16 results on '"Effenberger, F."'
Search Results
2. Electron Power-Law Spectra in Solar and Space Plasmas
- Author
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Oka, M., Birn, J., Battaglia, M., Chaston, C. C., Hatch, S. M., Livadiotis, G., Imada, S., Miyoshi, Y., Kuhar, M., Effenberger, F., Eriksson, E., Khotyaintsev, Y. V., and Retinò, A.
- Published
- 2018
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3. Extreme Solar Events: Setting up a Paradigm.
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Usoskin, Ilya, Miyake, Fusa, Baroni, Melanie, Brehm, Nicolas, Dalla, Silvia, Hayakawa, Hisashi, Hudson, Hugh, Jull, A. J. Timothy, Knipp, Delores, Koldobskiy, Sergey, Maehara, Hiroyuki, Mekhaldi, Florian, Notsu, Yuta, Poluianov, Stepan, Rozanov, Eugene, Shapiro, Alexander, Spiegl, Tobias, Sukhodolov, Timofei, Uusitalo, Joonas, and Wacker, Lukas
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SOLAR energetic particles ,SUN ,CORONAL mass ejections ,SOLAR activity ,COSMOGENIC nuclides ,OPEN-ended questions - Abstract
The Sun is magnetically active and often produces eruptive events on different energetic and temporal scales. Until recently, the upper limit of such events was unknown and believed to be roughly represented by direct instrumental observations. However, two types of extreme events were discovered recently: extreme solar energetic particle events on the multi-millennial time scale and super-flares on sun-like stars. Both discoveries imply that the Sun might rarely produce events, called extreme solar events (ESE), whose energy could be orders of magnitude greater than anything we have observed during recent decades. During the years following these discoveries, great progress has been achieved in collecting observational evidence, uncovering new events, making statistical analyses, and developing theoretical modelling. The ESE paradigm lives and is being developed. On the other hand, many outstanding questions still remain open and new ones emerge. Here we present an overview of the current state of the art and the forming paradigm of ESE from different points of view: solar physics, stellar–solar projections, cosmogenic-isotope data, modelling, historical data, as well as terrestrial, technological and societal effects of ESEs. Special focus is paid to open questions and further developments. This review is based on the joint work of the International Space Science Institute (ISSI) team #510 (2020–2022). [ABSTRACT FROM AUTHOR]
- Published
- 2023
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4. Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN's Low Altitude Perspective.
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Angelopoulos, V., Zhang, X.-J., Artemyev, A. V., Mourenas, D., Tsai, E., Wilkins, C., Runov, A., Liu, J., Turner, D. L., Li, W., Khurana, K., Wirz, R. E., Sergeev, V. A., Meng, X., Wu, J., Hartinger, M. D., Raita, T., Shen, Y., An, X., and Shi, X.
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ION acoustic waves ,ELECTRONS ,OCEAN wave power ,DELOCALIZATION energy ,RELATIVISTIC electrons ,CYCLOTRONS ,ELECTRON scattering - Abstract
We review comprehensive observations of electromagnetic ion cyclotron (EMIC) wave-driven energetic electron precipitation using data collected by the energetic electron detector on the Electron Losses and Fields InvestigatioN (ELFIN) mission, two polar-orbiting low-altitude spinning CubeSats, measuring 50-5000 keV electrons with good pitch-angle and energy resolution. EMIC wave-driven precipitation exhibits a distinct signature in energy-spectrograms of the precipitating-to-trapped flux ratio: peaks at >0.5 MeV which are abrupt (bursty) (lasting ∼17 s, or Δ L ∼ 0.56 ) with significant substructure (occasionally down to sub-second timescale). We attribute the bursty nature of the precipitation to the spatial extent and structuredness of the wave field at the equator. Multiple ELFIN passes over the same MLT sector allow us to study the spatial and temporal evolution of the EMIC wave - electron interaction region. Case studies employing conjugate ground-based or equatorial observations of the EMIC waves reveal that the energy of moderate and strong precipitation at ELFIN approximately agrees with theoretical expectations for cyclotron resonant interactions in a cold plasma. Using multiple years of ELFIN data uniformly distributed in local time, we assemble a statistical database of ∼50 events of strong EMIC wave-driven precipitation. Most reside at L ∼ 5 − 7 at dusk, while a smaller subset exists at L ∼ 8 − 12 at post-midnight. The energies of the peak-precipitation ratio and of the half-peak precipitation ratio (our proxy for the minimum resonance energy) exhibit an L -shell dependence in good agreement with theoretical estimates