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The study aimed to examine the excessive use of the Internet in the mental health of students of Veterinary Medicine and Zootechnics at the National University of the Alti-plano, Puno, Peru. The study was descriptive, explanatory and cross-sectional, carried out with 226 students (152 men and 74 women) from I to X cycle, aged 23.4 ± 5.5 years. Mental health was related to anxiety, depression and the sleep quality index. Internet use was quantified through a survey, exploring the time (h/day) of use during the last 30 days; anxiety and depression were determined through the Hamilton Rating Scale (HARS and HDRS), with internal consistency, α = 0.93 and 0.89, respectively; and the sleep quality index using the Pittsburgh questionnaire (α=0.87). The results indicate that depression (β= 0.292; p, El estudio tuvo como objetivo examinar el uso excesivo de Internet en la salud mental de estudiantes de Medicina Veterinaria y Zootecnia de la Universidad Nacional del Alti-plano, Puno, Perú. El estudio fue de tipo descriptivo, explicativo y de corte transversal, realizado con 226 alumnos (152 varones y 74 mujeres) de I a X ciclo, con edades de 23.4± 5.5 años. La salud mental fue relacionada con la ansiedad, la depresión y el índice de la calidad de sueño. El uso de Internet se cuantificó mediante encuesta, explorando el tiempo (h/día) de uso durante los últimos 30 días; la ansiedad y la depresión fue determi-nada a través de la escala de valoración de Hamilton (HARS y HDRS), con una consis-tencia interna, α = 0.93 y 0.89, respectivamente; y el índice de la calidad del sueño median-te el cuestionario de Pittsburgh (α=0.87). Los resultados indican que la depresión (β = 0.292; p

We present a review of Anomalous Cosmic Rays (ACRs), including the history of their discovery and recent insights into their acceleration and transport in the heliosphere. We focus on a few selected topics including a discussion of mechanisms of their acceleration, escape from the heliosphere, their effects on the dynamics of the heliosheath, transport in the inner heliosphere, and their solar cycle dependence. A discussion concerning their name is also presented towards the end of the review. We note that much is known about ACRs and perhaps the term Anomalous Cosmic Ray is not particularly descriptive to a non specialist. We suggest that the more-general term: “Heliospheric Energetic Particles”, which is more descriptive, for which ACRs and other energetic particle species of heliospheric origin are subsets, might be more appropriate.

Our understanding of the interaction of the large-scale heliosphere with the local interstellar medium (LISM) has undergone a profound change since the very earliest analyses of the problem. In part, the revisions have been a consequence of ever-improving and widening observational results, especially those that identified the entrance of interstellar material and gas into the heliosphere. Accompanying these observations was the identification of the basic underlying physics of how neutral interstellar gas and interstellar charged particles of different energies, up to and including interstellar dust grains, interacted with the temporal flows and electromagnetic fields of the heliosphere. The incorporation of these various basic effects into global models of the interaction, whether focused on neutral interstellar gas and pickup ions, energetic particles such as anomalous and galactic cosmic rays, or magnetic fields and large-scale flows, has profoundly changed our view of how the heliosphere and LISM interact. This article presents a brief history of the conceptual and observation evolution of our understanding of the interaction of the heliosphere with the local interstellar medium, up until approximately 1996., Space Science Reviews, 218, ISSN:1572-9672, ISSN:0038-6308

We observe and analyse a long-lived corotating interaction region (CIR), originating from a single coronal hole (CH), recurring in 27 consecutive Carrington rotations 2057-2083 in the time period from June 2007 - May 2009. We studied the in situ measurements of this long-lived CIR as well as the corresponding depression in the cosmic ray (CR) count observed by SOHO/EPHIN throughout different rotations. We performed a statistical analysis, as well as the superposed epoch analysis, using relative values of the key parameters: the total magnetic field strength, B, the magnetic field fluctuations, dBrms, plasma flow speed, v, plasma density, n, plasma temperature, T , and the SOHO/EPHIN F-detector particle count, and CR count. We find that the mirrored CR count-time profile is correlated with that of the flow speed, ranging from moderate to strong correlation, depending on the rotation. In addition, we find that the CR count dip amplitude is correlated to the peak in the magnetic field and flow speed of the CIR. These results are in agreement with previous statistical studies. Finally, using the superposed epoch analysis, we obtain a generic CIR example, which reflects the in situ properties of a typical CIR well. Our results are better explained based on the combined convection-diffusion approach of the CIR-related GCR modulation. Furthermore, qualitatively, our results do not differ from those based on different CHs samples. This indicates that the change of the physical properties of the recurring CIR from one rotation to another is not qualitatively different from the change of the physical properties of CIRs originating from different CHs. Finally, the obtained generic CIR example, analyzed on the basis of superposed epoch analysis, can be used as a reference for testing future models., Comment: 13 pages, A&A in press

