive evidence until now. We investigated the characteristics of these ions, paying special attention to the connection between the solar wind dynamic pressure and the amount and energy of the medium-energy ions. Our findings reveal a strikingly accurate direct correlation between the dynamic pressure of the solar wind at the position of the comet and the amount of medium-energy ions measured by Rosetta. The ion energy also unquestionably reacts to the effects of solar wind pressure variation, but this parameter is strongly affected by the production rate and the distance from the nucleus as well. We explain these close correlations between cometary ion and solar wind characteristics using the well-founded assumption that certain boundary layers of the magnetosphere can move in and out under the influence of higher and lower solar wind pressure.

Context. Directional discontinuities (DDs) are common structures in the solar wind plasma and are among the most important discontinuities besides shock waves. The Parker Solar Probe and Solar Orbiter spacecraft currently provide whole new insight into the inner heliosphere in spatial coverage and timescales. Aims. We search for DDs and classify them into subgroups of tangential (TD) and rotational (RD) discontinuities. The analysis of the DD thicknesses allows us to test different theories about their origin and evolution. Methods. We applied an automatic algorithm to select discontinuities between heliocentric distances of 0.06-1.01 AU. The method uses the spatial rotation of the magnetic field to identify the DDs and minimum variance analysis to determine the normal vector of the discontinuity surface. A classification into TDs and RDs was carried out using the magnetic field data and the Walen test in both the spacecraft and the deHoffmann-Teller frame. Results. With strict conditions, we found more than 140 000 DDs in the time intervals. We find that the spatial density of DDs decreases with increasing radial distance from the Sun in the innermost heliosphere. The comprehensive analysis revealed that most of the DD, for which the normal component of the magnetic field is small are in fact TDs, regardless of the jump in field magnitude. After the classification, we were able to determine the radial thickness evolution for the TDs and RDs separately. We found that the thickness of RDs decreases from 0.06 to 0.30 AU, and beyond this (0.30-1.01 AU) it increases with the local ion inertial length. This characteristic scaling is present for TDs throughout between 0.06 and 1.01 AU. Conclusions. Our results give us a simple classification tool for future studies of DDs, that is based only on magnetic field measurements. After we analyzed the DD thickness, we observationally confirmed that RDs are produced by Alfven-wave steepening, while the TDs are most likely the boundaries of flux tubes.

Solar wind parameters, such as the velocity, density or pressure of the solar wind, are one of the most important factors in space physics, and their knowledge at as many points in the heliosphere as possible contributes to a broader understanding of our solar system. Solar wind parameters at various points in the inner heliosphere are estimated using extrapolation methods. Currently, all spacecraft measuring solar wind parameters are in the ecliptic plane, thus it is enough to extrapolate the data from space probes to other spacecraft or celestial bodies near the ecliptic. Solar Orbiter, on the other hand, will soon leave the ecliptic and reach heliocentric latitudes of 34 degrees by the end of the mission, opening a new perspective. The ballistic method extrapolates solar wind parameters in one dimension from the point of measurement to a chosen heliospheric position. The simple ballistic model considers the average rotation period of the Sun for the extrapolation in longitude while assuming a constant solar wind velocity during radial propagation. Our improved solar wind propagation model takes into account the interaction of slow and fast solar wind by applying a pressure correction during the extrapolation. Applying this pressure-corrected ballistic method to data from solar corona models, we determined the solar wind parameters in the heliosphere in three dimensions. The advantage of our pressure-corrected ballistic method is that it is simple, it requires little calculation and it can be easily applied to the data of solar corona models in order to obtain a fast and efficient prediction in three dimensions.

We present five events of SLAMS (short large-amplitude magnetic structures) detected upstream of the quasi-parallel bow shock of Saturn. The events were discovered and further analyzed using the measurements of the Cassini Plasma Spectrometer and the Magnetometer instruments of the Cassini spacecraft. Directional, speed and temperature analysis of the charged particles in the vicinity of the SLAM structures is presented. We also analyze the effect of upstream parameters (especially the IMF and cone angle) on the ULF wave frequency and subsequent SLAMS formation. We use a simple empirical model to estimate location of the bow shock related to the SLAMS observations. We also discuss the spatial characteristics of SLAMS observed near Saturn by extrapolating the measurements and morphology derived by the four Cluster probes at Earth.

<div>The importance of background solar wind is unquestionable as it carries information on the solar surface conditions and has a major role in space weather events. The current solar minimum is a perfect time period for investigations regarding this field, with several space probes providing in-situ measurements.</div><div> </div><div>Our aim is to determine the spatial variations in the background solar wind through multi-spacecraft data analysis, including recent missions, such as Parker Solar Probe and Solar Orbiter. We adjust for the radial and longitudinal time-lags between the different spacecraft, then compare their solar wind plasma measurements. The effects of latitudinal differences between the observations is then backmapped to coronagraph imagery. The results will be useful for further analysis of inner heliospheric structures, for the improvement of propagation models, and to support the analysis of out-of-ecliptic solar wind observations.</div>

In order to improve the predictions of the solar wind environment at planets, moons, comets and interplanetary spacecraft, we study the temporal evolution and spatial variation of solar wind structures. Special emphasis is put on the fast and slow solar wind stream interaction regions (SIRs or CIRs). Currently, a huge fleet of solar observatories is available throughout the inner heliosphere, hence a multi-spacecraft study of the propagation and evolution of these structures is possible. We improve solar wind predictions by removing ICME signatures from the input data to reduce the number of false alarms. Ballistic radial propagation models are refined by pressure correction at CIRs. Latitudinal effects are taken into account to improve the models and to extend our predictions to three dimensions.