based on prior statistical observations of EMIC wave power spectra. The precipitation ratio's spectral shape for the most intense events has an exponential falloff away from the peak (i.e., on either side of ∼ 1.45 MeV). It too agrees well with quasi-linear diffusion theory based on prior statistics of wave spectra. It should be noted though that this diffusive treatment likely includes effects from nonlinear resonant interactions (especially at high energies) and nonresonant effects from sharp wave packet edges (at low energies). Sub-MeV electron precipitation observed concurrently with strong EMIC wave-driven >1 MeV precipitation has a spectral shape that is consistent with efficient pitch-angle scattering down to ∼ 200-300 keV by much less intense higher frequency EMIC waves at dusk (where such waves are most frequent). At ∼100 keV, whistler-mode chorus may be implicated in concurrent precipitation. These results confirm the critical role of EMIC waves in driving relativistic electron losses. Nonlinear effects may abound and require further investigation. [ABSTRACT FROM AUTHOR]
- Published
- 2023
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5. Dust in and Around the Heliosphere and Astrospheres.
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Sterken, Veerle J., Baalmann, Lennart R., Draine, Bruce T., Godenko, Egor, Herbst, Konstantin, Hsu, Hsiang-Wen, Hunziker, Silvan, Izmodenov, Vladislav, Lallement, Rosine, and Slavin, Jonathan D.
- Abstract
Interstellar dust particles were discovered in situ, in the solar system, with the Ulysses mission’s dust detector in 1992. Ever since, more interstellar dust particles have been measured inside the solar system by various missions, providing insight into not only the composition of such far-away visitors, but also in their dynamics and interaction with the heliosphere. The dynamics of interstellar (and interplanetary) dust in the solar/stellar systems depend on the dust properties and also on the space environment, in particular on the heliospheric/astrospheric plasma, and the embedded time-variable magnetic fields, via Lorentz forces. Also, solar radiation pressure filters out dust particles depending on their composition. Charge exchanges between the dust and the ambient plasma occur, and pick-up ions can be created. The role of the dust for the physics of the heliosphere and astrospheres is fairly unexplored, but an important and a rapidly growing topic of investigation. This review paper gives an overview of dust processes in heliospheric and astrospheric environments, with its resulting dynamics and consequences. It discusses theoretical modeling, and reviews in situ measurements and remote sensing of dust in and near our heliosphere and astrospheres, with the latter being a newly emerging field of science. Finally, it summarizes the open questions in the field. [ABSTRACT FROM AUTHOR]
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- 2022
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6. Turbulence in the Outer Heliosphere.
- Author
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Fraternale, Federico, Adhikari, Laxman, Fichtner, Horst, Kim, Tae K., Kleimann, Jens, Oughton, Sean, Pogorelov, Nikolai V., Roytershteyn, Vadim, Smith, Charles W., Usmanov, Arcadi V., Zank, Gary P., and Zhao, Lingling
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HELIOSPHERE ,TURBULENCE ,CHARGE exchange ,SOLAR wind ,INTERSTELLAR medium - Abstract
The solar wind (SW) and local interstellar medium (LISM) are turbulent media. Their interaction is governed by complex physical processes and creates heliospheric regions with significantly different properties in terms of particle populations, bulk flow and turbulence. Our knowledge of the solar wind turbulence nature and dynamics mostly relies on near-Earth and near-Sun observations, and has been increasingly improving in recent years due to the availability of a wealth of space missions, including multi-spacecraft missions. In contrast, the properties of turbulence in the outer heliosphere are still not completely understood. In situ observations by Voyager and New Horizons, and remote neutral atom measurements by IBEX strongly suggest that turbulence is one of the critical processes acting at the heliospheric interface. It is intimately connected to charge exchange processes responsible for the production of suprathermal ions and energetic neutral atoms. This paper reviews the observational evidence of turbulence in the distant SW and in the LISM, advances in modeling efforts, and open challenges. [ABSTRACT FROM AUTHOR]
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- 2022
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7. The Structure of the Large-Scale Heliosphere as Seen by Current Models.