Kollhoff, A., et al., Context. On 2020 November 29, the first widespread solar energetic particle (SEP) event of solar cycle 25 was observed at four widely separated locations in the inner (≲ 1 AU) heliosphere. Relativistic electrons as well as protons with energies > 50 MeV were observed by Solar Orbiter (SolO), Parker Solar Probe, the Solar Terrestrial Relations Observatory (STEREO)-A and multiple near-Earth spacecraft. The SEP event was associated with an M4.4 class X-ray flare and accompanied by a coronal mass ejection and an extreme ultraviolet (EUV) wave as well as a type II radio burst and multiple type III radio bursts. Aims. We present multi-spacecraft particle observations and place them in context with source observations from remote sensing instruments and discuss how such observations may further our understanding of particle acceleration and transport in this widespread event. Methods. Velocity dispersion analysis (VDA) and time shift analysis (TSA) were used to infer the particle release times at the Sun. Solar wind plasma and magnetic field measurements were examined to identify structures that influence the properties of the energetic particles such as their intensity. Pitch angle distributions and first-order anisotropies were analyzed in order to characterize the particle propagation in the interplanetary medium. Results. We find that during the 2020 November 29 SEP event, particles spread over more than 230° in longitude close to 1 AU. The particle onset delays observed at the different spacecraft are larger as the flare-footpoint angle increases and are consistent with those from previous STEREO observations. Comparing the timing when the EUV wave intersects the estimated magnetic footpoints of each spacecraft with particle release times from TSA and VDA, we conclude that a simple scenario where the particle release is only determined by the EUV wave propagation is unlikely for this event. Observations of anisotropic particle distributions at SolO, Wind, and STEREO-A do not rule out that particles are injected over a wide longitudinal range close to the Sun. However, the low values of the first-order anisotropy observed by near-Earth spacecraft suggest that diffusive propagation processes are likely involved., The CAU Kiel team acknowledges support from the German Federal Ministry for Economic Affairs and Energy, the German Space Agency (Deutsches Zentrum für Luft- und Raumfahrt e.V., DLR) under grants 50OT0901, 50OT1202, 50OT1702, and 50OT2002. A.K. acknowledges financial support from the ANR COROSHOCK project (ANR-17-CE31-0006-01). D.L. acknowledges support from NASA-HGI grant NNX16AF73G and the NASA Program NNH17ZDA001N-LWS. This study has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No. 101004159 (SERPENTINE). The U. Turku team acknowledges funding by the Academy of Finland (Grant No. 336809). The UAH team acknowledges financial support by the Spanish Ministerio de Ciencia, Innovación y Universidades FEDER/MCIU/AEI Projects ESP2017-88436-R and PID2019-104863RB-I00/AEI/10.13039/501100011033. [...] The Swedish National Space Agency, ESA-PRODEX and all the participating institutes. I.G.R. acknowledges support from NASA programs NNH19ZDA001N-HSR and NNH19ZDA001N-LWS, and the STEREO mission. IRFU team acknowledges support from the Swedish National Space Agency grant 20/136. A.A. acknowledges the support of the Spanish Ministerio de Ciencia e Innovación (MICINN) under grant PID2019- 105510GB-C31 and through the ‘Center of Excellence María de Maeztu 2020-2023’ award to the ICCUB (CEX2019-000918- M). F.C. acknowledges the financial support by the Spanish MINECO-FPI-2016 predoctoral grant with FSE. E.A. would like to acknowledge the financial support by the Academy of Finland (Postdoctoral Grant No 322455). V.K. acknowledges the support by NASA under grants 18-2HSWO218_2-0010 and 19-HSR-19_2-0143. Solar Orbiter magnetometer operations are funded by the UK Space Agency (grant ST/T001062/1). T.S.H. is supported by STFC grant ST/S000364/1. T.L. and S.D. acknowledge support from the UK Science and Technology Facilities Council (STFC; grant ST/R000425/1).

The radiation data collected by the Standard Radiation Environment Monitor (SREM) aboard ESA missions INTEGRAL (INTErnational Gamma-Ray Astrophysics Laboratory), Rosetta, Herschel, Planck and Proba-1, and by the high-energy neutron detector (HEND) instrument aboard Mars Odyssey, are analysed with an emphasis on characterising galactic cosmic rays (GCRs) in the inner heliosphere. A cross calibration between all sensors was performed for this study, which can also be used in subsequent works. We investigate the stability of the SREM detectors over long-term periods. The radiation data are compared qualitatively and quantitatively with the corresponding solar activity. Based on INTEGRAL and Rosetta SREM data, a GCR helioradial gradient of 2.96 % AU−1 is found between 1 and 4.5 AU. In addition, the data during the last phase of the Rosetta mission around comet 67P/Churyumov–Gerasimenko were studied in more detail. An unexpected yet unexplained 8 % reduction of the Galactic Comic Ray flux measured by Rosetta SREM in the vicinity of the comet is noted.

Context. The shape of the pitch-angle distribution (PAD) of solar energetic particles (SEPs) can be used to infer information about their source and interplanetary transport. In modeling and observational studies of SEP events, these PADs are frequently applied to determine the anisotropy which is a proxy for the strength of the pitch-angle scattering during transport. For the determination of the PAD, derivation of the pitch angle of SEPs takes on a crucial role. For most instrument-sampled PADs, the particle’s pitch angle cannot be resolved directly but is usually approximated by considering the time-averaged in situ magnetic field direction, and the center viewing direction of the telescope. However, variations of the magnetic field, and the extent of the physical opening of the instrument lead to uncertainty on the determination of the pitch angle and therefore to uncertainty on the anisotropy and its interpretation. Aims. In this work, we present a new method to determine a distribution of anisotropy values which allows us to estimate the corresponding uncertainty ranges. We apply our method to electron measurements by the Solar Electron and Proton Telescope on board each STEREO spacecraft. Methods. We determined a distribution of anisotropy values by solving an inversion problem that takes into account the directional response of the instrument, the variation of the in situ magnetic field, and the stochastic nature of particle detection. Using 95% confidence intervals, we estimate the uncertainty on the anisotropy. Results. The application of our method to a solar electron event observed by STEREO B on 14 August 2010 yields a maximum anisotropy of 1.9 with an uncertainty on the order of ±0.1. During the background period, the anisotropy shows strong fluctuations, and absolute uncertainties on the order of ±0.5 that are attributable to low counting statistics.

