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Готові списки джерел за темами / Inner-Heliosphere

Добірка наукової літератури з теми "Inner-Heliosphere"

Автор: Grafiati

Опубліковано: 10 червня 2023

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Статті в журналах з теми "Inner-Heliosphere":

1

Hewish, A. "Physics of the inner Heliosphere." Journal of Atmospheric and Terrestrial Physics 54, no. 7-8 (July 1992): 1085. http://dx.doi.org/10.1016/0021-9169(92)90076-w.

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2

Luhmann, Janet G. "The Inner Heliosphere at Fifty." Eos, Transactions American Geophysical Union 94, no. 38 (September 17, 2013): 329–30. http://dx.doi.org/10.1002/2013eo380001.

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3

Vogt, A., B. Heber, A. Kopp, M. S. Potgieter, and R. D. Strauss. "Jovian electrons in the inner heliosphere." Astronomy & Astrophysics 613 (May 2018): A28. http://dx.doi.org/10.1051/0004-6361/201731736.

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Context. Since the Pioneer 10 flyby of Jupiter it has become well known that electrons of Jovian origin dominate the lower MeV range of charged energetic particles in the inner heliosphere. Aims. Because the Jovian source can be treated as point-like in numerical models, many attempts to investigate charged particle transport in the inner heliosphere have utilized Jovian electrons as test particles. The reliability of the derived parameters for convective and diffusive transport processes are therefore highly dependent on an accurate estimation of the Jovian source spectrum. In this study we aim to provide such an estimation. Methods. In this study we have proposed a new electron source spectrum, specified at the boundary of the Jovian magnetosphere, fitted to flyby measurements by Pioneer 10 and Ulysses, with a spectral shape also in agreement with measurements at Earth’s orbit by Ulysses, Voyager 1, ISEE and SOHO. Results. The proposed spectrum is consistent with all previous theoretical suggestions, but deviates considerably in the lower MeV range which was inaccessible to those studies.

4

Kallenrode, May Britt. "Particle propagation in the inner heliosphere." Journal of Geophysical Research: Space Physics 98, A11 (November 1, 1993): 19037–47. http://dx.doi.org/10.1029/93ja02079.

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5

Nkosi, G. S., M. S. Potgieter, and S. E. S. Ferreira. "Electron anisotropies in the inner heliosphere." Planetary and Space Science 56, no. 3-4 (March 2008): 501–9. http://dx.doi.org/10.1016/j.pss.2007.10.003.

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6

Tenerani, Anna, Nikos Sioulas, Lorenzo Matteini, Olga Panasenco, Chen Shi, and Marco Velli. "Evolution of Switchbacks in the Inner Heliosphere." Astrophysical Journal Letters 919, no. 2 (October 1, 2021): L31. http://dx.doi.org/10.3847/2041-8213/ac2606.

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7

Tenerani, Anna, Nikos Sioulas, Lorenzo Matteini, Olga Panasenco, Chen Shi, and Marco Velli. "Evolution of Switchbacks in the Inner Heliosphere." Astrophysical Journal Letters 919, no. 2 (October 1, 2021): L31. http://dx.doi.org/10.3847/2041-8213/ac2606.

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8

Stansby, D., and T. S. Horbury. "Number density structures in the inner heliosphere." Astronomy & Astrophysics 613 (May 2018): A62. http://dx.doi.org/10.1051/0004-6361/201732567.

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Aims. The origins and generation mechanisms of the slow solar wind are still unclear. Part of the slow solar wind is populated by number density structures, discrete patches of increased number density that are frozen in to and move with the bulk solar wind. In this paper we aimed to provide the first in-situ statistical study of number density structures in the inner heliosphere. Methods. We reprocessed in-situ ion distribution functions measured by Helios in the inner heliosphere to provide a new reliable set of proton plasma moments for the entire mission. From this new data set we looked for number density structures measured within 0.5 AU of the Sun and studied their properties. Results. We identified 140 discrete areas of enhanced number density. The structures occurred exclusively in the slow solar wind and spanned a wide range of length scales from 50 Mm to 2000 Mm, which includes smaller scales than have been previously observed. They were also consistently denser and hotter that the surrounding plasma, but had lower magnetic field strengths, and therefore remained in pressure balance. Conclusions. Our observations show that these structures are present in the slow solar wind at a wide range of scales, some of which are too small to be detected by remote sensing instruments. These structures are rare, accounting for only 1% of the slow solar wind measured by Helios, and are not a significant contribution to the mass flux of the solar wind.

