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1. Measurements of Cosmic Rays by a Mini‐Neutron Monitor at Neumayer III From 2014 to 2017

Author

M. Walter, C. Gnebner, B. Heber, K. Herbst, H. Krüger, H. G. Krüger, P. Kühl, H. P. Prokoph, and R. D. Strauss

Subjects
Galactic Cosmic Rays, mini neutron monitor, Forbush decreases, Meteorology. Climatology, QC851-999, Astrophysics, QB460-466
Abstract

Abstract A mini‐neutron monitor (MNM) was installed at the German Antarctic Neumayer III station, measuring the variation of galactic cosmic rays and searching for Forbush Decreases (FDs) caused by solar activities. Running continuously from 2014 until the end of 2017, the long‐term stability of the detector could be investigated. After correcting the air pressure and normalization to the 27 days running mean averages of the SANAE and TERA Neutron Monitors (NMs), the daily running mean count rates are compared with the SANAE and TERA NMs also installed in Antarctica. For most of the 14 FDs with magnitudes greater than 3, taken from the list compiled by the IZMIRAN group (http://spaceweather.izmiran.ru/eng/dbs.html), the three detectors show consistent particle flux variation, although the average rate of the MNM is more than a hundred times smaller. The light and low‐cost MNM is an ideal alternative to heavy and old NMs, especially at high altitudes and remote environments.

Published
2024
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2. Jovian Electrons in the Inner Heliosphere: Opportunities for Multi-spacecraft Observations and Modeling

Author

R. D. Strauss, N. Dresing, N. E. Engelbrecht, J. G. Mitchell, P. Kühl, S. Jensen, S. Fleth, B. Sánchez-Cano, A. Posner, J. S Rankin, C. O. Lee, J. P. van den Berg, S. E. S. Ferreira, and B. Heber

Subjects
Heliosphere, Interplanetary turbulence, Cosmic rays, Astrophysics, QB460-466
Abstract

In this paper we explore the idea of using multi-spacecraft observations of Jovian electrons to measure the 3D distribution of these particles in the inner heliosphere. We present simulations of Jovian electron intensities along selected spacecraft trajectories for 2021 and compare these, admittedly qualitatively, to these measurements. Using the data–model comparison we emphasize how such a study can be used to constrain the transport parameters in the inner heliosphere, and how this can lead to additional insight into energetic particle transport. Model results are also shown along the expected trajectories of selected spacecraft, including the off-ecliptic phase of the Solar Orbiter mission from 2025 onward. Lastly, we revisit the use of historical data and discuss upcoming missions that may contribute to Jovian electron measurements.

Published
2024
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3. A dense network of cosmic-ray neutron sensors for soil moisture observation in a highly instrumented pre-Alpine headwater catchment in Germany

Author

B. Fersch, T. Francke, M. Heistermann, M. Schrön, V. Döpper, J. Jakobi, G. Baroni, T. Blume, H. Bogena, C. Budach, T. Gränzig, M. Förster, A. Güntner, H.-J. Hendricks Franssen, M. Kasner, M. Köhli, B. Kleinschmit, H. Kunstmann, A. Patil, D. Rasche, L. Scheiffele, U. Schmidt, S. Szulc-Seyfried, J. Weimar, S. Zacharias, M. Zreda, B. Heber, R. Kiese, V. Mares, H. Mollenhauer, I. Völksch, and S. Oswald

Subjects
Environmental sciences, GE1-350, Geology, QE1-996.5
Abstract

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).

Published
2020
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4. Multi-point galactic cosmic ray measurements between 1 and 4.5 AU over a full solar cycle

Author

T. Honig, O. G. Witasse, H. Evans, P. Nieminen, E. Kuulkers, M. G. G. T. Taylor, B. Heber, J. Guo, and B. Sánchez-Cano

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

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.

Published
2019
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5. A Multi‐Purpose Heliophysics L4 Mission

Author

A. Posner, C. N. Arge, J. Staub, O. C. StCyr, D. Folta, S. K. Solanki, R. D. T. Strauss, F. Effenberger, A. Gandorfer, B. Heber, C. J. Henney, J. Hirzberger, S. I. Jones, P. Kühl, O. Malandraki, and V. J. Sterken

Subjects
space weather, solar wind, solar energetic particles, solar remote sensing, orbital analysis, cosmic dust, Meteorology. Climatology, QC851-999, Astrophysics, QB460-466
Abstract

Abstract The Earth‐Sun Lagrangian point 4 is a meta‐stable location at 1 AU from the Sun, 60° ahead of Earth's orbit. It has an uninterrupted view of the solar photosphere centered on W60, the Earth's nominal magnetic field connection to the Sun. Such a mission on its own would serve as a solar remote sensing observatory that would oversee the entire solar radiation hemisphere with significant relevance for protecting Moon and Mars explorers from radiation exposure. In combination with appropriately planned observatories at L1 and L5, the three spacecraft would provide 300° longitude coverage of photospheric magnetic field structure, and allow continuous viewing of both solar poles, with >3.6° elevation. Ideally, the L4 and L5 missions would orbit the Sun with a 7.2° inclination out of the heliographic equator, 14.5° out of the ecliptic plane. We discuss the impact of extending solar magnetic field observations in both longitude and latitude to improve global solar wind modeling and, with the development of local helioseismology, the potential for long‐term solar activity forecasting. Such a mission would provide a unique opportunity for interplanetary and interstellar dust science. It would significantly add to reliability of operational observations on fast coronal mass ejections directed at Earth and for human Mars explorers on their round‐trip journey. The L4 mission concept is technically feasible, and is scientifically compelling.

Published
2021
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6. Yield Function of the DOSimetry TELescope Count and Dose Rates Aboard the International Space Station

Author

A. S. Caprotti, M. Brüdern, S. Burmeister, B. Heber, and K. Herbst

Subjects
energetic particle measurements, galactic cosmic rays, yield function, Meteorology. Climatology, QC851-999, Astrophysics, QB460-466
Abstract

Abstract The Earth is constantly hit by energetic particles originating from galactic sources. The flux of these particles is altered by the magnetized solar wind in the heliosphere and the Earth's magnetic field. For this reason, the ability of a particle to approach a spacecraft in low Earth orbit depends on its energy and the position of the spacecraft within the Earth's magnetosphere. Moreover, there are some areas (radiation belts) where the particles are trapped for a long time and, therefore, the flux of energetic particles is particularly high. Occasionally, solar energetic particles contribute to the energetic particle flux too. DOSimetry TELescope (DOSTEL) is one of the instruments aboard the International Space Station (ISS) that monitors the radiation field within the European module Columbus. Because being installed inside the ISS, particles produced by the interaction between the “primary” radiation and the ISS materials are also measured. To describe the observations in such a complex radiation field, we follow the method by Caballero‐Lopez and Moraal (2012, Journal of Geophysical Research, 117[A12], A12103. doi:10.1029/2012JA017794) to compute the so‐called yield function using precise measurements of the proton and helium energy spectra obtained by alpha magnet spectrometer and the systematic variation of the DOSTEL measurements within the Earth's magnetosphere.

Published
2021
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7. Influence of the terrestrial magnetic field geometry on the cutoff rigidity of cosmic ray particles

Author

K. Herbst, A. Kopp, and B. Heber

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

Studies of the propagation of charged energetic particles in the Earth's magnetic field go back to Carl Størmer. In the end, his investigations finally lead to the definition of the so-called cutoff rigidity RC; that is, the minimum momentum per charge a particle must have in order to reach a certain geographical location. Employing Monte Carlo simulations with the PLANETOCOSMICS code we investigate the correlation between the geomagnetic field structure and the cutoff rigidity. We show that the geometry of the magnetic field has a considerable influence on the resulting cutoff rigidity distribution. Furthermore, we will present a simple geometry-based parameter, δB, which is able to reflect the location-dependent cutoff rigidity. We show that this correlation is also visible in the temporal evolution of the Earth's magnetic field, at least over the last 100 yr. Using latitude scans with neutron monitors, changes of the relative counting rates at different positions are calculated, showing small variations for, e.g., Kiel and Moscow, while large ones occur at Mexico City as well as on the British Virgin Islands.

Published
2013
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8. Comparative time-series analysis of MeV electron data by Ulysses and Pioneer 10/11 in the Jovian magnetosphere

Author

P. Dunzlaff, B. Heber, A. Kopp, and M. S. Potgieter

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

The dynamics of the Jovian magnetosphere is dominated by the planet's fast rotation with a period of ~ 10 h. Within the magnetosphere, this periodicity can in particular be seen in the temporal variation of the spectral index of MeV electrons: every ~ 10 h the counting rates show a maximum (minimum), while the spectral index shows a minimum (maximum) known as the Jovian "clock" mechanism. In this study we re-analyse Ulysses and Pioneer 10/11 data and show that another periodic modulation in the MeV electrons can be identified, manifested by local maxima of the spectral index and local minima of the counting rates. For Ulysses, this modulation can be observed throughout the magnetosphere near the magnetic equator, suggesting an azimuthal asymmetric distribution of MeV electrons near the current sheet. This modulation is found to trail the "clock" mechanism by ~ 3.25 h. The Pioneer 10 data, however, only show occasional evidence of the presence of these local maxima while there is no evidence of this modulation in the Pioneer 11 data. A comparison of the times of observed minor peaks and Ulysses' distance from the current sheet using a simple rigid disc model as well as the model of Khurana and Schwarzl (2005) is performed.

Published
2013
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9. STEREO/SEPT observations of upstream particle events: almost monoenergetic ion beams

Author

A. Klassen, R. Gómez-Herrero, R. Müller-Mellin, S. Böttcher, B. Heber, R. Wimmer-Schweingruber, and G. M. Mason

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

We present observations of Almost Monoenergetic Ion (AMI) events in the energy range of 100–1200 keV detected with the Solar Electron and Proton Telescope (SEPT) onboard both STEREO spacecraft. The energy spectrum of AMI events contain 1, 2, or 3 narrow peaks with the relative width at half maximum of 0.1–0.7 and their energy maxima varies for different events from 120 to 1200 keV. These events were detected close to the bow-shock (STEREO-A&B) and to the magnetopause at STEREO-B as well as unexpectedly far upstream of the bow-shock and far away from the magnetotail at distances up to 1100 RE (STEREO-B) and 1900 RE (STEREO-A). We discuss the origin of AMI events, the connection to the Earth's bow-shock and to the magnetosphere, and the conditions of the interplanetary medium and magnetosphere under which these AMI bursts occur. Evidence that the detected spectral peaks were caused by quasi-monoenergetic beams of protons, helium, and heavier ions are given. Furthermore, we present the spatial distribution of all AMI events from December 2006 until August 2007.