The solar wind properties at a given point in the heliosphere depend strongly on the source surface characteristics, the dynamical effects during propagation and the transient events. We study the background solar wind structures after modelling their propagation throughout the 3-dimensional heliosphere. We remove the transient events from the observations, then apply the ballistic propagation method corrected for pressure gradients at stream interactions. A detailed multi-spacecraft investigation of the radial and latitudinal effects improves our model. These results are applied to study the temporal evolution of the solar wind by excluding the spatial effects through adjusting for the timelag calculated from the spacecraft separations.

The Parker Solar Probe and Solar Orbiter spacecraft make whole new spatial and time scales available in the inner Heliosphere. With these new data, we study directional discontinuities that are common structures in the solar wind in this region. Their radial distribution can provide insight into the physical processes of this virtually collisionless plasma. Applying a method (Erdős & Balogh, 2008) based on minimum variance analysis to select directional discontinuities in magnetic field data, we determine their number as a function of distance from the Sun. How the directional discontinuity occurrence rate depends on the solar wind speed is also part of our analysis.

<p>Co-rotating Interaction Regions are complex and fascianting structures in the Heliosphere that <br>play an important role in space weather. They arise from the fast solar wind interacting with the <br>slow solar wind streams. The interface between fast and slow solar wind is called the stream <br>interface, and it is common for CIRs to produce forward shock at the leading edge and reverse <br>shock at the trailing edge. CIRs often have considerable tilts in the north-south axis, owing to the magnetic <br>conditions on the Sun.</p><p><br>Examination of the spatial structure of CIRs, – most importantly the aforementioned tilt – is not <br>an easy task. We attempt a multi-spacecraft investigation in order to examine the spatial <br>structure of CIRs on different distance scales. Using all available spacecraft data nearby, the tilt <br>of the stream interface can be determined considering the time delays of the effects caused by <br>the CIR recorded by each spacecraft. Our final aim is to improve solar wind propagation <br>methods with these detailed CIR results.</p>

We compare the predictions of the GUMICS$-$4 global magnetohydrodynamic model for the interaction of the solar wind with the Earth's magnetosphere with Cluster~SC3 measurements for over one year, from January 29, 2002, to February 2, 2003. In particular, we compare model predictions with the north/south component of the magnetic field ($B_{z}$) seen by the magnetometer, the component of the velocity along the Sun-Earth line ($V_{x}$), and the plasma density as determined from a top hat plasma spectrometer and the spacecraft's potential from the electric field instrument. We select intervals in the solar wind, the magnetosheath, and the magnetosphere where these instruments provided good-quality data, and the model correctly predicted the region in which the spacecraft is located. We determine the location of the bow shock, the magnetopause, and the neutral sheet from the spacecraft measurements and compare these locations to those predicted by the simulation. The GUMICS$-$4 model agrees well with the measurements in the solar wind however its accuracy is worse in the magnetosheath. The simulation results are not realistic in the magnetosphere. The bow shock location is predicted well, however, the magnetopause location is less accurate. The neutral sheet positions are located quite accurately thanks to the special solar wind conditions when the $B_{y}$ component of the interplanetary magnetic field is small.

After accompanying comet 67P/Churyumov–Gerasimenko on its journey around the Sun and observing the evolution of its induced magnetosphere throughout the comet's life-cycle, the Rosetta operations concluded at the end of September 2016 with a controlled impact on the cometary nucleus. At that time, the comet was located more than 3.7 AU from the Sun, but the data still show clear indications of a weak but well developed plasma environment around the nucleus. Rosetta observed this fading cometary magnetosphere along multiple recurring elliptical orbits, which allow us to investigate its properties and spatial structure. We examined the measured electron and neutral densities along these consecutive orbits, from which we were able to determine the structure of the spatial plasma distribution using a simple latitude and longitude dependent model.

In order to build a diverse, inclusive community of geoscientists within Europe, a statistical study is carried out based on participation statistics of different conferences in Europe over the past five years. Data of geoscience conferences (EGU, IUGG), planetary (EPSC) and solar-terrestrial science conferences (ESWW, ESPM) are investigated. Special focus is given to the historical division between Eastern and Western Europe and senior and junior scientists. The aim is to show that the geographical division continues to exist and does not show a general improving trend, while the position of the younger generation seems to improve. Some “success cases” defying the usual trend are shown and analysed in detail. We suggest some reasons behind the statistics and draw some lessons that can help integrating less represented researchers into the mainstream of European geosciences.