9

Chashei, I. V. "Turbulence dissipation scale in the inner heliosphere." Advances in Space Research 20, no. 12 (January 1997): 2299–302. http://dx.doi.org/10.1016/s0273-1177(97)00903-4.

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10

Davila, Joseph M. "Observing the inner heliosphere from new perspectives." Advances in Space Research 21, no. 1-2 (January 1998): 319–23. http://dx.doi.org/10.1016/s0273-1177(97)00988-5.

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Дисертації з теми "Inner-Heliosphere":

1

Reid, Hamish Andrew Sinclair. "Solar electron beam transport in the inner heliosphere." Thesis, University of Glasgow, 2011. http://theses.gla.ac.uk/2370/.

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Impulsive solar electron beams have an attractive diagnostic potential for poorly understood particle acceleration processes in solar flares. Solar flare accelerated electron beams propagating away from the Sun can interact with the turbulent interplanetary media, producing Langmuir waves and type III radio emission. In this thesis, we simulate electron beam propagation from the Sun to the Earth in the weak turbulent regime taking into account the self-consistent generation of Langmuir waves. We show that an injected single power-law spectrum will be detected at 1 AU as a broken power-law due to wave-particle interaction in the inhomogeneous plasma. We further extend these results by investigating the Langmuir wave interaction with background electron density fluctuations from low frequency MHD turbulence. We find a direct correlation between the spectra of the double power-law below the break energy and the turbulent intensity of the background plasma. Solar flares are believed to accelerate both upward and downward propagating electron beams which can radiate emission at radio and X-ray wavelengths correspondingly. The correlation between X-ray and radio emissions in a well observed solar flare allowed us detailed study of the electron acceleration region properties. We used the Nancay Radioheliograph, Phoenix-2 and RHESSI to infer the type III position, type III starting frequency and spectral index of the HXR emission respectively. Using these datasets and numerical simulations of the electron beam transport in the corona plasma, we were able to infer not only the location (the height in the corona), but to estimate the spatial length of the electron acceleration site.

2

Moise, Elena. "Acceleration of interstellar helium in the inner heliosphere." Diss., The University of Arizona, 2004. http://hdl.handle.net/10150/280630.

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The heliosphere, the volume inflated by the solar wind, is impenetrable to inter-stellar plasma, except for high-energy galactic cosmic rays. Neutral components of the local interstellar medium (LISM), however, do enter at the speed of Sun's relative motion to LISM. On their journey through the heliosphere, interstellar neutrals are subject to ionization by solar wind protons and electrons, solar photons, and also the gravitational pull of the Sun. Once ionized, the newly created ions, called "pickup ions" (PUIs), are swept out by the solar wind toward the termination shock (TS). Helium atoms, having a higher ionization potential, penetrate deeper into the solar system, with their trajectories gravitational focused to form a cone of high concentration of LISM He in the wake of the Sun's motion through LISM. This He cone provides a rich source of He⁺ PUIs. Recent theories suggest that PUIs are the seed particles for the detected anomalous cosmic rays (ACRs)--singly-charged ions highly enriched in He, N, O, and Ne, and with energies < 50 MeV/nuc after solar modulation. To reach such high energies, it would be necessary that the PUIs be pre-accelerated before reaching the TS, where the ions are finally accelerated to become ACRs. This thesis investigates two aspects of the PUIs life cycle by using the data gathered by Solar Wind Composition Spectrometer (SWICS) on the Advance Composition Explorer (ACE). The first is a study of pre-acceleration of He⁺ PUIs up to 100 KeV, by shocks generated by coronal mass ejecta. Our result implies that quasi-parallel shocks are more efficient at accelerating He⁺ PUIs in this energy interval than quasi-perpendicular shocks. The second is a study of time-variability of the gravitationally focused He cone. Our results suggest that the most likely cause of observed variability is due to the changing ionization rate of He over the solar cycle.

3

Conlon, Thomas Michael. "STEREO observations of solar wind transients in the inner heliosphere." Thesis, University of Leicester, 2015. http://hdl.handle.net/2381/32897.