Published
2009
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10. Observations of recurrent cosmic ray decreases during solar cycles 22 and 23

Author

P. Dunzlaff, B. Heber, A. Kopp, O. Rother, R. Müller-Mellin, A. Klassen, R. Gómez-Herrero, and R. Wimmer-Schweingruber

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

During solar cycle 22, the modulation of several hundred MeV galactic cosmic rays (GCRs) by recurrent and transient cosmic ray decreases was observed by the Ulysses spacecraft on its descent towards the solar south pole. In solar cycle 23, Ulysses repeated this trajectory segment during a similar phase of the solar cycle, but with opposite heliospheric magnetic field polarity. Since cosmic ray propagation in the heliosphere should depend on drift effects, we determine in this study the latitudinal distribution of the amplitude of recurrent cosmic ray decreases in solar cycles 22 and 23. As long as we measure the recurrent plasma structures in situ, we find that these decreases behave nearly the same in both cycles. Measurements in the fast solar wind, however, show differences: in cycle 22 (A>0) the recurrent cosmic ray decreases show a clear maximum near 25° and are still present beyond 40°, whereas we see in cycle 23 (A

Published
2008
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11. Modelling cosmic ray intensities along the Ulysses trajectory

Author

D. C. Ndiitwani, S. E. S. Ferreira, M. S. Potgieter, and B. Heber

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

Time dependent cosmic ray modulation in the inner heliosphere is studied by comparing results from a 2-D, time-dependent cosmic ray transport model with Ulysses observations. A compound approach, which combines the effects of the global changes in the heliospheric magnetic field magnitude with drifts to establish a realistic time-dependence, in the diffusion and drift coefficients, are used. We show that this model results in realistic cosmic ray modulation from the Ulysses launch (1990) until recently (2004) when compared to 2.5-GV electron and proton and 1.2-GV electron and Helium observations from this spacecraft. This approach is also applied to compute radial gradients present in 2.5-GV cosmic ray electron and protons in the inner heliosphere. The observed latitude dependence for both positive and negative charged particles during both the fast latitude scan periods, corresponding to different solar activity conditions, could also be realistically computed. For this an additional reduction in particle drifts (compared to diffusion) toward solar maximum is needed. This results in a realistic charge-sign dependent modulation at solar maximum and the model is also applied to predict charge-sign dependent modulation up to the next expected solar minimum.

Published
2005
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12. Delay in solar energetic particle onsets at high heliographic latitudes

Author

S. Dalla, A. Balogh, S. Krucker, A. Posner, R. Müller-Mellin, J. D. Anglin, M. Y. Hofer, R. G. Marsden, T. R. Sanderson, B. Heber, M. Zhang, and R. B. McKibben

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

Ulysses observations have shown that solar energetic particles (SEPs) can easily reach high heliographic latitudes. To obtain information on the release and propagation of SEPs prior to their arrival at Ulysses, we analyse the onsets of nine large high-latitude particle events. We measure the onset times in several energy channels, and plot them versus inverse particle speed. This allows us to derive an experimental path length and time of release from the solar atmosphere. We repeat the procedure for near-Earth observations by Wind and SOHO. We find that the derived path lengths at Ulysses are 1.06 to 2.45 times the length of a Parker spiral magnetic field line connecting the spacecraft to the Sun. The time of particle release from the Sun is between 100 and 350 min later than the release time derived from in-ecliptic measurements. We find no evidence of correlation between the delay in release and the inverse of the speed of the CME associated with the event, or the inverse of the speed of the corresponding interplanetary shock. The main parameter determining the magnitude of the delay appears to be the difference in latitude between the flare and the footpoint of the spacecraft.Key words. Interplanetary physics (energetic particles) – Solar physics, astrophysics and astronomy (energetic particles, flares and mass ejections)

Published
2003
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13. Ulysses COSPIN observations of cosmic rays and solar energetic particles from the South Pole to the North Pole of the Sun during solar maximum

Author

R. B. McKibben, J. J. Connell, C. Lopate, M. Zhang, J. D. Anglin, A. Balogh, S. Dalla, T. R. Sanderson, R. G. Marsden, M. Y. Hofer, H. Kunow, A. Posner, and B. Heber

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

In 2000–2001 Ulysses passed from the south to the north polar regions of the Sun in the inner heliosphere, providing a snapshot of the latitudinal structure of cosmic ray modulation and solar energetic particle populations during a period near solar maximum. Observations from the COSPIN suite of energetic charged particle telescopes show that latitude variations in the cosmic ray intensity in the inner heliosphere are nearly non-existent near solar maximum, whereas small but clear latitude gradients were observed during the similar phase of Ulysses’ orbit near the 1994–95 solar minimum. At proton energies above ~10 MeV and extending up to >70 MeV, the intensities are often dominated by Solar Energetic Particles (SEPs) accelerated near the Sun in association with intense solar flares and large Coronal Mass Ejections (CMEs). At lower energies the particle intensities are almost constantly enhanced above background, most likely as a result of a mix of SEPs and particles accelerated by interplanetary shocks. Simultaneous high-latitude Ulysses and near-Earth observations show that most events that produce large flux increases near Earth also produce flux increases at Ulysses, even at the highest latitudes attained. Particle anisotropies during particle onsets at Ulysses are typically directed outwards from the Sun, suggesting either acceleration extending to high latitudes or efficient cross-field propagation somewhere inside the orbit of Ulysses. Both cosmic ray and SEP observations are consistent with highly efficient transport of energetic charged particles between the equatorial and polar regions and across the mean interplanetary magnetic fields in the inner heliosphere.Key words. Interplanetary physics (cosmic rays) – Solar physics, astrophysics and astronomy (energetic particles; flares and mass ejections)

Published
2003
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14. The Ulysses fast latitude scans: COSPIN/KET results

Author

B. Heber, G. Sarri, G. Wibberenz, C. Paizis, P. Ferrando, A. Raviart, A. Posner, R. Müller-Mellin, and H. Kunow

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

Ulysses, launched in October 1990, began its second out-of-ecliptic orbit in December 1997, and its second fast latitude scan in September 2000. In contrast to the first fast latitude scan in 1994/1995, during the second fast latitude scan solar activity was close to maximum. The solar magnetic field reversed its polarity around July 2000. While the first latitude scan mainly gave a snapshot of the spatial distribution of galactic cosmic rays, the second one is dominated by temporal variations. Solar particle increases are observed at all heliographic latitudes, including events that produce >250 MeV protons and 50 MeV electrons. Using observations from the University of Chicago’s instrument on board IMP8 at Earth, we find that most solar particle events are observed at both high and low latitudes, indicating either acceleration of these particles over a broad latitude range or an efficient latitudinal transport. The latter is supported by "quiet time" variations in the MeV electron background, if interpreted as Jovian electrons. No latitudinal gradient was found for >106 MeV galactic cosmic ray protons, during the solar maximum fast latitude scan. The electron to proton ratio remains constant and has practically the same value as in the previous solar maximum. Both results indicate that drift is of minor importance. It was expected that, with the reversal of the solar magnetic field and in the declining phase of the solar cycle, this ratio should increase. This was, however, not observed, probably because the transition to the new magnetic cycle was not completely terminated within the heliosphere, as indicated by the Ulysses magnetic field and solar wind measurements. We argue that the new AKey words. Interplanetary physics (cosmic rays; energetic particles; interplanetary magnetic fields)

Published
2003
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15. Charge-sign dependent modulation in the heliosphere over a 22-year cycle

Author

S. E. S. Ferreira, M. S. Potgieter, B. Heber, and H. Fichtner

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

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)

Published
2003
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18. ULYSSES observations of energetic particle acceleration and the superposed CME and CIR events of November 1992

Author

T. L. Lim, J. J. Quenby, M. K. Reuss, E. Keppler, H. Kunow, B. Heber, and R. J. Forsyth

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

During November 1992, a series of forward and reverse shocks passed the ULYSSES spacecraft. Spectral and anisotropy measurements are reported for protons and alpha particles between 0.28 and 6 MeV observed by the Energetic Particle Composition Experiment, data recorded by the Magnetometer Experiment and the high-energy (2.7–300 MeV) proton data from the Kiel Electron Telescope. An analysis of energetic particle, plasma and magnetometer data from ULYSSES has allowed a unique study of the corresponding arrival of fare particles, particles within a corotating interaction region and particles transported with a coronal mass ejection. We present an analysis of these data in terms of possible diffusive shock acceleration but conclude that this is likely to be incompatible with the short transit time of the particles. Shock drift acceleration of particles with energies 0.3 MeV/nucleon or solar acceleration followed by particle trapping behind the shock front are alternative possibilities.