Wimmer-Schweingruber, R. F., et al., [Context] Solar Orbiter strives to unveil how the Sun controls and shapes the heliosphere and fills it with energetic particle radiation. To this end, its Energetic Particle Detector (EPD) has now been in operation, providing excellent data, for just over a year. [Aims] EPD measures suprathermal and energetic particles in the energy range from a few keV up to (near-) relativistic energies (few MeV for electrons and about 500 MeV nuc-1 for ions). We present an overview of the initial results from the first year of operations and we provide a first assessment of issues and limitations. In addition, we present areas where EPD excels and provides opportunities for significant scientific progress in understanding how our Sun shapes the heliosphere. [Methods] We used the solar particle events observed by Solar Orbiter on 21 July and between 10 and 11 December 2020 to discuss the capabilities, along with updates and open issues related to EPD on Solar Orbiter. We also give some words of caution and caveats related to the use of EPD-derived data. [Results] During this first year of operations of the Solar Orbiter mission, EPD has recorded several particle events at distances between 0.5 and 1 au from the Sun. We present dynamic and time-averaged energy spectra for ions that were measured with a combination of all four EPD sensors, namely: the SupraThermal Electron and Proton sensor (STEP), the Electron Proton Telescope (EPT), the Suprathermal Ion Spectrograph (SIS), and the High-Energy Telescope (HET) as well as the associated energy spectra for electrons measured with STEP and EPT. We illustrate the capabilities of the EPD suite using the 10 and 11 December 2020 solar particle event. This event showed an enrichment of heavy ions as well as 3He, for which we also present dynamic spectra measured with SIS. The high anisotropy of electrons at the onset of the event and its temporal evolution is also shown using data from these sensors. We discuss the ongoing in-flight calibration and a few open instrumental issues using data from the 21 July and the 10 and 11 December 2020 events and give guidelines and examples for the usage of the EPD data. We explain how spacecraft operations may affect EPD data and we present a list of such time periods in the appendix. A list of the most significant particle enhancements as observed by EPT during this first year is also provided., We acknowledge the Spanish Ministerio de Ciencia, Innovación y Universidades for their invaluable support on the development of the EPD suite and the ICU under grants FEDER/MCIU – Agencia Estatal de Investigación/Projects ESP2015-68266-R, ESP2017-88436-R and PID2019-104863RB-I00/AEI/10.13039/501100011033. We also thank acknowledge the financial support by the Spanish MINECO-FPI-2016 predoctoral grant with FSE. We thank the German Federal Ministry for Economic Affairs and Energy and the German Space Agency (Deutsches Zentrum für Luft- und Raumfahrt, e.V., (DLR)) for their unwavering support of STEP, EPT, and HET under grants numbers 50OT0901, 50OT1202, 50OT1702, and 50OT2002; and ESA for supporting the build of SIS under contract number SOL.ASTR.CON.00004, as well as the University of Kiel and the Land Schleswig-Holstein for their support of SIS. We thank NASA headquarters and the GSFC Solar Orbiter project office for support of SIS at APL under contract NNN06AA01C. A.A. acknowledges the support by the Spanish Ministerio de Ciencia e Innovación (MICINN) under grant PID2019- 105510GB-C31 and through the ‘Center of Excellence María de Maeztu 2020-2023’ award to the ICCUB (CEX2019-000918- M). Solar Orbiter magnetometer operations are funded by the UK Space Agency (grant ST/T001062/1). Tim Horbury is supported by STFC grant ST/S000364/1. We acknowledge funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No. 101004159 (SERPENTINE).

Gómez-Herrero, R., et al., Context. Solar Orbiter, launched in February 2020, started its cruise phase in June 2020, in coincidence with its first perihelion at 0.51 au from the Sun. The in situ instruments onboard, including the Energetic Particle Detector (EPD), operate continuously during the cruise phase enabling the observation of solar energetic particles. Aims. In situ measurements of the first near-relativistic solar electron events observed in July 2020 by EPD are analyzed and the solar origins and the conditions for the interplanetary transport of these particles investigated. Methods. Electron observations from keV energies to the near-relativistic range were combined with the detection of type III radio bursts and extreme ultraviolet (EUV) observations from multiple spacecraft in order to identify the solar origin of the electron events. Electron anisotropies and timing as well as the plasma and magnetic field environment were evaluated to characterize the interplanetary transport conditions. Results. All electron events were clearly associated with type III radio bursts. EUV jets were also found in association with all of them except one. A diversity of time profiles and pitch-angle distributions was observed. Different source locations and different magnetic connectivity and transport conditions were likely involved. The July 11 event was also detected by Wind, separated 107 degrees in longitude from Solar Orbiter. For the July 22 event, the Suprathermal Electron and Proton sensor of EPD allowed for us to not only resolve multiple electron injections at low energies, but it also provided an exceptionally high pitch-angle resolution of a very anisotropic beam. This, together with radio observations of local Langmuir waves suggest a very good magnetic connection during the July 22 event. This scenario is challenged by a high-frequency occultation of the type III radio burst and a nominally non-direct connection to the source; therefore, magnetic connectivity requires further investigation., The UAH team acknowledges the financial support by the Spanish MICIU under projects ESP2017-88436-R and PID2019-104863RB-I00/AEI/10.13039/501100011033. The CAU Kiel team acknowledges support by the German Federal Ministry for Economic Affairs and Energy, the German Space Agency (Deutsches Zentrum für Luft- und Raumfahrt e.V., DLR) under grants 50OT0901, 50OT1202, 50OT1702, 50OT2002, and 50OC1702. A. Aran acknowledges the support by the Spanish Ministerio de Ciencia e Innovación (MICINN) under grant PID2019-105510GB-C31 and through the “Center of Excellence María de Maeztu 2020-2023” award to the ICCUB (CEX2019-000918-M). The RPW team thanks the French space agency CNES, the Center National de Recherches Scientifiques, the Paris Observatory, the Swedish National Space agency, ESA-PRODEX and the Czech Science Foundation (17-08772S) for the funding provided. V. Krupar acknowledges the support by NASA under grants 18-2HSWO218_2-0010 and 19-HSR-19_2-0143. The Solar Orbiter magnetometer was funded by the UK Space Agency (grant ST/T001062/1).