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This thesis investigates the implications of relaxing assumptions inherent in techniques that analyse solar wind transients observed by NASA's Solar TErrestrial RElations Observatory (STEREO). In the first research chapter, I relaxed the assumption that the STEREO spacecraft are stationary while observing a transient. For much of the parameter space investigated, this effect was minimal, however in some cases it resulted in differences in derived radial speeds of hundreds of km s-1, leading to large errors. Using real data examples, the difference this effect makes was shown. The second research chapter applies the previous analysis to Corotating Interactions Region (CIR) observations. CIR events were identifed in STEREO HI J-maps, analysed, and their predicted arrival times calculated at each of the STEREO and Advanced Composition Explorer (ACE) spacecraft. A superposed epoch analysis was conducted using the predicted arrival times as the zero epoch time. It was found that when the fixed STEREO spacecraft assumption was relaxed, the CIR related transients that I observed had their estimated propagation speed increase such that they were propagating at (or close to) the slow solar wind speed, a physically realistic change. Changes in the structure of a stream interface over 1-2 days were seen, calling into question some of the underlying assumptions, which assume constant propagation characteristics over longer time-scales. Finally, I consider acceleration of solar wind transients close to the Sun. I use the analysis from previous chapters to perform fits to transient trajectories close to the Sun and infers the size of the acceleration region required to achieve convincing fits at low elongation values. It was found that the behaviour of the transients is consistent with an acceleration region within which the transient accelerates and then adopts a constant propagation speed. The acceleration region does not appear to occur at a fixed radial distance, but rather is different for each event analysed.

4

Chollet, Eileen Emily. "Solar-Energetic Particles as a Probe of the Inner Heliosphere." Diss., The University of Arizona, 2008. http://hdl.handle.net/10150/195499.

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In this dissertation, I explore the relationship between solar energetic particles (SEPs) and the interplanetary magnetic field, and I use observations of SEPs to probe the region of space between the Sun and the Earth. After an introduction of major concepts in heliospheric physics, describing some of the history of energetic particles and defining the data sets used in the work, the rest of this dissertation is organized around three major concepts related to energetic particle transport: magnetic field-line length, interplanetary turbulence, and particle scattering and diffusion. In Chapter 2, I discuss how energetic particles can be used to measure the lengths of field lines and how particle scattering complicates the interpretation of these measurements. I then propose applying these measurements to a particular open problem: the origin and properties of heliospheric current sheets. In the next chapter, I move from the large to small scale and apply energetic particle measurements to important problems in interplanetary turbulence. I introduce two energetic-particle features, one of which I discovered in the course of this work, which have size scales roughly that of the correlation scale of the turbulence (the largest scale over which observations are expected to be similar). I discuss how multi-spacecraft measurements of these energetic particle features can provide a measure of the correlation scale independent of the magnetic field measurements. Finally, I consider interplanetary scattering and diffusion in detail. I describe new observations of particle diffusion in the direction perpendicular to the average magnetic field, showing that particles only scatter a few times between their injection at the Sun and observation at the Earth. I also provide numerical simulation results of diffusion parallel to the field which can be used to correct for the effects of transport on the particles. These corrections allow inferences to be made about the particle energies at injection from observations of the event-integrated fluences at 1 AU. By carefully including scattering, cooling, field line meandering and turbulence effects, solar-energetic particles become a powerful tool for studying the inner heliosphere.

5

Yu, Jia [Verfasser]. "Measurements of Suprathermal Particles at 1 AU and in the inner Heliosphere / Jia Yu." Kiel : Universitätsbibliothek Kiel, 2018. http://d-nb.info/1160939020/34.

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6

Rouillard, Alexis Paul. "The shielding of galactic cosmic rays by the solar magnetic field in the inner heliosphere." Thesis, University of Southampton, 2007. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.439364.

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7

Magidimisha, Edwin. "A study of the time-dependent modulation of cosmic rays in the inner heliosphere / E. Magidimisha." Thesis, North-West University, 2010. http://hdl.handle.net/10394/4402.