Published
1996
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19. New Release Products: Combining the Relativistic Electron Alert System for Exploration With Other Early Indicators of Solar Energetic Particle Events

Author

A. Posner, O. Malandraki, M. Karavolos, K. Tziotziou, T. Smanis, B. Heber, H. Droge, A. Kollhoff, M. Laurenza, I.G. Richardson, and L. Zhao

Subjects
Solar Physics
Abstract

The Relativistic Electron Alert System for Exploration (“REleASE”) exploits the prompt arrival of near-relativistic electrons in the Earth/moon system to rapidly warn human explorers of the imminent arrival of hazardous energetic ions from solar energetic particle (SEP) events. Since 2008, the REleASE system has been implemented in near-real-time, initially with electron observations from SOHO, and since 2017 with additional observations from ACE as “HESPERIA REleASE”: upcoming opportunities will utilize IMAP and SWFO observations. REleASE is undergoing performance validation as part of the NASA/CCMC SEP scoreboarding process (https://ccmc.gsfc.nasa.gov/scoreboards/sep/). The ongoing return of STEREO-A to the vicinity of Earth provides observations of radio waves in near-real-time and allows REleASE to be combined with the identification of type-III radio bursts, which provide additional evidence of particle escape from the Sun (the use of type-III bursts for SEP forecasting was pioneered by “ESPERTA” developed by Laurenza et al., 2009). The aim of this planned “REleASE+” system is to further reduce the rate of false alarms. Another opportunity, facilitated by the CLEAR space weather center (PI L. Zhao, Univ. Michigan) will combine REleASE with “SEPSTER” (Richardson et al., 2018) to reduce the high rate of false alarms produced by SEPSTER, which is triggered by reports of CMEs, the vast majority of which do not result in detected SEP ion events. This presentation will give a status update on these objectives.

Published
2024

20. Temporal Structures in Positron Spectra and Charge-Sign Effects in Galactic Cosmic Rays

Author

M. Aguilar, G. Ambrosi, H. Anderson, L. Arruda, N. Attig, C. Bagwell, F. Barao, M. Barbanera, L. Barrin, A. Bartoloni, R. Battiston, N. Belyaev, J. Berdugo, B. Bertucci, V. Bindi, K. Bollweg, J. Bolster, M. Borchiellini, B. Borgia, M. J. Boschini, M. Bourquin, J. Burger, W. J. Burger, X. D. Cai, M. Capell, J. Casaus, G. Castellini, F. Cervelli, Y. H. Chang, G. M. Chen, G. R. Chen, H. Chen, H. S. Chen, Y. Chen, L. Cheng, H. Y. Chou, S. Chouridou, V. Choutko, C. H. Chung, C. Clark, G. Coignet, C. Consolandi, A. Contin, C. Corti, Z. Cui, K. Dadzie, F. D’Angelo, A. Dass, C. Delgado, S. Della Torre, M. B. Demirköz, L. Derome, S. Di Falco, V. Di Felice, C. Díaz, F. Dimiccoli, P. von Doetinchem, F. Dong, F. Donnini, M. Duranti, A. Egorov, A. Eline, F. Faldi, J. Feng, E. Fiandrini, P. Fisher, V. Formato, C. Gámez, R. J. García-López, C. Gargiulo, H. Gast, M. Gervasi, F. Giovacchini, D. M. Gómez-Coral, J. Gong, C. Goy, D. Grandi, M. Graziani, A. N. Guracho, S. Haino, K. C. Han, R. K. Hashmani, Z. H. He, B. Heber, T. H. Hsieh, J. Y. Hu, B. W. Huang, M. Ionica, M. Incagli, Yi Jia, H. Jinchi, G. Karagöz, S. Khan, B. Khiali, Th. Kirn, A. P. Klipfel, O. Kounina, A. Kounine, V. Koutsenko, D. Krasnopevtsev, A. Kuhlman, A. Kulemzin, G. La Vacca, E. Laudi, G. Laurenti, G. LaVecchia, I. Lazzizzera, H. T. Lee, S. C. Lee, H. L. Li, J. Q. Li, M. Li, Q. Li, Q. Y. Li, S. Li, S. L. Li, J. H. Li, Z. H. Li, J. Liang, M. J. Liang, C. H. Lin, T. Lippert, J. H. Liu, S. Q. Lu, Y. S. Lu, K. Luebelsmeyer, J. Z. Luo, S. D. Luo, Xi Luo, C. Mañá, J. Marín, J. Marquardt, T. Martin, G. Martínez, N. Masi, D. Maurin, T. Medvedeva, A. Menchaca-Rocha, Q. Meng, M. Molero, P. Mott, L. Mussolin, Y. Najafi Jozani, J. Negrete, R. Nicolaidis, N. Nikonov, F. Nozzoli, J. Ocampo-Peleteiro, A. Oliva, M. Orcinha, M. A. Ottupara, M. Palermo, F. Palmonari, M. Paniccia, A. Pashnin, M. Pauluzzi, S. Pensotti, V. Plyaskin, S. Poluianov, X. Qin, Z. Y. Qu, L. Quadrani, P. G. Rancoita, D. Rapin, A. Reina Conde, E. Robyn, I. Rodríguez-García, L. Romaneehsen, F. Rossi, A. Rozhkov, D. Rozza, R. Sagdeev, E. Savin, S. Schael, A. Schultz von Dratzig, G. Schwering, E. S. Seo, B. S. Shan, T. Siedenburg, G. Silvestre, J. W. Song, X. J. Song, R. Sonnabend, L. Strigari, T. Su, Q. Sun, Z. T. Sun, M. Tacconi, X. W. Tang, Z. C. Tang, J. Tian, Y. Tian, Samuel C. C. Ting, S. M. Ting, N. Tomassetti, J. Torsti, T. Urban, I. Usoskin, V. Vagelli, R. Vainio, M. Valencia-Otero, E. Valente, E. Valtonen, M. Vázquez Acosta, M. Vecchi, M. Velasco, J. P. Vialle, C. X. Wang, L. Wang, L. Q. Wang, N. H. Wang, Q. L. Wang, S. Wang, X. Wang, Yu Wang, Z. M. Wang, J. Wei, Z. L. Weng, H. Wu, Y. Wu, J. N. Xiao, R. Q. Xiong, X. Z. Xiong, W. Xu, Q. Yan, H. T. Yang, Y. Yang, A. Yelland, H. Yi, Y. H. You, Y. M. Yu, Z. Q. Yu, C. Zhang, F. Zhang, F. Z. Zhang, J. Zhang, J. H. Zhang, Z. Zhang, F. Zhao, C. Zheng, Z. M. Zheng, H. L. Zhuang, V. Zhukov, A. Zichichi, and P. Zuccon

Published
2023
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21. ULYSSES observations of energetic particle acceleration and the superposed CME and CIR events of November 1992

Author

T. L. Lim, J. J. Quenby, M. K. Reuss, E. Keppler, H. Kunow, B. Heber, and R. J. Forsyth

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

During November 1992, a series of forward and reverse shocks passed the ULYSSES spacecraft. Spectral and anisotropy measurements are reported for protons and alpha particles between 0.28 and 6 MeV observed by the Energetic Particle Composition Experiment, data recorded by the Magnetometer Experiment and the high-energy (2.7–300 MeV) proton data from the Kiel Electron Telescope. An analysis of energetic particle, plasma and magnetometer data from ULYSSES has allowed a unique study of the corresponding arrival of fare particles, particles within a corotating interaction region and particles transported with a coronal mass ejection. We present an analysis of these data in terms of possible diffusive shock acceleration but conclude that this is likely to be incompatible with the short transit time of the particles. Shock drift acceleration of particles with energies 0.3 MeV/nucleon or solar acceleration followed by particle trapping behind the shock front are alternative possibilities.

22. Properties of Cosmic-Ray Sulfur and Determination of the Composition of Primary Cosmic-Ray Carbon, Neon, Magnesium, and Sulfur: Ten-Year Results from the Alpha Magnetic Spectrometer

Author

M. Aguilar, L. Ali Cavasonza, B. Alpat, G. Ambrosi, L. Arruda, N. Attig, C. Bagwell, F. Barao, L. Barrin, A. Bartoloni, S. Başeğmez-du Pree, R. Battiston, N. Belyaev, J. Berdugo, B. Bertucci, V. Bindi, K. Bollweg, J. Bolster, M. Borchiellini, B. Borgia, M. J. Boschini, M. Bourquin, E. F. Bueno, J. Burger, W. J. Burger, X. D. Cai, M. Capell, J. Casaus, G. Castellini, F. Cervelli, Y. H. Chang, G. M. Chen, G. R. Chen, H. Chen, H. S. Chen, Y. Chen, L. Cheng, H. Y. Chou, S. Chouridou, V. Choutko, C. H. Chung, C. Clark, G. Coignet, C. Consolandi, A. Contin, C. Corti, Z. Cui, K. Dadzie, A. Dass, C. Delgado, S. Della Torre, M. B. Demirköz, L. Derome, S. Di Falco, V. Di Felice, C. Díaz, F. Dimiccoli, P. von Doetinchem, F. Dong, F. Donnini, M. Duranti, A. Egorov, A. Eline, F. Faldi, J. Feng, E. Fiandrini, P. Fisher, V. Formato, C. Gámez, R. J. García-López, C. Gargiulo, H. Gast, M. Gervasi, F. Giovacchini, D. M. Gómez-Coral, J. Gong, C. Goy, V. Grabski, D. Grandi, M. Graziani, A. N. Guracho, S. Haino, K. C. Han, R. K. Hashmani, Z. H. He, B. Heber, T. H. Hsieh, J. Y. Hu, B. W. Huang, M. Incagli, W. Y. Jang, Yi Jia, H. Jinchi, G. Karagöz, B. Khiali, G. N. Kim, Th. Kirn, O. Kounina, A. Kounine, V. Koutsenko, D. Krasnopevtsev, A. Kuhlman, A. Kulemzin, G. La Vacca, E. Laudi, G. Laurenti, G. LaVecchia, I. Lazzizzera, H. T. Lee, S. C. Lee, H. L. Li, J. Q. Li, M. Li, Q. Li, Q. Y. Li, S. Li, S. L. Li, J. H. Li, Z. H. Li, J. Liang, M. J. Liang, C. H. Lin, T. Lippert, J. H. Liu, S. Q. Lu, Y. S. Lu, K. Luebelsmeyer, J. Z. Luo, S. D. Luo, Xi Luo, F. Machate, C. Mañá, J. Marín, J. Marquardt, T. Martin, G. Martínez, N. Masi, D. Maurin, T. Medvedeva, A. Menchaca-Rocha, Q. Meng, V. V. Mikhailov, M. Molero, P. Mott, L. Mussolin, J. Negrete, N. Nikonov, F. Nozzoli, J. Ocampo-Peleteiro, A. Oliva, M. Orcinha, M. A. Ottupara, M. Palermo, F. Palmonari, M. Paniccia, A. Pashnin, M. Pauluzzi, S. Pensotti, V. Plyaskin, S. Poluianov, X. Qin, Z. Y. Qu, L. Quadrani, P. G. Rancoita, D. Rapin, A. Reina Conde, E. Robyn, L. Romaneehsen, A. Rozhkov, D. Rozza, R. Sagdeev, S. Schael, A. Schultz von Dratzig, G. Schwering, E. S. Seo, B. S. Shan, T. Siedenburg, J. W. Song, X. J. Song, R. Sonnabend, L. Strigari, T. Su, Q. Sun, Z. T. Sun, M. Tacconi, X. W. Tang, Z. C. Tang, J. Tian, Y. Tian, Samuel C. C. Ting, S. M. Ting, N. Tomassetti, J. Torsti, T. Urban, I. Usoskin, V. Vagelli, R. Vainio, M. Valencia-Otero, E. Valente, E. Valtonen, M. Vázquez Acosta, M. Vecchi, M. Velasco, J. P. Vialle, C. X. Wang, L. Wang, L. Q. Wang, N. H. Wang, Q. L. Wang, S. Wang, X. Wang, Yu Wang, Z. M. Wang, J. Wei, Z. L. Weng, H. Wu, Y. Wu, J. N. Xiao, R. Q. Xiong, X. Z. Xiong, W. Xu, Q. Yan, H. T. Yang, Y. Yang, I. I. Yashin, A. Yelland, H. Yi, Y. H. You, Y. M. Yu, Z. Q. Yu, M. Zannoni, C. Zhang, F. Zhang, F. Z. Zhang, J. Zhang, J. H. Zhang, Z. Zhang, F. Zhao, C. Zheng, Z. M. Zheng, H. L. Zhuang, V. Zhukov, A. Zichichi, and P. Zuccon