Monitoring soil moisture is still a challenge: it varies strongly in space and time and at various scales while conventional sensors typically suffer from small spatial support. With a sensor footprint up to several hectares, cosmic-ray neutron sensing (CRNS) is a modern technology to address that challenge. So far, the CRNS method has typically been applied with single sensors or in sparse national-scale networks. This study presents, for the first time, a dense network of 24 CRNS stations that covered, from May to July 2019, an area of just 1 km2: the pre-Alpine Rott headwater catchment in Southern Germany, which is characterized by strong soil moisture gradients in a heterogeneous landscape with forests and grasslands. With substantially overlapping sensor footprints, this network was designed to study root-zone soil moisture dynamics at the catchment scale. The observations of the dense CRNS network were complemented by extensive measurements that allow users to study soil moisture variability at various spatial scales: roving (mobile) CRNS units, remotely sensed thermal images from unmanned areal systems (UASs), permanent and temporary wireless sensor networks, profile probes, and comprehensive manual soil sampling. Since neutron counts are also affected by hydrogen pools other than soil moisture, vegetation biomass was monitored in forest and grassland patches, as well as meteorological variables; discharge and groundwater tables were recorded to support hydrological modeling experiments. As a result, we provide a unique and comprehensive data set to several research communities: to those who investigate the retrieval of soil moisture from cosmic-ray neutron sensing, to those who study the variability of soil moisture at different spatiotemporal scales, and to those who intend to better understand the role of root-zone soil moisture dynamics in the context of catchment and groundwater hydrology, as well as land–atmosphere exchange processes. The data set is available through the EUDAT Collaborative Data Infrastructure and is split into two subsets: https://doi.org/10.23728/b2share.282675586fb94f44ab2fd09da0856883 (Fersch et al., 2020a) and https://doi.org/10.23728/b2share.bd89f066c26a4507ad654e994153358b (Fersch et al., 2020b).

El trabajo tuvo como objetivo evaluar la posibilidad de elaborar queso a partir de leche de alpaca. Se determinaron las propiedades fisicoquímicas de la leche, así como el rendimiento, composición química y características sensoriales del queso. La leche se obtuvo por ordeño manual de alpacas madres en inicio de lactación con crías en pie, apartadas 12 horas antes del ordeño. En la leche se analizó la densidad, acidez Dornic, grasa Gerber, y se estimaron los sólidos totales y no grasos de la leche. La composición química del queso se determinó por métodos oficiales de la AOAC, y las características sensoriales del queso a través de la prueba hedónica en escala de 1 a 4 con 100 panelistas. La leche fresca presentó una densidad de 1.0469 ± 0.0025, acidez 16.92 ± 1.74 °D, grasa 4.12 ± 0.08%, proteína 6.34 ± 0.41%, sólidos totales 16.84 ± 0.70%, sólidos no grasos 12.72 ± 0.63% y un rendimiento quesero de 21.6 ± 1.9%. La composición química del queso fue humedad 46.5%, ceniza 18.9%, proteína 41.8%, grasa 24.4% (en materia seca). El queso resultó un producto magro, de textura dura y agradable al consumo. The objective of this study was to evaluate the possibility of making cheese from alpaca milk. The physicochemical properties of the milk were determined, as well as the yield, chemical composition, and sensorial characteristics of the cheese. Milk was obtained by manual milking of alpacas at the beginning of lactation with crias at foot, set aside 12 hours before milking. The density, Dornic acidity and Gerber fat were determined, and total and non-fat milk solids were estimated in the milk. The chemical composition of the cheese was determined by official methods of the AOAC, and the sensory characteristics of the cheese through the hedonic test on a scale of 1 to 4 with 100 panelists. Fresh milk had a density of 1.0469 ± 0.0025, acidity 16.92 ± 1.74 °D, fat 4.12 ± 0.08%, protein 6.34 ± 0.41%, total solids 16.84 ± 0.70%, solids non-fat 12.72 ± 0.63% and a cheese yield of 21.6 ± 1.9%. The chemical composition of the cheese indicated 46.5% humidity, 18.9% ash, 41.8% protein, and 24.4% fat (dry matter). The cheese was a lean product with a hard texture and pleasant for consumption.