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Kleimann, Jens, Dialynas, Konstantinos, Fraternale, Federico, Galli, André, Heerikhuisen, Jacob, Izmodenov, Vladislav, Kornbleuth, Marc, Opher, Merav, and Pogorelov, Nikolai
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HELIOSPHERE ,MAGNETIC structure ,NUMBER concept ,MAGNETIC fields ,COMPUTER simulation - Abstract
This review summarizes the current state of research aiming at a description of the global heliosphere using both analytical and numerical modeling efforts, particularly in view of the overall plasma/neutral flow and magnetic field structure, and its relation to energetic neutral atoms. Being part of a larger volume on current heliospheric research, it also lays out a number of key concepts and describes several classic, though still relevant early works on the topic. Regarding numerical simulations, emphasis is put on magnetohydrodynamic (MHD), multi-fluid, kinetic-MHD, and hybrid modeling frameworks. Finally, open issues relating to the physical relevance of so-called "croissant" models of the heliosphere, as well as the general (dis)agreement of model predictions with observations are highlighted and critically discussed. [ABSTRACT FROM AUTHOR]
- Published
- 2022
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8. The Heliosphere and Local Interstellar Medium from Neutral Atom Observations at Energies Below 10 keV.
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Galli, André, Baliukin, Igor I., Bzowski, Maciej, Izmodenov, Vladislav V., Kornbleuth, Marc, Kucharek, Harald, Möbius, Eberhard, Opher, Merav, Reisenfeld, Dan, Schwadron, Nathan A., and Swaczyna, Paweł
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INTERSTELLAR medium ,HELIOSPHERE ,LOCAL mass media ,HYDROGEN atom ,SOLAR wind ,ATOMS - Abstract
As the heliosphere moves through the surrounding interstellar medium, a fraction of the interstellar neutral helium, hydrogen, and heavier species crossing the heliopause make it to the inner heliosphere as neutral atoms with energies ranging from few eV to several hundred eV. In addition, energetic neutral hydrogen atoms originating from solar wind protons and from pick-up ions are created through charge-exchange with interstellar atoms. This review summarizes all observations of heliospheric energetic neutral atoms and interstellar neutrals at energies below 10 keV. Most of these data were acquired with the Interstellar Boundary Explorer launched in 2008. Among many other IBEX breakthroughs, it provided the first ever all-sky maps of energetic neutral atoms from the heliosphere and enabled the science community to measure in-situ interstellar neutral hydrogen, oxygen, and neon for the first time. These observations have revolutionized and keep challenging our understanding of the heliosphere shaped by the combined forces of the local interstellar flow, the local interstellar magnetic field, and the time-dependent solar wind. [ABSTRACT FROM AUTHOR]
- Published
- 2022
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9. Astrospheres of Planet-Hosting Cool Stars and Beyond ⋅ When Modeling Meets Observations.
- Author
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Herbst, Konstantin, Baalmann, Lennart R., Bykov, Andrei, Engelbrecht, N. Eugene, Ferreira, Stefan E. S., Izmodenov, Vladislav V., Korolkov, Sergey D., Levenfish, Ksenia P., Linsky, Jeffrey L., Meyer, Dominique M.-A., Scherer, Klaus, and Strauss, R. Du Toit
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GALACTIC cosmic rays ,EARLY stars ,INTERSTELLAR medium ,SOLAR wind ,EXTRASOLAR planets ,STELLAR winds ,NEUTRON stars - Abstract
Thanks to dedicated long-term missions like Voyager and GOES over the past 50 years, much insight has been gained on the activity of our Sun, the solar wind, its interaction with the interstellar medium, and, thus, about the formation, the evolution, and the structure of the heliosphere. Additionally, with the help of multi-wavelength observations by the Hubble Space Telescope, Kepler, and TESS, we not only were able to detect a variety of extrasolar planets and exomoons but also to study the characteristics of their host stars, and thus became aware that other stars drive bow shocks and astrospheres. Although features like, e.g., stellar winds, could not be measured directly, over the past years several techniques have been developed allowing us to indirectly derive properties like stellar mass-loss rates and stellar wind speeds, information that can be used as direct input to existing astrospheric modeling codes. In this review, the astrospheric modeling efforts of various stars will be presented. Starting with the heliosphere as a benchmark of astrospheric studies, investigating the paleo-heliospheric changes and the Balmer H α projections to 1 pc , we investigate the surroundings of cool and hot stars, but also of more exotic objects like neutron stars. While pulsar wind nebulae (PWNs) might be a source of high-energy galactic cosmic rays (GCRs), the astrospheric environments of cool and hot stars form a natural shield against GCRs. Their modulation within these astrospheres, and the possible impact of turbulence, are also addressed. This review shows that all of the presented modeling efforts are in excellent agreement with currently available observations. [ABSTRACT FROM AUTHOR]
- Published
- 2022
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10. Recent Developments in Particle Acceleration at Shocks: Theory and Observations.