Published
2023
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23. Temporal Structures in Electron Spectra and Charge Sign Effects in Galactic Cosmic Rays

Author

M. Aguilar, L. Ali Cavasonza, G. Ambrosi, L. Arruda, N. Attig, C. Bagwell, F. Barao, L. Barrin, A. Bartoloni, S. Başeğmez-du Pree, R. Battiston, M. Behlmann, N. Belyaev, J. Berdugo, B. Bertucci, V. Bindi, K. Bollweg, J. Bolster, B. Borgia, M. J. Boschini, M. Bourquin, E. F. Bueno, J. Burger, W. J. Burger, S. Burmeister, X. D. Cai, M. Capell, J. Casaus, G. Castellini, F. Cervelli, Y. H. Chang, G. M. Chen, G. R. Chen, H. S. Chen, Y. Chen, L. Cheng, H. Y. Chou, S. Chouridou, V. Choutko, C. H. Chung, C. Clark, G. Coignet, C. Consolandi, A. Contin, C. Corti, Z. Cui, K. Dadzie, A. Dass, C. Delgado, S. Della Torre, M. B. Demirköz, L. Derome, S. Di Falco, V. Di Felice, C. Díaz, F. Dimiccoli, P. von Doetinchem, F. Dong, F. Donnini, M. Duranti, A. Egorov, A. Eline, F. Faldi, J. Feng, E. Fiandrini, P. Fisher, V. Formato, C. Freeman, C. Gámez, R. J. García-López, C. Gargiulo, H. Gast, M. Gervasi, F. Giovacchini, D. M. Gómez-Coral, J. Gong, C. Goy, V. Grabski, D. Grandi, M. Graziani, A. N. Guracho, S. Haino, K. C. Han, R. K. Hashmani, Z. H. He, B. Heber, T. H. Hsieh, J. Y. Hu, M. Incagli, W. Y. Jang, Yi Jia, H. Jinchi, G. Karagöz, B. Khiali, G. N. Kim, Th. Kirn, O. Kounina, A. Kounine, V. Koutsenko, D. Krasnopevtsev, A. Kuhlman, A. Kulemzin, G. La Vacca, E. Laudi, G. Laurenti, G. LaVecchia, I. Lazzizzera, H. T. Lee, S. C. Lee, H. L. Li, J. Q. Li, M. Li, Q. Li, Q. Y. Li, S. Li, S. L. Li, J. H. Li, Z. H. Li, J. Liang, M. J. Liang, C. Light, C. H. Lin, T. Lippert, J. H. Liu, S. Q. Lu, Y. S. Lu, K. Luebelsmeyer, J. Z. Luo, Xi Luo, F. Machate, C. Mañá, J. Marín, J. Marquardt, T. Martin, G. Martínez, N. Masi, D. Maurin, T. Medvedeva, A. Menchaca-Rocha, Q. Meng, V. V. Mikhailov, M. Molero, P. Mott, L. Mussolin, J. Negrete, N. Nikonov, F. Nozzoli, J. Ocampo-Peleteiro, A. Oliva, M. Orcinha, M. Palermo, F. Palmonari, M. Paniccia, A. Pashnin, M. Pauluzzi, S. Pensotti, V. Plyaskin, M. Pohl, S. Poluianov, X. Qin, Z. Y. Qu, L. Quadrani, P. G. Rancoita, D. Rapin, A. Reina Conde, E. Robyn, S. Rosier-Lees, A. Rozhkov, D. Rozza, R. Sagdeev, S. Schael, A. Schultz von Dratzig, G. Schwering, E. S. Seo, B. S. Shan, T. Siedenburg, J. W. Song, X. J. Song, R. Sonnabend, L. Strigari, T. Su, Q. Sun, Z. T. Sun, M. Tacconi, X. W. Tang, Z. C. Tang, J. Tian, Samuel C. C. Ting, S. M. Ting, N. Tomassetti, J. Torsti, T. Urban, I. Usoskin, V. Vagelli, R. Vainio, M. Valencia-Otero, E. Valente, E. Valtonen, M. Vázquez Acosta, M. Vecchi, M. Velasco, J. P. Vialle, C. X. Wang, L. Wang, L. Q. Wang, N. H. Wang, Q. L. Wang, S. Wang, X. Wang, Yu Wang, Z. M. Wang, J. Wei, Z. L. Weng, H. Wu, R. Q. Xiong, W. Xu, Q. Yan, Y. Yang, I. I. Yashin, A. Yelland, H. Yi, Y. M. Yu, Z. Q. Yu, M. Zannoni, C. Zhang, F. Zhang, F. Z. Zhang, J. H. Zhang, Z. Zhang, F. Zhao, C. Zheng, Z. M. Zheng, H. L. Zhuang, V. Zhukov, A. Zichichi, and P. Zuccon

Published
2023
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25. Sun Chaser - A Mission to the Earth-Sun Lagrangian Point 4

Author

A. Posner, S. K. Solanki, C. N. Arge, A. Bemporad, K.-S. Cho, Y. M. Collado-Vega, C. Dong, F. Effenberger, R. Filwett, A. Gandorfer, N. Hatten, B. Heber, C. J. Henney, D. Jha, S. Jones, P. Kühl, C. Lee, O. Malandraki, N. Nitta, Y.-D. Park, H. Peter, A. A. Pevtsov, J. Straub, O. C. StCyr, V. Sterken, R. D. T. Strauss, L. Upton, and K. Whitman

Subjects
Solar Physics
Abstract

Placed at L4, Sun Chaser is a mission concept that will follow (or chase) high-energy processes around the west limb, combining solar remote sensing & in situ observations, and overseeing the entire solar radiation hemisphere. Sun Chaser’s remote sensing is essential for ~90% of current physics-based and empirical solar energetic particle (SEP) event forecasting techniques. Without Sun Chaser, there cannot be a basis for SEP event all-clear forecasting. It establishes and maintains a space weather (SWx) radiation safe zone that supports all near-term human missions to the Moon and Mars. Sun Chaser latitude in-situ coverage also provides a unique opportunity for solar wind-, interplanetary- and interstellar-dust science. In combination with existing and planned observatories at L1 and L5, the three locations provide 240° longitude coverage of resolving photospheric magnetic field structure and safe Earth-directed CME viewing. A ~14°-inclination of both L4 and L5 out of the ecliptic guarantees continuous viewing of both solar poles and continuous in-situ presence on both sides of the heliographic equator, with >3.6° elevation. Extended observations in both longitude and latitude will revolutionize global solar wind modeling and immediate validation, and enables the development of local helioseismology, with potential for long-term solar activity forecasting.