The NAVIgation DOsimetry System (NAVIDOS) comprises a complete readout system for a radiation detec- tor, an air pressure sensor and a GPS receiver. The detector system DOSTEL uses silicon detectors which make NAVI- DOS light weighted and compact in size. Therefore, NAVI- DOS is well suited to be installed on board aircraft. The cal- ibration of NAVIDOS in terms of ambient dose equivalent is done by an in-field comparison with the PTB reference in- strument DOS. We also show that the dependence of these results on the vertical cut-off rigidity can be explained by the low response of the silicon detectors for neutrons. Therefore, in-flight measurements have been performed together with the PTB reference instrument DOS. The dose rates, cal- culated using the PTB code FDOScalc, were verified with these DOS measurements. The calibration of NAVIDOS was done with FDOScalc and results in calibration factors between 3.4 in the polar and 2.4 in the equator region.

The physics of the heliosphere has seen several exciting developments in the past years since the in situ discovery of the termination shock by Voyager 1 at 94 AU and radio observations of the interaction of GMIRs with the heliopause. The local hydrogen wall ahead of the heliosphere has been inferred from interstellar absorption lines and information about the interstellar magnetic field is now available. This sudden richness of information has lead to a waking realisation about the importance of the heliosphere for long-term space climate and possibly even terrestrial climate.

We have analyzed 124 electron bursts at energies above 0.25 MeV observed with the EPHIN/COSTEP instrument onboard the SOHO spacecraft far upstream of the Earth's bow-shock at the libration point L1 from 1996 through 2005. Most of the bursts were observed during low solar activity (in 1996–1997 and in 2005) and all 124 bursts were not associated with solar particle events. It is shown that some upstream events are detected at energies above 0.7 MeV. We find that the event occurrence number shows a distinct seasonal variation with maxima around equinoxes and minima near solstices. This together with a close correspondence between the event occurrence number with maxima in solar wind speed (Vsw), geomagnetic activity index (Ap) and in the southward interplanetary magnetic field (IMF) component (Bz) indicates that the observed events can be explained in terms of leakage of magnetospheric particles during enhanced geoactivity rather than by acceleration at the Earth's bow-shock.

Solar sail technology holds the promise of enhancing the interplanetary transportation infrastructure for low-cost space exploration missions in the new millennium, by exploiting the freely available, space-pervading resource of solar radiation pressure for primary propulsion. Despite the large distances to the Sun and the reduced solar radiation pressure, fast missions to the outer edge of our solar system belong to the promising mission applications of solar sails. In order to realize such a mission, the sailcraft would first perform a so-called “solar photonic assist”, approaching the Sun to less than 0.3 AU thus exploiting the increased solar radiation pressure, to pick up enough orbital energy to enter a hyperbolic orbit. This concept has been extended to a double and triple solar approach which reduces the requirement for very high area-to-mass ratios of the sailcraft. The target distance of the Heliopause Explorer mission is set to 200 AU. The science objective was defined as to allow the Heliopause Explorer to perform in situ observations which cannot be obtained within the remaining life time of the two Voyager spacecraft. A first feasibility study was initiated to derive technology requirements for the realization of such a challenging deep space mission.

A time-dependent model based on a numerical solution of Parker’s transport equation is used to model the modulation of cosmic ray protons, electrons and helium for full 11-year and 22-year modulation cycles using a compound approach. This approach incorporates the concept of propagating diffusion barriers based on global increases in the heliospheric magnetic field as they propagate from the Sun throughout the heliosphere, combined with gradient, curvature and current sheet drifts and the other basic modulation mechanisms. The model results are compared to the observed 11-year and 22-year cycles for 1.2 GV electrons and 1.2 GV Helium at Earth for the period 1975–1998. The model solutions are also compared to the observed charge-sign dependent modulation along Ulysses’ trajectory for the period 1990–1998. This compound approach to long-term modulation, especially charge-sign dependent modulation, is found to be remarkably successful. It is shown that the model can easily account for the latitude dependence for cosmic ray protons and the lack thereof for cosmic ray electrons by assuming large perpendicular diffusion in the polar direction. This approach contributes to an improved understanding of how diffusion and drifts vary from solar minimum to maximum modulation, and what the time-dependence of the heliospheric diffusion coefficients may be. Key words. Interplanetary physics (energetic particles; cosmic rays; general or miscellaneous)

In mid 1996 the Comprehensive Suprathermal and Energetic Particle Analyser (COSTEP) onboard the Solar and Heliospheric Observatory, at 1 AU in the ecliptic plane, detected recurrent periods of enhanced MeV ions in association with a corotating interaction region (CIR). Measurements of energetic ions from the Cosmic Ray and Solar Particle Instrument/Low Energy Telescope (COSPIN/LET) onboard Ulysses taken at 5 AU, at mid-northern heliographic latitudes, showed that Ulysses encountered recurrent particle events during the same time period. We used the solar wind speeds observed at both locations to estimate the corresponding solar source longitudes of the particle events. These longitudes are related to warps of the Sun's large high latitude northern coronal hole boundaries observed by SOHO's Extreme Ultraviolet Imaging Telescope (EIT). The findings are supported by threedimensional magnetohydrodynamic (MHD) calculations of the footpoint positions of the magnetic field lines at both spacecraft. The observations suggest that close to the Sun a superradial expansion of the fast solar wind from the Sun's high latitude northern coronal hole down to ecliptic latitudes is present.