- Author
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Perri, Silvia, Bykov, Andrei, Fahr, Hans, Fichtner, Horst, and Giacalone, Joe
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PARTICLE acceleration ,INTERPLANETARY medium ,SOLAR wind ,SOLAR corona ,HELIOSPHERE ,COMPUTER simulation ,COSMIC rays - Abstract
Energetic particles represent an important component of the plasma in the heliosphere. They range from particles accelerated at impulsive events in the solar corona and at large scale structures in the interplanetary medium, to anomalous cosmic rays accelerated at the boundaries of the heliosphere. In-situ satellite observations, numerical simulations and theoretical models have advanced, often in a cooperative way, our knowledge on the acceleration processes involved. In this paper we review recent developments on particle acceleration, with major emphasis on shock acceleration, giving an overview of recent observations at interplanetary shocks and at the termination shock of the solar wind. We discuss their interpretation in terms of analytical models and numerical simulations. The influence of the particle transport properties on the acceleration mechanism will also be addressed. [ABSTRACT FROM AUTHOR]
- Published
- 2022
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11. Understanding the Origins of Problem Geomagnetic Storms Associated with "Stealth" Coronal Mass Ejections.
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Nitta, Nariaki V., Mulligan, Tamitha, Kilpua, Emilia K. J., Lynch, Benjamin J., Mierla, Marilena, O'Kane, Jennifer, Pagano, Paolo, Palmerio, Erika, Pomoell, Jens, Richardson, Ian G., Rodriguez, Luciano, Rouillard, Alexis P., Sinha, Suvadip, Srivastava, Nandita, Talpeanu, Dana-Camelia, Yardley, Stephanie L., and Zhukov, Andrei N.
- Subjects
CORONAL mass ejections ,MAGNETIC storms ,SPACE environment ,SOLAR activity ,SOLAR cycle ,SOLAR corona ,GEOMAGNETISM ,HELIOSEISMOLOGY - Abstract
Geomagnetic storms are an important aspect of space weather and can result in significant impacts on space- and ground-based assets. The majority of strong storms are associated with the passage of interplanetary coronal mass ejections (ICMEs) in the near-Earth environment. In many cases, these ICMEs can be traced back unambiguously to a specific coronal mass ejection (CME) and solar activity on the frontside of the Sun. Hence, predicting the arrival of ICMEs at Earth from routine observations of CMEs and solar activity currently makes a major contribution to the forecasting of geomagnetic storms. However, it is clear that some ICMEs, which may also cause enhanced geomagnetic activity, cannot be traced back to an observed CME, or, if the CME is identified, its origin may be elusive or ambiguous in coronal images. Such CMEs have been termed "stealth CMEs". In this review, we focus on these "problem" geomagnetic storms in the sense that the solar/CME precursors are enigmatic and stealthy. We start by reviewing evidence for stealth CMEs discussed in past studies. We then identify several moderate to strong geomagnetic storms (minimum Dst < − 50 nT) in solar cycle 24 for which the related solar sources and/or CMEs are unclear and apparently stealthy. We discuss the solar and in situ circumstances of these events and identify several scenarios that may account for their elusive solar signatures. These range from observational limitations (e.g., a coronagraph near Earth may not detect an incoming CME if it is diffuse and not wide enough) to the possibility that there is a class of mass ejections from the Sun that have only weak or hard-to-observe coronal signatures. In particular, some of these sources are only clearly revealed by considering the evolution of coronal structures over longer time intervals than is usually considered. We also review a variety of numerical modelling approaches that attempt to advance our understanding of the origins and consequences of stealthy solar eruptions with geoeffective potential. Specifically, we discuss magnetofrictional modelling of the energisation of stealth CME source regions and magnetohydrodynamic modelling of the physical processes that generate stealth CME or CME-like eruptions, typically from higher altitudes in the solar corona than CMEs from active regions or extended filament channels. [ABSTRACT FROM AUTHOR]
- Published
- 2021
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12. The Magnetic Electron Ion Spectrometer: A Review of On-Orbit Sensor Performance, Data, Operations, and Science.