Published
2022

26. Properties of Daily Helium Fluxes

Author

M. Aguilar, L. Ali Cavasonza, G. Ambrosi, L. Arruda, N. Attig, F. Barao, L. Barrin, A. Bartoloni, S. Başeğmez-du Pree, R. Battiston, M. Behlmann, J. Berdugo, B. Bertucci, V. Bindi, K. Bollweg, B. Borgia, M. J. Boschini, M. Bourquin, E. F. Bueno, J. Burger, W. J. Burger, S. Burmeister, X. D. Cai, M. Capell, J. Casaus, G. Castellini, F. Cervelli, Y. H. Chang, G. M. Chen, G. R. Chen, H. S. Chen, Y. Chen, L. Cheng, H. Y. Chou, S. Chouridou, V. Choutko, C. H. Chung, C. Clark, G. Coignet, C. Consolandi, A. Contin, C. Corti, Z. Cui, K. Dadzie, A. Dass, C. Delgado, S. Della Torre, M. B. Demirköz, L. Derome, S. Di Falco, V. Di Felice, C. Díaz, F. Dimiccoli, P. von Doetinchem, F. Dong, F. Donnini, M. Duranti, A. Egorov, A. Eline, J. Feng, E. Fiandrini, P. Fisher, V. Formato, C. Freeman, C. Gámez, R. J. García-López, C. Gargiulo, H. Gast, M. Gervasi, F. Giovacchini, D. M. Gómez-Coral, J. Gong, C. Goy, V. Grabski, D. Grandi, M. Graziani, S. Haino, K. C. Han, R. K. Hashmani, Z. H. He, B. Heber, T. H. Hsieh, J. Y. Hu, M. Incagli, W. Y. Jang, Yi Jia, H. Jinchi, G. Karagöz, B. Khiali, G. N. Kim, Th. Kirn, M. Konyushikhin, O. Kounina, A. Kounine, V. Koutsenko, D. Krasnopevtsev, A. Kuhlman, A. Kulemzin, G. La Vacca, E. Laudi, G. Laurenti, I. Lazzizzera, H. T. Lee, S. C. Lee, H. L. Li, J. Q. Li, M. Li, Q. Li, Q. Y. Li, S. Li, S. L. Li, J. H. Li, Z. H. Li, J. Liang, M. J. Liang, C. Light, C. H. Lin, T. Lippert, J. H. Liu, S. Q. Lu, Y. S. Lu, K. Luebelsmeyer, J. Z. Luo, Xi Luo, F. Machate, C. Mañá, J. Marín, J. Marquardt, T. Martin, G. Martínez, N. Masi, D. Maurin, T. Medvedeva, A. Menchaca-Rocha, Q. Meng, V. V. Mikhailov, M. Molero, P. Mott, L. Mussolin, J. Negrete, N. Nikonov, F. Nozzoli, J. Ocampo-Peleteiro, A. Oliva, M. Orcinha, M. Palermo, F. Palmonari, M. Paniccia, A. Pashnin, M. Pauluzzi, S. Pensotti, V. Plyaskin, M. Pohl, S. Poluianov, X. Qin, Z. Y. Qu, L. Quadrani, P. G. Rancoita, D. Rapin, A. Reina Conde, E. Robyn, S. Rosier-Lees, A. Rozhkov, D. Rozza, R. Sagdeev, S. Schael, A. Schultz von Dratzig, G. Schwering, E. S. Seo, B. S. Shan, T. Siedenburg, J. W. Song, X. J. Song, R. Sonnabend, L. Strigari, T. Su, Q. Sun, Z. T. Sun, M. Tacconi, X. W. Tang, Z. C. Tang, J. Tian, Samuel C. C. Ting, S. M. Ting, N. Tomassetti, J. Torsti, T. Urban, I. Usoskin, V. Vagelli, R. Vainio, M. Valencia-Otero, E. Valente, E. Valtonen, M. Vázquez Acosta, M. Vecchi, M. Velasco, J. P. Vialle, C. X. Wang, L. Wang, L. Q. Wang, N. H. Wang, Q. L. Wang, S. Wang, X. Wang, Yu Wang, Z. M. Wang, J. Wei, Z. L. Weng, H. Wu, R. Q. Xiong, W. Xu, Q. Yan, Y. Yang, I. I. Yashin, H. Yi, Y. M. Yu, Z. Q. Yu, M. Zannoni, C. Zhang, F. Zhang, F. Z. Zhang, J. H. Zhang, Z. Zhang, F. Zhao, C. Zheng, Z. M. Zheng, H. L. Zhuang, V. Zhukov, A. Zichichi, and P. Zuccon

Published
2022
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28. Periodicities in the Daily Proton Fluxes from 2011 to 2019 Measured by the Alpha Magnetic Spectrometer on the International Space Station from 1 to 100 GV

Author

M. Aguilar, L. Ali Cavasonza, G. Ambrosi, L. Arruda, N. Attig, F. Barao, L. Barrin, A. Bartoloni, S. Başeğmez-du Pree, R. Battiston, M. Behlmann, B. Beranek, J. Berdugo, B. Bertucci, V. Bindi, K. Bollweg, B. Borgia, M. J. Boschini, M. Bourquin, E. F. Bueno, J. Burger, W. J. Burger, S. Burmeister, X. D. Cai, M. Capell, J. Casaus, G. Castellini, F. Cervelli, Y. H. Chang, G. M. Chen, G. R. Chen, H. S. Chen, Y. Chen, L. Cheng, H. Y. Chou, S. Chouridou, V. Choutko, C. H. Chung, C. Clark, G. Coignet, C. Consolandi, A. Contin, C. Corti, Z. Cui, K. Dadzie, A. Dass, C. Delgado, S. Della Torre, M. B. Demirköz, L. Derome, S. Di Falco, V. Di Felice, C. Díaz, F. Dimiccoli, P. von Doetinchem, F. Dong, F. Donnini, M. Duranti, A. Egorov, A. Eline, J. Feng, E. Fiandrini, P. Fisher, V. Formato, C. Freeman, C. Gámez, R. J. García-López, C. Gargiulo, H. Gast, M. Gervasi, F. Giovacchini, D. M. Gómez-Coral, J. Gong, C. Goy, V. Grabski, D. Grandi, M. Graziani, S. Haino, K. C. Han, R. K. Hashmani, Z. H. He, B. Heber, T. H. Hsieh, J. Y. Hu, M. Incagli, W. Y. Jang, Yi Jia, H. Jinchi, G. Karagöz, B. Khiali, G. N. Kim, Th. Kirn, M. Konyushikhin, O. Kounina, A. Kounine, V. Koutsenko, D. Krasnopevtsev, A. Kuhlman, A. Kulemzin, G. La Vacca, E. Laudi, G. Laurenti, I. Lazzizzera, A. Lebedev, H. T. Lee, S. C. Lee, J. Q. Li, M. Li, Q. Li, S. Li, J. H. Li, Z. H. Li, J. Liang, C. Light, C. H. Lin, T. Lippert, J. H. Liu, Z. Liu, S. Q. Lu, Y. S. Lu, K. Luebelsmeyer, J. Z. Luo, Xi Luo, F. Machate, C. Mañá, J. Marín, J. Marquardt, T. Martin, G. Martínez, N. Masi, D. Maurin, T. Medvedeva, A. Menchaca-Rocha, Q. Meng, V. V. Mikhailov, M. Molero, P. Mott, L. Mussolin, J. Negrete, N. Nikonov, F. Nozzoli, A. Oliva, M. Orcinha, M. Palermo, F. Palmonari, M. Paniccia, A. Pashnin, M. Pauluzzi, S. Pensotti, H. D. Phan, V. Plyaskin, M. Pohl, S. Poluianov, X. Qin, Z. Y. Qu, L. Quadrani, P. G. Rancoita, D. Rapin, A. Reina Conde, E. Robyn, S. Rosier-Lees, A. Rozhkov, D. Rozza, R. Sagdeev, S. Schael, A. Schultz von Dratzig, G. Schwering, E. S. Seo, Z. Shakfa, B. S. Shan, T. Siedenburg, C. Solano, J. W. Song, X. J. Song, R. Sonnabend, L. Strigari, T. Su, Q. Sun, Z. T. Sun, M. Tacconi, X. W. Tang, Z. C. Tang, J. Tian, Samuel C. C. Ting, S. M. Ting, N. Tomassetti, J. Torsti, T. Urban, I. Usoskin, V. Vagelli, R. Vainio, M. Valencia-Otero, E. Valente, E. Valtonen, M. Vázquez Acosta, M. Vecchi, M. Velasco, J. P. Vialle, C. X. Wang, L. Wang, L. Q. Wang, N. H. Wang, Q. L. Wang, S. Wang, X. Wang, Yu Wang, Z. M. Wang, J. Wei, Z. L. Weng, H. Wu, R. Q. Xiong, W. Xu, Q. Yan, Y. Yang, I. I. Yashin, H. Yi, Y. M. Yu, Z. Q. Yu, M. Zannoni, C. Zhang, F. Zhang, F. Z. Zhang, J. H. Zhang, Z. Zhang, F. Zhao, C. Zheng, Z. M. Zheng, H. L. Zhuang, V. Zhukov, A. Zichichi, and P. Zuccon

Published
2021
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29. Properties of a New Group of Cosmic Nuclei: Results from the Alpha Magnetic Spectrometer on Sodium, Aluminum, and Nitrogen

Author

M. Aguilar, L. Ali Cavasonza, B. Alpat, G. Ambrosi, L. Arruda, N. Attig, F. Barao, L. Barrin, A. Bartoloni, S. Başeğmez-du Pree, R. Battiston, M. Behlmann, B. Beranek, J. Berdugo, B. Bertucci, V. Bindi, K. Bollweg, B. Borgia, M. J. Boschini, M. Bourquin, E. F. Bueno, J. Burger, W. J. Burger, S. Burmeister, X. D. Cai, M. Capell, J. Casaus, G. Castellini, F. Cervelli, Y. H. Chang, G. M. Chen, G. R. Chen, H. S. Chen, Y. Chen, L. Cheng, H. Y. Chou, S. Chouridou, V. Choutko, C. H. Chung, C. Clark, G. Coignet, C. Consolandi, A. Contin, C. Corti, Z. Cui, K. Dadzie, C. Delgado, S. Della Torre, M. B. Demirköz, L. Derome, S. Di Falco, V. Di Felice, C. Díaz, F. Dimiccoli, P. von Doetinchem, F. Dong, F. Donnini, M. Duranti, A. Egorov, A. Eline, J. Feng, E. Fiandrini, P. Fisher, V. Formato, C. Freeman, C. Gámez, R. J. García-López, C. Gargiulo, H. Gast, M. Gervasi, F. Giovacchini, D. M. Gómez-Coral, J. Gong, C. Goy, V. Grabski, D. Grandi, M. Graziani, S. Haino, K. C. Han, R. K. Hashmani, Z. H. He, B. Heber, T. H. Hsieh, J. Y. Hu, M. Incagli, W. Y. Jang, Yi Jia, H. Jinchi, B. Khiali, G. N. Kim, Th. Kirn, M. Konyushikhin, O. Kounina, A. Kounine, V. Koutsenko, D. Krasnopevtsev, A. Kuhlman, A. Kulemzin, G. La Vacca, E. Laudi, G. Laurenti, I. Lazzizzera, A. Lebedev, H. T. Lee, S. C. Lee, J. Q. Li, M. Li, Q. Li, S. Li, J. H. Li, Z. H. Li, J. Liang, C. Light, C. H. Lin, T. Lippert, J. H. Liu, Z. Liu, S. Q. Lu, Y. S. Lu, K. Luebelsmeyer, J. Z. Luo, Xi Luo, F. Machate, C. Mañá, J. Marín, J. Marquardt, T. Martin, G. Martínez, N. Masi, D. Maurin, T. Medvedeva, A. Menchaca-Rocha, Q. Meng, V. V. Mikhailov, M. Molero, P. Mott, L. Mussolin, J. Negrete, N. Nikonov, F. Nozzoli, A. Oliva, M. Orcinha, M. Palermo, F. Palmonari, M. Paniccia, A. Pashnin, M. Pauluzzi, S. Pensotti, H. D. Phan, V. Plyaskin, M. Pohl, S. Poluianov, X. Qin, Z. Y. Qu, L. Quadrani, P. G. Rancoita, D. Rapin, A. Reina Conde, E. Robyn, S. Rosier-Lees, A. Rozhkov, D. Rozza, R. Sagdeev, S. Schael, A. Schulz von Dratzig, G. Schwering, E. S. Seo, Z. Shakfa, B. S. Shan, T. Siedenburg, C. Solano, J. W. Song, X. J. Song, R. Sonnabend, L. Strigari, T. Su, Q. Sun, Z. T. Sun, M. Tacconi, X. W. Tang, Z. C. Tang, J. Tian, Samuel C. C. Ting, S. M. Ting, N. Tomassetti, J. Torsti, C. Tüysüz, T. Urban, I. Usoskin, V. Vagelli, R. Vainio, M. Valencia-Otero, E. Valente, E. Valtonen, M. Vázquez Acosta, M. Vecchi, M. Velasco, J. P. Vialle, C. X. Wang, L. Wang, L. Q. Wang, N. H. Wang, Q. L. Wang, S. Wang, X. Wang, Yu Wang, Z. M. Wang, J. Wei, Z. L. Weng, H. Wu, R. Q. Xiong, W. Xu, Q. Yan, Y. Yang, I. I. Yashin, H. Yi, Y. M. Yu, Z. Q. Yu, M. Zannoni, C. Zhang, F. Zhang, F. Z. Zhang, J. H. Zhang, Z. Zhang, F. Zhao, C. Zheng, Z. M. Zheng, H. L. Zhuang, V. Zhukov, A. Zichichi, and P. Zuccon