According to standard drift dominated modulation models the intensity variations of galactic cosmic ray protons and electrons respond differently to the latitudinal extension of the heliospheric current sheet α. In an A>0 solar cycle intensities of protons should vary weakly with the latitudinal extension, whereas electrons should show a strong response. We investigate this charge dependent variation in the 1990s (A>0) using Ulysses Kiel Electron Telescope (KET) measurements. Proton measurements at 2.5 GV corrected for latitudinal variations show the same time profile as electrons from mid 1994 until the beginning of 1996, and later from September 1997 to the end of 1997. In 1996 and 1997, when α was below ∼25°, two long lasting time periods were found when electrons had a ∼5–10% higher level. These variations are in agreement with our computations indicating that drift effects play an important role in determining the temporal variation of electrons close to solar minimum.

Corotating Interaction Regions are long lasting large-scale plasma structures generated in low and middle latitude regions of the heliosphere by the interaction of a stable fast solar wind stream with the surrounding slow solar wind. Associated with these plasma structures are recurrent MeV-ion events and recurrent decreases of the galactic and anomalous cosmic ray intensities. Prior to the Ulysses-mission the effect of corotating interaction regions could only be observed at low or moderate heliographic latitudes. The three-dimensional extent and their role in structuring the quiet heliosphere became clear after Ulysses high latitude observations had became available. Corotating interaction regions possibly play a role in determining solar modulation of galactic and anomalous cosmic rays during periods of low to moderate solar activity. In March 1996, April 1997, and June 1998 two workshops on Development and Effects of Corotating Interaction Regions were held at Elmau Castle, Germany, and at the International Space Science Institute in Bern, Switzerland, primarily based on new high latitude observations from Ulysses and considering as well in-ecliptic and outer-heliospheric spacecraft result. In this paper MeV-particle, galactic and anomalous cosmic ray as well as plasma observations from spacecraft in the inner heliosphere will be presented.

Ulysses, launched in October 1990, crossed in December 1997 the heliographic equator and completed its first out of ecliptic orbit. During the time period from February 1995 to November 1997 solar activity was low and the spacecraft scanned the latitude range from 80° N to the heliographic equator. The Kiel Electron Telescope on-board Ulysses measures protons and α-particles in the energy range from 5 MeV/n to > 2 GeV/n. To separate spatial and temporal variations of > 2 GeV/n protons and α-particles along the spacecraft trajectory we used the data set from the world wide neutron monitor network. We found negligible latitudinal gradients below ∼29° N and for the radial gradient an upper limit of ≈ 0.5 %/AU for > 2 GeV/n protons and α-particles. In the latitudinal range from ≈ 25 to > 70° N the latitudinal gradient is ∼0.17 %/° and ∼0.12 %/° for > 2 GeV/n protons and α-particles, respectively, independent of spacecraft latitude and radial distance.

The spatial intensity gradients of galactic and anomalous cosmic ray helium are studied over the 1993.0–1998.0 time period using data from cosmic ray experiments on IMP 8, Ulysses, Voyagers 1 and 2 and Pioneer 10. When combined with the results of previous studies, a remarkable ordering of the radial gradients for the galactic component is found over 2 complete solar cycles and 3 successive solar minima. The latitudinal gradients for the cycle 22 solar minimum period are zero or small and positive in the inner and outer heliosphere in contrast to the much larger negative latitudinal gradients observed in the outer heliosphere in 1987 over the cycle 21 solar minimum. The changes in the intensity gradients over the 3 solar minimum periods require that at these times drift effects play an important role in the transport of cosmic rays in the heliosphere and provide further evidence for the existence of a 22-year solar modulation cycle. The Ulysses data plays a pivotal role in understanding the spatial gradients over the cycle 22 recovery and solar minimum period.

The high energy cosmic rays observed with the Kiel Electron Telescope (KET) on board ULYSSES vary with solar activity as well as with heliospheric position. Starting February 1992 ULYSSES climbed to high latitudes with a maximum reached in mid September 1994 at 80° above the south polar cap. During the time of transition to solar minimum conditions the observed latitude dependence is much smaller than expected for both positively and negatively charged particles. Latitudinal gradients of quiet time nuclei are between 0.1 and 0.6%/° with similar values for electrons. Surprisingly effects of corotating interaction regions were observed up into the solar polar region as accelerated low energy ions and as recurrent decreases of high energy ions.

Summary Background. Autoimmune bullous disorders of the pemphigus group are characterized by autoantibodies targeting desmoglein (Dsg)1, Dsg3 and Dsg4 and occasionally, desmocollin (Dsc)1, Dsc2 and Dsc3. Both Dsg and Dsc are components of desmosomal adhesion complexes. Aim. To investigate the presence of IgG and IgA autoantibodies against Dsc1, Dsc2 and Dsc3 in a cohort of patients with bullous disorders. Methods. IgG and IgA autoantibodies against Dsc1, Dsc2 and Dsc3 were investigated by ELISA and immunoblotting analysis in a cohort of European patients with pemphigus vulgaris (PV; n = 74), IgA pemphigus (n = 3), paraneoplastic pemphigus (PNP; n = 3) and two cases of atypical pemphigus (n = 2). Results. Of the two cases with atypical pemphigus, one showed IgA reactivity against Dsc1 and Dsc3 and weak reactivity against Dsc2, and the other showed both IgG and IgA reactivity against Dsc1. One patient with IgA pemphigus had IgA autoantibodies against Dsc1, Dsc2 and Dsg1, and one patient with PNP had IgG reactivity against with Dsc3. In contrast, all the PV sera showed IgG reactivity against Dsg3 but not against Dsc1–3. Thus, IgG and IgA reactivity against Dsc was restricted to cases of PNP, IgA pemphigus and atypical pemphigus. Conclusions. These findings support the concept that desmocollins are not important autoantigens in PV.