- Author
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Claudepierre, S. G., Blake, J. B., Boyd, A. J., Clemmons, J. H., Fennell, J. F., Gabrielse, C., Looper, M. D., Mazur, J. E., O'Brien, T. P., Reeves, G. D., Roeder, J. L., Spence, H. E., and Turner, D. L.
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MAGNETIC ions ,RELATIVISTIC electrons ,RADIATION belts ,SPACE environment ,SPECTROMETERS ,ASTROPHYSICAL radiation - Abstract
Measurements from NASA's Van Allen Probes have transformed our understanding of the dynamics of Earth's geomagnetically-trapped, charged particle radiation. The Van Allen Probes were equipped with the Magnetic Electron Ion Spectrometers (MagEIS) that measured energetic and relativistic electrons, along with energetic ions, in the radiation belts. Accurate and routine measurement of these particles was of fundamental importance towards achieving the scientific goals of the mission. We provide a comprehensive review of the MagEIS suite's on-orbit performance, operation, and data products, along with a summary of scientific results. The purpose of this review is to serve as a complement to the MagEIS instrument paper, which was largely completed before flight and thus focused on pre-flight design and performance characteristics. As is the case with all space-borne instrumentation, the anticipated sensor performance was found to be different once on orbit. Our intention is to provide sufficient detail on the MagEIS instruments so that future generations of researchers can understand the subtleties of the sensors, profit from these unique measurements, and continue to unlock the mysteries of the near-Earth space radiation environment. [ABSTRACT FROM AUTHOR]
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- 2021
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13. A Primer on Focused Solar Energetic Particle Transport.
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van den Berg, Jabus, Strauss, Du Toit, and Effenberger, Frederic
- Abstract
The basics of focused transport as applied to solar energetic particles are reviewed, paying special attention to areas of common misconception. The micro-physics of charged particles interacting with slab turbulence are investigated to illustrate the concept of pitch-angle scattering, where after the distribution function and focused transport equation are introduced as theoretical tools to describe the transport processes and it is discussed how observable quantities can be calculated from the distribution function. In particular, two approximations, the diffusion-advection and the telegraph equation, are compared in simplified situations to the full solution of the focused transport equation describing particle motion along a magnetic field line. It is shown that these approximations are insufficient to capture the complexity of the physical processes involved. To overcome such limitations, a finite-difference model, which is open for use by the public, is introduced to solve the focused transport equation. The use of the model is briefly discussed and it is shown how the model can be applied to reproduce an observed solar energetic electron event, providing insights into the acceleration and transport processes involved. Past work and literature on the application of these concepts are also reviewed, starting with the most basic models and building up to more complex models. [ABSTRACT FROM AUTHOR]
- Published
- 2020
- Full Text
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14. Perpendicular Transport of Energetic Particles in Magnetic Turbulence.