Published
2021
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30. Properties of Heavy Secondary Fluorine Cosmic Rays: Results from the Alpha Magnetic Spectrometer

Author

M. Aguilar, L. Ali Cavasonza, M. S. Allen, B. Alpat, G. Ambrosi, L. Arruda, N. Attig, F. Barao, L. Barrin, A. Bartoloni, S. Başeğmez-du Pree, R. Battiston, M. Behlmann, B. Beranek, J. Berdugo, B. Bertucci, V. Bindi, K. Bollweg, B. Borgia, M. J. Boschini, M. Bourquin, E. F. Bueno, J. Burger, W. J. Burger, S. Burmeister, X. D. Cai, M. Capell, J. Casaus, G. Castellini, F. Cervelli, Y. H. Chang, G. M. Chen, G. R. Chen, H. S. Chen, Y. Chen, L. Cheng, H. Y. Chou, S. Chouridou, V. Choutko, C. H. Chung, C. Clark, G. Coignet, C. Consolandi, A. Contin, C. Corti, Z. Cui, K. Dadzie, C. Delgado, S. Della Torre, M. B. Demirköz, L. Derome, S. Di Falco, V. Di Felice, C. Díaz, F. Dimiccoli, P. von Doetinchem, F. Dong, F. Donnini, M. Duranti, A. Egorov, A. Eline, J. Feng, E. Fiandrini, P. Fisher, V. Formato, C. Freeman, Y. Galaktionov, C. Gámez, R. J. García-López, C. Gargiulo, H. Gast, M. Gervasi, F. Giovacchini, D. M. Gómez-Coral, J. Gong, C. Goy, V. Grabski, D. Grandi, M. Graziani, S. Haino, K. C. Han, R. K. Hashmani, Z. H. He, B. Heber, T. H. Hsieh, J. Y. Hu, M. Incagli, W. Y. Jang, Yi Jia, H. Jinchi, K. Kanishev, B. Khiali, G. N. Kim, Th. Kirn, M. Konyushikhin, O. Kounina, A. Kounine, V. Koutsenko, A. Kuhlman, A. Kulemzin, G. La Vacca, E. Laudi, G. Laurenti, I. Lazzizzera, A. Lebedev, H. T. Lee, S. C. Lee, J. Q. Li, M. Li, Q. Li, S. Li, J. H. Li, Z. H. Li, J. Liang, C. Light, C. H. Lin, T. Lippert, J. H. Liu, Z. Liu, S. Q. Lu, Y. S. Lu, K. Luebelsmeyer, J. Z. Luo, Xi Luo, S. S. Lyu, F. Machate, C. Mañá, J. Marín, J. Marquardt, T. Martin, G. Martínez, N. Masi, D. Maurin, A. Menchaca-Rocha, Q. Meng, V. V. Mikhailov, D. C. Mo, M. Molero, P. Mott, L. Mussolin, J. Negrete, N. Nikonov, F. Nozzoli, A. Oliva, M. Orcinha, M. Palermo, F. Palmonari, M. Paniccia, A. Pashnin, M. Pauluzzi, S. Pensotti, H. D. Phan, R. Piandani, V. Plyaskin, S. Poluianov, X. Qin, Z. Y. Qu, L. Quadrani, P. G. Rancoita, D. Rapin, A. Reina Conde, E. Robyn, S. Rosier-Lees, A. Rozhkov, D. Rozza, R. Sagdeev, S. Schael, A. Schulz von Dratzig, G. Schwering, E. S. Seo, Z. Shakfa, B. S. Shan, T. Siedenburg, C. Solano, J. W. Song, X. J. Song, R. Sonnabend, L. Strigari, T. Su, Q. Sun, Z. T. Sun, M. Tacconi, X. W. Tang, Z. C. Tang, J. Tian, Samuel C. C. Ting, S. M. Ting, N. Tomassetti, J. Torsti, C. Tüysüz, T. Urban, I. Usoskin, V. Vagelli, R. Vainio, M. Valencia-Otero, E. Valente, E. Valtonen, M. Vázquez Acosta, M. Vecchi, M. Velasco, J. P. Vialle, C. X. Wang, L. Wang, L. Q. Wang, N. H. Wang, Q. L. Wang, S. Wang, X. Wang, Yu Wang, Z. M. Wang, J. Wei, Z. L. Weng, H. Wu, R. Q. Xiong, W. Xu, Q. Yan, Y. Yang, I. I. Yashin, H. Yi, Y. M. Yu, Z. Q. Yu, M. Zannoni, C. Zhang, F. Zhang, F. Z. Zhang, J. H. Zhang, Z. Zhang, F. Zhao, C. Zheng, Z. M. Zheng, H. L. Zhuang, V. Zhukov, A. Zichichi, and P. Zuccon

Published
2021
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31. Properties of Iron Primary Cosmic Rays: Results from the Alpha Magnetic Spectrometer

Author

M. Aguilar, L. Ali Cavasonza, M. S. Allen, B. Alpat, G. Ambrosi, L. Arruda, N. Attig, F. Barao, L. Barrin, A. Bartoloni, S. Başeğmez-du Pree, R. Battiston, M. Behlmann, B. Beischer, J. Berdugo, B. Bertucci, V. Bindi, W. de Boer, K. Bollweg, B. Borgia, M. J. Boschini, M. Bourquin, E. F. Bueno, J. Burger, W. J. Burger, S. Burmeister, X. D. Cai, M. Capell, J. Casaus, G. Castellini, F. Cervelli, Y. H. Chang, G. M. Chen, G. R. Chen, H. S. Chen, Y. Chen, L. Cheng, H. Y. Chou, S. Chouridou, V. Choutko, C. H. Chung, C. Clark, G. Coignet, C. Consolandi, A. Contin, C. Corti, Z. Cui, K. Dadzie, C. Delgado, S. Della Torre, M. B. Demirköz, L. Derome, S. Di Falco, V. Di Felice, C. Díaz, F. Dimiccoli, P. von Doetinchem, F. Dong, F. Donnini, M. Duranti, A. Egorov, A. Eline, J. Feng, E. Fiandrini, P. Fisher, V. Formato, C. Freeman, Y. Galaktionov, C. Gámez, R. J. García-López, C. Gargiulo, H. Gast, M. Gervasi, F. Giovacchini, D. M. Gómez-Coral, J. Gong, C. Goy, V. Grabski, D. Grandi, M. Graziani, S. Haino, K. C. Han, R. K. Hashmani, Z. H. He, B. Heber, T. H. Hsieh, J. Y. Hu, M. Incagli, W. Y. Jang, Yi Jia, H. Jinchi, K. Kanishev, B. Khiali, G. N. Kim, Th. Kirn, M. Konyushikhin, O. Kounina, A. Kounine, V. Koutsenko, A. Kuhlman, A. Kulemzin, G. La Vacca, E. Laudi, G. Laurenti, I. Lazzizzera, A. Lebedev, H. T. Lee, S. C. Lee, J. Q. Li, M. Li, Q. Li, S. Li, J. H. Li, Z. H. Li, J. Liang, C. Light, C. H. Lin, T. Lippert, J. H. Liu, Z. Liu, S. Q. Lu, Y. S. Lu, K. Luebelsmeyer, J. Z. Luo, Xi Luo, S. S. Lyu, F. Machate, C. Mañá, J. Marín, J. Marquardt, T. Martin, G. Martínez, N. Masi, D. Maurin, A. Menchaca-Rocha, Q. Meng, V. V. Mikhailov, D. C. Mo, M. Molero, P. Mott, L. Mussolin, J. Negrete, N. Nikonov, F. Nozzoli, A. Oliva, M. Orcinha, M. Palermo, F. Palmonari, M. Paniccia, A. Pashnin, M. Pauluzzi, S. Pensotti, H. D. Phan, R. Piandani, V. Plyaskin, S. Poluianov, X. Qin, Z. Y. Qu, L. Quadrani, P. G. Rancoita, D. Rapin, A. Reina Conde, E. Robyn, S. Rosier-Lees, A. Rozhkov, D. Rozza, R. Sagdeev, S. Schael, A. Schulz von Dratzig, G. Schwering, E. S. Seo, Z. Shakfa, B. S. Shan, T. Siedenburg, C. Solano, J. W. Song, X. J. Song, R. Sonnabend, L. Strigari, T. Su, Q. Sun, Z. T. Sun, M. Tacconi, X. W. Tang, Z. C. Tang, J. Tian, Samuel C. C. Ting, S. M. Ting, N. Tomassetti, J. Torsti, C. Tüysüz, T. Urban, I. Usoskin, V. Vagelli, R. Vainio, M. Valencia-Otero, E. Valente, E. Valtonen, M. Vázquez Acosta, M. Vecchi, M. Velasco, J. P. Vialle, C. X. Wang, L. Wang, L. Q. Wang, N. H. Wang, Q. L. Wang, S. Wang, X. Wang, Yu Wang, Z. M. Wang, J. Wei, Z. L. Weng, H. Wu, R. Q. Xiong, W. Xu, Q. Yan, Y. Yang, I. I. Yashin, H. Yi, Y. M. Yu, Z. Q. Yu, M. Zannoni, C. Zhang, F. Zhang, F. Z. Zhang, J. H. Zhang, Z. Zhang, F. Zhao, C. Zheng, Z. M. Zheng, H. L. Zhuang, V. Zhukov, A. Zichichi, N. Zimmermann, and P. Zuccon