Cosmic ray research began in 1912 when Victor Hess measured the intensity of the then unknown ionizing radiation with an electroscope in a balloon up to an altitude of about 5,000 m. He discovered that this very penetrating radiation, later called cosmic rays, was coming from outside the atmosphere (for a historic review, see Simpson, 2001).The systematic experimental study of cosmic rays began in the 1930s, using ground-based and balloon-borne ionization chambers. In the 1950s it expanded on a much larger scale with neutron monitors, coordinated world-wide during the International Geophysical Year (IGY) in 1957 (Simpson, 2000). When Parker (1958) described the solar wind, the theoretical research of cosmic rays began, stimulated by the beginning of in situ space observations that have led over four decades to important space missions, including the Ulysses mission to high heliolatitudes.

In October 2011, ESA announced the selection of Solar Orbiter as one of the Cosmic Vision M missions. It's launch is foreseen in 2018. Therefore it is worthwhile to revisit the energetic particle measurements together with the solar wind and magnetic field data from Helios in light of better theoretical understanding and advanced analysis and modelling techniques developed during the past 20 years. In this contribution we will present a GEANT 4 simulation of the response function of the Helios E6 experiment, that measured electrons in the energy range from a few 100 keV to above 10 MeV, ions from 1 MeV/nucleon to above 50 MeV/nucleon, and its application to the data analysis with respect to the chemical composition of the Galactic Cosmic Rays.

Neutron monitors (NMs) are ground-based devices to measure the variation of cosmic ray intensities, and although being reliable they have two disadvantages: their size as well as their weight. As consequence, [1] suggested the development of a portable, and thus much smaller and lighter, calibration neutron monitor that can be carried to any existing station around the world [see 2; 3]. But this mini neutron monitor, moreover, can also be installed as an autonomous station at any location that provides ''office" conditions such as a) temperatures within the range of around 0 to less than 40 degree C as well as b) internet and c) power supply. However, the best location is when the material above the NM is minimized. In 2011 a mini Neutron Monitor was installed at the Neumayer III station in Antarctica as well as the German research vessel Polarstern, providing scientific data since January 2014 and October 2012, respectively. The Polarstern, which is in the possession of the Federal Republic of Germany represented by the Ministry of Education and Research and operated by the Alfred Wegener Institute, Helmholtz Centre for Polar and Marine Research and managed by the shipping company Laeisz, was specially designed for working in the polar seas and is currently one of the most sophisticated polar research vessels worldwide. It spends almost 310 days a year at sea usually being located in the waters of Antarctica between November and March while spending the northern summer months in Arctic waters. Therefore, the vessel scans the rigidity range below the atmospheric threshold and above 10 GV twice a year. In contrast to spacecraft measurements NM data are influenced by variations of the geomagnetic field as well as the atmospheric conditions. Thus, in order to interpret the data a detailed knowledge of the instrument sensitivity with geomagnetic latitude (rigidity) and atmospheric pressure is essential. In order to determine the atmospheric response data from the Neumayer III station here we will perform comparisons to other polar stations, resulting in an atmospheric pressure coefficient of 7.5‰/hPa, while the rigidity dependence will be determined experimentally by utilizing several latitude scans. Thereby, the atmospheric pressure and temperature correction will be discussed in more detail and the results of the latitude scan performed between October 2012 and March 2013 will be presented. Moreover, we will show that this latitude scan can also be described by using the yield function of [4].

After the exciting in-situ observations of the ter- mination shock and the entry of the Voyager 1 spacecraft in the heliosheath, there is a growing awareness of the signifi- cance of the physics of the outer heliosphere. Its understand- ing helps to clarify the structure of our immediate interstellar neighbourhood, contributes to the clarification of fundamen- tal astrophysical processes like the acceleration of charged particles at a steller wind termination shock, and also sheds light on the question to what extent interstellar-terrestrial re- lations are important for the environment of and on the Earth. Consequently, there are new seriously discussed suggestions for sending a modern spacecraft into the heliosheath and be- yond. One of those candidates is the Interstellar Heliopause Probe (IHP) that has been studied in a Technology Reference Study by ESA/ESTEC. Here, we discuss the science objec- tives and expected scientific performance of this mission.

[1] We have examined the 52-day average intensities of 1.2-GV electrons and positively charged nuclei of the same rigidity during the time period from 1978 to 2004. This time period covers a complete 22-year solar cycle plus data from 2000 to 2004 that can be used to examine the repetitive nature of the variations. The 11-year solar modulation changes both the electrons and nuclei intensities by similar overall factors ∼10 at 1.2 GV. Differences in the electron/nuclei modulation as exhibited by the e/nuclei ratios occur mainly between 1980–1984, 1990–1994, and 2000–2004. At these times the e/nuclei ratios increase or decrease by a factor ∼2 at 1.2 GV in close correspondence with the changes in solar magnetic polarity from positive to negative (1980) and negative to positive (1990). The e/nuclei ratio changes in 2000–2004 match those seen in 1980–1984, thus confirming the 22-year nature of the e/nuclei variations.