- Author
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Shalchi, Andreas
- Subjects
MAGNETIC particles ,SOLAR energetic particles ,COSMIC rays ,RANDOM fields ,INTERPLANETARY medium ,TURBULENCE ,SOLAR atmosphere ,COSMIC ray showers - Abstract
Scientists have explored how energetic particles such as solar energetic particles and cosmic rays move through a magnetized plasma such as the interplanetary and interstellar medium since more than five decades. From a theoretical point of view, this topic is difficult because the particles experience complicated interactions with turbulent magnetic fields. Besides turbulent fields, there are also large scale or mean magnetic fields breaking the symmetry in such systems and one has to distinguish between transport of particles parallel and perpendicular with respect to such mean fields. In standard descriptions of transport phenomena, one often assumes that the transport in both directions is normal diffusive but non-diffusive transport was found in more recent work. This is in particular true for early and intermediate times where the diffusive regime is not yet reached. In recent years researchers employed advanced numerical tools in order to simulate the motion of those particles through the aforementioned systems. Nevertheless, the analytical description of the problem discussed here is of utmost importance since analytical forms of particle transport parameters need to be known in several applications such as solar modulation studies or investigations of shock acceleration. The latter process is directly linked to the question of what the sources of high energy cosmic rays are, a problem which is considered to be one of the most important problems of the sciences of the 21st century. The present review article discusses analytical theories developed for describing particle transport across a large scale magnetic field as well as field line random walk. A heuristic approach explaining the basic physics of perpendicular transport is also presented. Simple analytical forms for the perpendicular diffusion coefficient are proposed which can easily be incorporated in numerical codes for solar modulation or shock acceleration studies. Test-particle simulations are also discussed together with a comparison with analytical results. Several applications such as cosmic ray propagation and diffusive shock acceleration are also part of this review. [ABSTRACT FROM AUTHOR]
- Published
- 2020
- Full Text
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15. A Hitch-hiker's Guide to Stochastic Differential Equations.
- Author
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Strauss, R. and Effenberger, Frederic
- Subjects
STOCHASTIC differential equations ,ASTROPHYSICS ,ACCELERATION (Mechanics) ,TRANSPORT equation ,COSMIC rays - Abstract
In this review, an overview of the recent history of stochastic differential equations (SDEs) in application to particle transport problems in space physics and astrophysics is given. The aim is to present a helpful working guide to the literature and at the same time introduce key principles of the SDE approach via 'toy models'. Using these examples, we hope to provide an easy way for newcomers to the field to use such methods in their own research. Aspects covered are the solar modulation of cosmic rays, diffusive shock acceleration, galactic cosmic ray propagation and solar energetic particle transport. We believe that the SDE method, due to its simplicity and computational efficiency on modern computer architectures, will be of significant relevance in energetic particle studies in the years to come. [ABSTRACT FROM AUTHOR]
- Published
- 2017
- Full Text
- View/download PDF
16. Interstellar Mapping and Acceleration Probe (IMAP): A New NASA Mission.
- Author
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McComas, D. J., Christian, E. R., Schwadron, N. A., Fox, N., Westlake, J., Allegrini, F., Baker, D. N., Biesecker, D., Bzowski, M., Clark, G., Cohen, C. M. S., Cohen, I., Dayeh, M. A., Decker, R., de Nolfo, G. A., Desai, M. I., Ebert, R. W., Elliott, H. A., Fahr, H., and Frisch, P. C.
- Subjects
INTERSTELLAR medium ,INTERPLANETARY medium ,SPACE vehicle orbits ,SOLAR energetic particles - Abstract
The Interstellar Mapping and Acceleration Probe (IMAP) is a revolutionary mission that simultaneously investigates two of the most important overarching issues in Heliophysics today: the acceleration of energetic particles and interaction of the solar wind with the local interstellar medium. While seemingly disparate, these are intimately coupled because particles accelerated in the inner heliosphere play critical roles in the outer heliospheric interaction. Selected by NASA in 2018, IMAP is planned to launch in 2024. The IMAP spacecraft is a simple sun-pointed spinner in orbit about the Sun-Earth L1 point. IMAP's ten instruments provide a complete and synergistic set of observations to simultaneously dissect the particle injection and acceleration processes at 1 AU while remotely probing the global heliospheric interaction and its response to particle populations generated by these processes. In situ at 1 AU, IMAP provides detailed observations of solar wind electrons and ions; suprathermal, pickup, and energetic ions; and the interplanetary magnetic field. For the outer heliosphere interaction, IMAP provides advanced global observations of the remote plasma and energetic ions over a broad energy range via energetic neutral atom imaging, and precise observations of interstellar neutral atoms penetrating the heliosphere. Complementary observations of interstellar dust and the ultraviolet glow of interstellar neutrals further deepen the physical understanding from IMAP. IMAP also continuously broadcasts vital real-time space weather observations. Finally, IMAP engages the broader Heliophysics community through a variety of innovative opportunities. This paper summarizes the IMAP mission at the start of Phase A development. [ABSTRACT FROM AUTHOR]
- Published
- 2018
- Full Text
- View/download PDF
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