Published
2021
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32. Properties of Neon, Magnesium, and Silicon Primary Cosmic Rays Results from the Alpha Magnetic Spectrometer

Author

M. Aguilar, L. Ali Cavasonza, G. Ambrosi, L. Arruda, N. Attig, F. Barao, L. Barrin, A. Bartoloni, S. Başeğmez-du Pree, R. Battiston, U. Becker, M. Behlmann, B. Beischer, J. Berdugo, B. Bertucci, V. Bindi, W. de Boer, K. Bollweg, B. Borgia, M. J. Boschini, M. Bourquin, E. F. Bueno, J. Burger, W. J. Burger, S. Burmeister, X. D. Cai, M. Capell, J. Casaus, G. Castellini, F. Cervelli, Y. H. Chang, G. M. Chen, H. S. Chen, Y. Chen, L. Cheng, H. Y. Chou, S. Chouridou, V. Choutko, C. H. Chung, C. Clark, G. Coignet, C. Consolandi, A. Contin, C. Corti, Z. Cui, K. Dadzie, Y. M. Dai, C. Delgado, S. Della Torre, M. B. Demirköz, L. Derome, S. Di Falco, V. Di Felice, C. Díaz, F. Dimiccoli, P. von Doetinchem, F. Dong, F. Donnini, M. Duranti, A. Egorov, A. Eline, J. Feng, E. Fiandrini, P. Fisher, V. Formato, C. Freeman, Y. Galaktionov, C. Gámez, R. J. García-López, C. Gargiulo, H. Gast, I. Gebauer, M. Gervasi, F. Giovacchini, D. M. Gómez-Coral, J. Gong, C. Goy, V. Grabski, D. Grandi, M. Graziani, K. H. Guo, S. Haino, K. C. Han, R. K. Hashmani, Z. H. He, B. Heber, T. H. Hsieh, J. Y. Hu, Z. C. Huang, M. Incagli, W. Y. Jang, Yi Jia, H. Jinchi, K. Kanishev, B. Khiali, G. N. Kim, Th. Kirn, M. Konyushikhin, O. Kounina, A. Kounine, V. Koutsenko, A. Kuhlman, A. Kulemzin, G. La Vacca, E. Laudi, G. Laurenti, I. Lazzizzera, A. Lebedev, H. T. Lee, S. C. Lee, J. Q. Li, M. Li, Q. Li, S. Li, T. X. Li, Z. H. Li, C. Light, C. H. Lin, T. Lippert, Z. Liu, S. Q. Lu, Y. S. Lu, K. Luebelsmeyer, J. Z. Luo, S. S. Lyu, F. Machate, C. Mañá, J. Marín, J. Marquardt, T. Martin, G. Martínez, N. Masi, D. Maurin, A. Menchaca-Rocha, Q. Meng, D. C. Mo, M. Molero, P. Mott, L. Mussolin, J. Q. Ni, N. Nikonov, F. Nozzoli, A. Oliva, M. Orcinha, M. Palermo, F. Palmonari, M. Paniccia, A. Pashnin, M. Pauluzzi, S. Pensotti, H. D. Phan, R. Piandani, V. Plyaskin, S. Poluianov, X. M. Qi, X. Qin, Z. Y. Qu, L. Quadrani, P. G. Rancoita, D. Rapin, A. Reina Conde, S. Rosier-Lees, A. Rozhkov, D. Rozza, R. Sagdeev, S. Schael, S. M. Schmidt, A. Schulz von Dratzig, G. Schwering, E. S. Seo, B. S. Shan, J. Y. Shi, T. Siedenburg, C. Solano, R. Sonnabend, J. W. Song, Q. Sun, Z. T. Sun, M. Tacconi, X. W. Tang, Z. C. Tang, J. Tian, Samuel C. C. Ting, S. M. Ting, N. Tomassetti, J. Torsti, C. Tüysüz, T. Urban, I. Usoskin, V. Vagelli, R. Vainio, E. Valente, E. Valtonen, M. Vázquez Acosta, M. Vecchi, M. Velasco, J. P. Vialle, C. Wallmann, L. Q. Wang, N. H. Wang, Q. L. Wang, S. Wang, X. Wang, Z. X. Wang, J. Wei, Z. L. Weng, H. Wu, R. Q. Xiong, W. Xu, Q. Yan, Y. Yang, H. Yi, Y. J. Yu, Z. Q. Yu, M. Zannoni, C. Zhang, F. Zhang, F. Z. Zhang, J. H. Zhang, Z. Zhang, F. Zhao, Z. M. Zheng, H. L. Zhuang, V. Zhukov, A. Zichichi, N. Zimmermann, and P. Zuccon

Published
2020
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34. Anxiety, depression and excessive use of the Internet in the quality of sleep of students of veterinary medicine and zootechnics

Author

Chui B., Heber, Pérez A., Katia, Roque H., Edgar, Sumari M., Regina, and Roque H., Bernardo

Subjects
calidad de sueño, estudiantes universitarios, uso excesivo de internet, sleep quality, university students, excessive internet use, mental health, salud mental
Abstract

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

Published
2023

35. Requerimientos de energia metabolizable para mantenimiento y ganancia de peso de llamas y alpacas determinados mediante la tecnica de sacrificio comparativo

Author

Roque H., Bernardo, Bautista P., José, Beltrán B., Pablo, Calsín C., Bilo, Medina S., Juan, Aro A., Juan, Araníbar A., Marcelino, Sumari M., Regina, Benito L., Diannett, Marca C., Uriel, Huareccallo M., Juan, Pari H., José, Ramírez A., José, Condori A., Evilio, Roque H., Edgar, Chui B., Heber, and Pinares Patiño, César S.

Published
2020
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36. Anomalous Cosmic Rays and Heliospheric Energetic Particles

Author

J. Giacalone, H. Fahr, H. Fichtner, V. Florinski, B. Heber, M. E. Hill, J. Kóta, R. A. Leske, M. S. Potgieter, and J. S. Rankin

Subjects
Space and Planetary Science, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astronomy and Astrophysics, ddc:530
Abstract

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.

Published
2022

37. Generic profile of a long-lived corotating interaction region and associated recurrent Forbush decrease

Author

M. Dumbović, B. Vršnak, M. Temmer, B. Heber, and P. Kühl

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Plasma Physics (physics.plasm-ph), Astrophysics - Solar and Stellar Astrophysics, Physics - Space Physics, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, solar-terrestrial relations, solar wind, interplanetary medium, Physics - Plasma Physics, Solar and Stellar Astrophysics (astro-ph.SR), Space Physics (physics.space-ph)
Abstract

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

Published
2022
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38. The first widespread solar energetic particle event observed by Solar Orbiter on 2020 November 29

Author

A. Kollhoff, A. Kouloumvakos, D. Lario, N. Dresing, R. Gómez-Herrero, L. Rodríguez-García, O. E. Malandraki, I. G. Richardson, A. Posner, K.-L. Klein, D. Pacheco, A. Klassen, B. Heber, C. M. S. Cohen, T. Laitinen, I. Cernuda, S. Dalla, F. Espinosa Lara, R. Vainio, M. Köberle, R. Kühl, Z. G. Xu, L. Berger, S. Eldrum, M. Brüdern, M. Laurenza, E. J. Kilpua, A. Aran, A. P. Rouillard, R. Bučík, N. Wijsen, J. Pomoell, R. F. Wimmer-Schweingruber, C. Martin, S. I. Böttcher, J. L. Freiherr von Forstner, J.-C. Terasa, S. Boden, S. R. Kulkarni, A. Ravanbakhsh, M. Yedla, N. Janitzek, J. Rodríguez-Pacheco, M. Prieto Mateo, S. Sánchez Prieto, P. Parra Espada, O. Rodríguez Polo, A. Martínez Hellín, F. Carcaboso, G. M. Mason, G. C. Ho, R. C. Allen, G. Bruce Andrews, C. E. Schlemm, H. Seifert, K. Tyagi, W. J. Lees, J. Hayes, S. D. Bale, V. Krupar, T. S. Horbury, V. Angelini, V. Evans, H. O’Brien, M. Maksimovic, Yu. V. Khotyaintsev, A. Vecchio, K. Steinvall, E. Asvestari, German Research Foundation, National Aeronautics and Space Administration (US), Academy of Finland, Ministerio de Ciencia, Innovación y Universidades (España), Swedish National Space Agency, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), ANR-17-CE31-0006,COROSHOCK,EVALUER LE ROLE DU CHOC COMME ACCELERATEUR DE PARTICULES SOLAIRES(2017), Space Physics Research Group, Doctoral Programme in Particle Physics and Universe Sciences, Department of Physics, University of Helsinki, and Particle Physics and Astrophysics

Subjects
Astronomy, particle emission [Sun], PROPAGATION, Astrophysics, PROTON, 7. Clean energy, Astronomi, astrofysik och kosmologi, Coronal mass ejection, Astronomy, Astrophysics and Cosmology, Astrophysics::Solar and Stellar Astrophysics, Physics, heliosphere [Sun], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], PLASMA, Astrophysics::Instrumentation and Methods for Astrophysics, F530, Fusion, Plasma and Space Physics, Solar cycle, Particle acceleration, Solar wind, Physical Sciences, Physics::Space Physics, ELECTRON, Astrophysics::Earth and Planetary Astrophysics, interplanetary medium, Sun: flares, MULTI-SPACECRAFT OBSERVATIONS, Sun: coronal mass ejections (CMEs), Interplanetary medium, Astronomy & Astrophysics, Computer Science::Digital Libraries, Fusion, plasma och rymdfysik, Sun: particle emission, Pitch angle, Sun: heliosphere, RELEASE, Science & Technology, RADIO, Astronomy and Astrophysics, WIND, 115 Astronomy, Space science, Physics::History of Physics, coronal mass ejections (CMEs) [Sun], TRANSPORT, flares [Sun], [SDU]Sciences of the Universe [physics], Space and Planetary Science, STEREO, Event (particle physics), Heliosphere
Abstract

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).