Two of the fundamental problems in modern cosmic ray astrophysics are 1) the determination of the local interstellar spectra of galactic cosmic rays at low energies (E∼1 GeV/N), and 2) the need for a correct quantitative treatment of particle propagation in turbulent magnetic fields. Both problems are linked to each other since the energy spectra measured in the vicinity of the Earth are altered by solar modulation, described by Parker’s transport equation. Computations done in the seventies predicted that the cosmic ray nuclei spectra are only weakly modulated over the poles of the Sun. The high heliospheric latitude ESA/NASA Ulysses mission, however, has measured strongly modulated energy spectra over the poles of the Sun around solar minimum, leading to a new understanding of the importance of the transport processes, especially the diffusion and drift coefficients, involved. Several attempts have been made to derive these parameters directly from the particle interaction with the turbulent magnetized plasma. Another approach is to utilize a cosmic ray propagation model and adjust the diffusion tensor so that the model “fits” in‐situ observations.

Cosmic ray particles respond to the heliospheric magnetic field in the expanding solar wind and its turbulence and therefore provide a unique probe for conditions in the changing heliosphere. During the last four years, concentrated around the solar minimum period of solar cycle 22, the exploration of the solar polar regions by the joint ESA/NASA mission Ulysses revealed the three-dimensional behavior of cosmic rays in the inner and middle heliosphere. Also during the last decades, the Pioneer and Voyager missions have greatly expanded our understanding of the structure and extent of the outer heliosphere. Simultaneously, numerical models describing the propagation of galactic cosmic rays are becoming sophisticated tools for interpreting and understanding these observations. We give an introduction to the subject of the modulation of galactic cosmic rays in the heliosphere during solar minimum. The modulation effects on cosmic rays of corotating interaction regions and their successors in the outer heliosphere are discussed in more detail by Gazis, McDonald et al. (1999) and McKibben, Jokipii et al. (1999) in this volume. Cosmic-ray observations from the Ulysses spacecraft at high heliographic latitudes are also described extensively in this volume by Kunow, Lee et al. (1999).

We investigate the intensity variation of low energy (∼6–23 MeV/N) heliospheric ions and of galactic protons (250–2200 MeV) observed by the Kiel Electron Telescope onboard the Ulysses spacecraft associated with Corotating Interaction Regions (CIR) from mid-1992 to end of June 1995. This period covers Ulysses’ transit to high southern latitudes, the south polar pass, return to the solar equator and ascent to the north pole up to 70°. We find that the flux of high energy protons exhibits a periodicity of about 26 days with a relative intensity variation of 10%. At latitudes below ∼50° the recurrent variations of galactic protons are in coincidence with the passage of CIRs and enhancements of low energies protons and alpha particles which are accelerated at the shocks of the CIRs. The modulation of galactic protons is observed up to high southern latitudes, where the signatures of a CIR are no longer visible in plasma or magnetic field data. The periodicity does not depend on latitude and its phase apparentl...

Ulysses, launched in October 1990, began its second out-of-ecliptic orbit in September 1997. In 2000/2001 the spacecraft passed from the south to the north polar regions of the Sun in the inner heliosphere. In contrast to the first rapid pole to pole passage in 1994/1995 close to solar minimum, Ulysses experiences now solar maximum conditions. The Kiel Electron Telescope (KET) measures also protons and alpha-particles in the energy range from 5 MeV/n to >2 GeV/n. To derive radial and latitudinal gradients for >2 GeV/n protons and alpha-particles, data from the Chicago instrument on board IMP-8 and the neutron monitor network have been used to determine the corresponding time profiles at Earth. We obtain a spatial distribution at solar maximum which differs greatly from the solar minimum distribution. A steady-state approximation, which was characterized by a small radial and significant latitudinal gradient at solar minimum, was interchanged with a highly variable one with a large radial and a small – consistent with zero – latitudinal gradient. A significant deviation from a spherically symmetric cosmic ray distribution following the reversal of the solar magnetic field in 2000/2001 has not been observed yet. A small deviation has only been observed at northern polar regions, showing an excess of particles instead of the expected depression. This indicates that the reconfiguration of the heliospheric magnetic field, caused by the reappearance of the northern polar coronal hole, starts dominating the modulation of galactic cosmic rays already at solar maximum.Key words. Interplanetary physics (cosmic rays; energetic particles) – Space plasma physics (charged particle motion and acceleration)

On studying the interactions of hydroxyquinoline and its watersoluble salts with substances commonly used to ointment preparation, the authors stated a large agreement between the decreases in release rate and the quotients of binding determined by equilibrium dialysis. Sodium carboxymethyl cellulose, zinc oxide, and talc react with these drugs to form bindings of some strength the impair the release of the drugs, whereas hydroxyethylcellulose and Aerosil behave indifferently.

Studies using the model according to Horsch and Kögel showed that the release kinetics of the suspended water-soluble (but not lipid-soluble) drugs hydroxyquinoline sulphate and hydroxy-quinoline sulphate--potassium sulphate from oleogels is of a zero order. Differences in drug dispersity do not affect the release rates. Oleogels containing the lipid-soluble hydroxyquinoline base yielded undersaturated solution ointments, the release kinetics of which can be stated by a semilogarithmic relationship. There exists a linear correlation between the release rates and the product of the lipid solubility of the drug and the reciprocal apparent distribution coefficient.