Rosetta observed medium-energy ions around comet 67P/Churyumov-Gerasimenko while orbiting deep inside the coma. These ions are thought to be accelerated towards the anti-sunward direction by some acceleration mechanism in the outer regions of the cometary magnetosphere. They usually reach energies up to 100-1000 eV and undergo deceleration in the dense neutral coma surrounding the nucleus. These ions usually appear in the ion dynamic spectrum as a new population rising from the low energy background, their energy peaking around 1000 eV and then decreasing until the population disappears again. We investigated the properties of these ions, as well as the relationship between the solar wind pressure and the energy of the medium-energy ions to discover the cause of the observed time variation. We show that there is a correlation between the solar wind dynamic pressure around the comet and the energy of the accelerated ions.

The dynamic changes of Mercury’s Na exosphere are investigated here, in relation to space weather conditions. Sodium plays a special role in Mercury’s exosphere: due to its strong resonance D lines at 5890-95Å it has been observed and monitored by Earth-based telescopes for decades. Different and highly variable patterns of Na-emission have been identified. In addition to the release processes already studied extensively in the past, we aim here to investigate the following factors more in detail: the distance to the Sun, position in relation to the ecliptic plane and solar wind magnetic field strength and direction. In order to better investigate the relationship of these factors, we have studied the intensity of Na-emission as a function of solar wind dynamic pressure and TAA of Mercury by means of the extended dataset images collected from 2009 to 2013 by Earth-based observations performed at the THEMIS solar telescope. Solar wind velocity and density values are propagated with the magnetic lasso method to the position of Mercury from nearby space probes and compared with Na emission intensity. Data of either ACE or one of the two STEREO spacecraft were used, depending on which spacecraft had a smaller angular distance to Mercury. Single cases are studied qualitatively, and a longer-term quantitative comparison is shown, including further parameters (solar wind magnetic field strength and direction, TAA).

Determining the ion bulk velocity is essential to understand the physics of the inner magnetosphere of comets. This velocity controls the strength of the ion-neutral drag force, which plays a very important role in the energy and momentum transfer processes of that region. Unfortunately there are no direct measurements of this quantity available. The energy thresholds of the ion instruments on board the Rosetta orbiter would prevent the direct detection of the bulk ion content of the plasma as long as the plasma is relatively slow and cold. The picture is further complicated by the spacecraft potential, which accelerates the thermal ions to energies higher than the measurement threshold, but effectively screens the magnitude and direction of their original velocity. That distortion effect is not arbitrary however; it is possible to recover the original ion velocity distribution from IES measurements by simulating the effects of the spacecraft potential on the ion motion. We performed these simulations for several bulk and thermal velocity as well as spacecraft potential values, and compared the results with IES measurements. From this we could determine the most probable values of the bulk and thermal speeds of the plasma ions in the inner magnetosphere of comet 67P/ Churyumov–Gerasimenko.

Determining the ion bulk velocity is essential to understand the physics of the inner magnetosphere of comets. This velocity controls the strength of the ion-neutral drag force, which plays a very important role in the energy and momentum transfer processes of that region. Unfortunately there are no direct measurements of this quantity available. The energy thresholds of the ion instruments on board the Rosetta orbiter would prevent the direct detection of the bulk ion content of the plasma as long as the plasma is relatively slow and cold. The picture is further complicated by the spacecraft potential, which accelerates the thermal ions to energies higher than the measurement threshold, but effectively screens the magnitude and direction of their original velocity. That distortion effect is not arbitrary however; it is possible to recover the original ion velocity distribution from IES measurements by simulating the effects of the spacecraft potential on the ion motion. We performed these simulations for several bulk and thermal velocity as well as spacecraft potential values, and compared the results with IES measurements. From this we could determine the most probable values of the bulk and thermal speeds of the plasma ions in the inner magnetosphere of comet 67P/ Churyumov–Gerasimenko.

Aims : The solar wind pressure is an important parameter of space weather, which plays a crucial role in the interaction of the solar wind with the planetary plasma environment. Here we investigate the possibility of determining a solar wind pressure proxy from Rosetta magnetic field data, measured deep inside the induced magnetosphere of comet 67P/Churyumov-Gerasimenko. This pressure proxy would be useful not only for other Rosetta related studies but could also serve as a new, independent input database for space weather propagation to other locations in the Solar System. Method : For the induced magnetospheres of comets the magnetic pressure in the innermost part of the pile-up region is balanced by the solar wind dynamic pressure. Recent investigations of Rosetta data have revealed that the maximum magnetic field in the pile-up region can be approximated by magnetic field measurements performed in the inner regions of the cometary magnetosphere, close to the boundary of the diamagnetic cavity, from which the external solar wind pressure can be estimated. Results : We were able to determine a solar wind pressure proxy for the time interval when the Rosetta spacecraft was located near the diamagnetic cavity boundary, between late April 2015 and January 2016. We then compared our Rosetta pressure proxy to solar wind pressure extrapolated to comet 67P from near-Earth. After the exclusion of disturbances caused by transient events, we found a strong correlation between the two datasets.