Published
2021
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39. A new method to determine solar energetic particle anisotropies and their associated uncertainties demonstrated for STEREO/SEPT

Author

M. Brüdern, L. Berger, B. Heber, V. Heidrich-Meisner, A. Klassen, A. Kollhoff, P. Kühl, R. D. Strauss, R. Wimmer-Schweingruber, and N. Dresing

Subjects
Space and Planetary Science, Astronomy and Astrophysics
Abstract

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.

Published
2022
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40. First year of energetic particle measurements in the inner heliosphere with Solar Orbiter's Energetic Particle Detector

Author

R. F. Wimmer-Schweingruber, N. P. Janitzek, D. Pacheco, I. Cernuda, F. Espinosa Lara, R. Gómez-Herrero, G. M. Mason, R. C. Allen, Z. G. Xu, F. Carcaboso, A. Kollhoff, P. Kühl, J. L. Freiherr von Forstner, L. Berger, J. Rodriguez-Pacheco, G. C. Ho, G. B. Andrews, V. Angelini, A. Aran, S. Boden, S. I. Böttcher, A. Carrasco, N. Dresing, S. Eldrum, R. Elftmann, V. Evans, O. Gevin, J. Hayes, B. Heber, T. S. Horbury, S. R. Kulkarni, D. Lario, W. J. Lees, O. Limousin, O. E. Malandraki, C. Martín, H. O’Brien, M. Prieto Mateo, A. Ravanbakhsh, O. Rodriguez-Polo, S. Sánchez Prieto, C. E. Schlemm, H. Seifert, J. C. Terasa, K. Tyagi, R. Vainio, A. Walsh, M. K. Yedla, Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), German Research Foundation, National Aeronautics and Space Administration (US), and European Commission

Subjects
010504 meteorology & atmospheric sciences, corona [Sun], FOS: Physical sciences, particle emission [Sun], 7. Clean energy, 01 natural sciences, instruments [Space vehicles], Physics - Space Physics, Sun: activity, Sun: particle emission, 0103 physical sciences, Space vehicles: instruments, activity [Sun], Sun: heliosphere, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, heliosphere [Sun], Sun: corona, Astronomy and Astrophysics, Space Physics (physics.space-ph), Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Interplanetary medium
Abstract

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).

Published
2021

41. First near-relativistic solar electron events observed by EPD onboard Solar Orbiter

Author

R. Gómez-Herrero, D. Pacheco, A. Kollhoff, F. Espinosa Lara, J. L. Freiherr von Forstner, N. Dresing, D. Lario, L. Balmaceda, V. Krupar, O. E. Malandraki, A. Aran, R. Bučík, A. Klassen, K.-L. Klein, I. Cernuda, S. Eldrum, H. Reid, J. G. Mitchell, G. M. Mason, G. C. Ho, J. Rodríguez-Pacheco, R. F. Wimmer-Schweingruber, B. Heber, L. Berger, R. C. Allen, N. P. Janitzek, M. Laurenza, R. De Marco, N. Wijsen, Y. Y. Kartavykh, W. Dröge, T. S. Horbury, M. Maksimovic, C. J. Owen, A. Vecchio, X. Bonnin, O. Kruparova, D. Píša, J. Souček, P. Louarn, A. Fedorov, H. O’Brien, V. Evans, V. Angelini, P. Zucca, M. Prieto, S. Sánchez-Prieto, A. Carrasco, J. J. Blanco, P. Parra, O. Rodríguez-Polo, C. Martín, J. C. Terasa, S. Boden, S. R. Kulkarni, A. Ravanbakhsh, M. Yedla, Z. Xu, G. B. Andrews, C. E. Schlemm, H. Seifert, K. Tyagi, W. J. Lees, J. Hayes, Ministerio de Ciencia, Innovación y Universidades (España), German Research Foundation, Centre National D'Etudes Spatiales (France), Czech Science Foundation, National Aeronautics and Space Administration (US), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Acceleration of particles, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, particle emission [Sun], Astrophysics, Electron, Physics::History of Physics, law.invention, Orbiter, [SDU]Sciences of the Universe [physics], Space and Planetary Science, law, Sun: activity, Sun: particle emission, Physics::Space Physics, activity [Sun], Astrophysics::Earth and Planetary Astrophysics
Abstract

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).

Published
2021
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42. Alpaca Cheese: A New Alternative

Author

Larico M, Heinz, Fernández R, Eliseo, Olarte D, Ceferino, Rodrigo V, Yésica, Machaca T, Pedro, Sumari M, Regina, Chui B, Heber, and Roque H, Bernardo

Subjects
cheese, leche, leche de alpaca, milk, alpaca cheese, cheese yield, rendimiento quesero, queso, alpaca milk, queso de alpaca
Abstract

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.

Published
2018

43. Requerimientos de energía metabolizable para mantenimiento y ganancia de peso de llamas y alpacas determinados mediante la técnica de sacrificio comparativo.

Author

H., Bernardo Roque, P., José Bautista, B., Pablo Beltrán, C., Bilo Calsín, S., Juan Medina, A., Juan Aro, A., Marcelino Araníbar, M., Regina Sumari, L., Diannett Benito, C., Uriel Marca, M., Juan Huareccallo, H., José Pari, A., José Ramírez, A., Evilio Condori, H., Edgar Roque, B., Heber Chui, and Pinares Patiño, César S.

Published
2020
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44. In-field calibration of the Navigation Dosimetry System (NAVIDOS) during solar minimum conditions

Author

F. Langner, T. Möller, B. Heber, Sönke Burmeister, O. Burda, and F. Wissmann

Subjects
Solar minimum, Physics, Physics and Astronomy (miscellaneous), Atmospheric pressure, Equivalent dose, business.industry, Detector, Astronomy and Astrophysics, Radiation, Optics, Assisted GPS, Calibration, Dosimetry, business
Abstract

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.

Published
2013
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46. Open Issues in Heliospheric Physics

Author

Robert F. Wimmer-Schweingruber, B. Heber, and H. Fitchner

Subjects
Interstellar medium, Physics, Planetary science, Energetic neutral atom, Space and Planetary Science, Earth and Planetary Sciences (miscellaneous), Astronomy, Astronomy and Astrophysics, Interstellar probe, Heliosphere, Astrobiology
Abstract

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.

Published
2009
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47. COSTEP/SOHO observations of energetic electrons far upstream of the Earth's bow-shock

Author

A. Klassen, R. Gómez-Herrero, E. Böhm, R. Müller-Mellin, B. Heber, and R. Wimmer-Schweingruber

Subjects
lcsh:Geophysics. Cosmic physics, lcsh:QC801-809, lcsh:Q, lcsh:Science, lcsh:Physics, lcsh:QC1-999
Abstract

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.

Published
2008

48. Heliopause Explorer—a sailcraft mission to the outer boundaries of the solar system

Author

T. Niederstadt, F. Burger, B. Heber, Christoph Sickinger, P. Groepper, Lars Herbeck, Michael Eiden, Bernd Dachwald, Manfred Leipold, Wolfgang Seboldt, H. Fichtner, and S. Lascar

Subjects
Astronautics, Solar System, Solar conjunction, Engineering, business.industry, Aerospace Engineering, Solar sail, Space exploration, Radiation pressure, Physics::Space Physics, Heliopause, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Aerospace engineering, Solar Sail, Interplanetary spaceflight, business, Heliosphere
Abstract

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.

Published
2006
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49. Modulation of Jovian and galactic electrons in the heliosphere: 2. Radial transport of a few MeV electrons

Author

S. E. S. Ferreira, M. S. Potgieter, R. A. Burger, B. Heber, H. Fichtner, and C. Lopate

Subjects
Atmospheric Science, Geophysics, Ecology, Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Paleontology, Soil Science, Forestry, Aquatic Science, Oceanography, Earth-Surface Processes, Water Science and Technology
Published
2001
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50. Energetic particle signatures of a corotating interaction region from a high latitude coronal hole: SOHO, wind and Ulysses observations

Author

Adam Szabo, Barbara J. Thompson, Richard G. Marsden, A. J. Lazarus, Volker Bothmer, T. R. Sanderson, J. T. Gosling, Reinhold Müller-Mellin, Arik Posner, H. Kunow, B. Heber, Zoran Mikic, and Jon A. Linker

Subjects
Physics, Atmospheric Science, Astrophysics::High Energy Astrophysical Phenomena, Ecliptic, Aerospace Engineering, Coronal hole, Astronomy, Astronomy and Astrophysics, Cosmic ray, Coronal loop, Corona, Solar wind, Geophysics, Space and Planetary Science, Physics::Space Physics, Coronal mass ejection, Extreme ultraviolet Imaging Telescope, Astrophysics::Solar and Stellar Astrophysics, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

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.

Published
2000
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