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A two-dimensional (2-D) time-dependent cosmic ray modulation model is used to calculate the modulation of cosmic-ray protons and electrons for 11-and 22-year modulation cycles using a compound approach to describe solar cycle related changes in the transport parameters. The compound approach was developed by Ferreira and Potgieter (2004) and incorporates the concept of propagation diffusion barriers, global changes in the magnetic field, time-dependent gradient, curvature and current-sheet drifts, and other basic modulation mechanisms. By comparing model results with 2.5 GV Ulysses observations, for both protons and electrons, it is shown that the compound approach results in computed intensities on a global scale compatible to observations. The model also computes the expected latitudinal dependence, as measured by the Ulysses spacecraft, for both protons and electrons. This is especially highlighted when computed intensities are compared to observations for the different fast latitude scan (FLS) periods. For cosmic ray protons a significant latitude dependence was observed for the first FLS period which corresponded to solar minimum conditions. For the second, which corresponded to solar maximum, no latitude dependence was observed as was the case for the third FLS period, which again corresponded to moderate to minimum solar activity. For the electrons the opposite occurred with only an observable latitude dependence in intensities for the third FLS period. It is shown that the model results in compatible intensities when compared to observations for these periods. Due to the success of the compound approach, it is also possible to compute charge-sign dependent modulation for 2.5 GV protons and electrons. The electron to proton ratio is presented at Earth and along the Ulysses trajectory. Lastly, it is also shown how the modulation amplitude between solar minimum and maximum depends on rigidity. This is investigated by computing cosmic ray intensities for both protons and electrons, not only at 2:5 GV, but also up to 7:5 GV. A refinement for the compound approach at higher rigidities is proposed.
Thesis (M.Sc. (Space Physics))--North-West University, Potchefstroom Campus, 2011.

8

Dresing, Nina [Verfasser]. "The longitudinal distribution of energetic particles in the inner heliosphere - multi-point observations with STEREO- / Nina Dresing." Kiel : Universitätsbibliothek Kiel, 2014. http://d-nb.info/1052529402/34.

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9

Mallik, Procheta Chandra Vasu. "Diagnostics of solar flare energetic particles : neglected hard X-ray processes and neutron astronomy in the inner heliosphere." Thesis, University of Glasgow, 2010. http://theses.gla.ac.uk/1510/.

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For work on my thesis dissertation, we have been studying some energetic processes in solar flares. On our work on hard X-ray (HXR) emission from flares, we have shown that non-thermal recombination emission can compare with the bremsstrahlung HXR flux for certain flare conditions. In this thesis, we show spectral features characteristic of non-thermal recombination HXR emission and suggest how it plays a signicant role in the flare HXR continuum, something that has been ignored in the past. It is important to note that these results could demand a reconsideration of the numbers of accelerated electrons since recombination can be much more efficient in producing HXR photons than bremsstrahlung. We go on to show that although nonthermal recombination is not likely to dominate the total HXR flux unless we consider extreme parameter regimes, it can still form a signicant proportion of the HXR flux for typical flare conditions, thereby remaining important for both spectral inversion and low energy electron cut-off diagnostic capabilities. In related work on diagnosing particle acceleration in flares, we also have an interest in studying solar neutrons. To this end, this thesis presents our work done with new-age neutron detectors developed by our colleagues at the University of New Hampshire. Using laboratory and simulated data from the detector to produce its response matrix, we then employ regularisation and deconvolution techniques to produce encouraging results for data inversion. As a corollary, we have been reconsidering the role of inverse Compton scattering (ICS) of photospheric photons. Gamma-ray observations clearly show the presence of 100 MeV electrons and positrons in the solar corona, by-products of GeV energy ions. We present results of ICS of solar flare photons taking proper account of radiation field geometry near the solar surface. If observed, such radiation would let us determine the number of secondary positrons produced in large flares, contributing to a full picture of ion acceleration and to predicting neutron fluxes to be encountered by future inner heliosphere space missions.

10

Pacheco, Mateo Daniel. "Analysis and modelling of the solar energetic particle radiation environment in the inner heliosphere in preparation for Solar Orbiter." Doctoral thesis, Universitat de Barcelona, 2019. http://hdl.handle.net/10803/667033.

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The Sun is the main source of all kind of solar energetic particles in the Solar System, electrons, protons and ions with energies from few keV to several GeV. These particles are released from the solar corona and spread through the interplanetary space, the heliosphere, influenced by the interplanetary magnetic field and arriving to the Earth and interacting with the terrestrial magnetosphere. The effects of SEP interactions with space-based devices, manned missions and the Earth atmosphere are encompassed by what is known as space weather. This thesis describes the work we performed on this field, that can be divided in three parts: i) observational studies of solar energetic particles carried out using data coming from space-based missions such as STEREO and Helios, as well as tools like SEPEM server; ii) the development of tools and particle instrument modelling in order to use of them with pre-existing models to be used in the simulation of solar events; iii) solar energetic particle event simulations making use of transport models, either adapting tools previously developed by our group, as SEPInversion, or creating new software capable of carrying out full inversions of events, that is, taking into account the angular response and the energetic response of the particle instrument. These tools developed during this work have allow us to study and characterise the radiation conditions in the inner heliosphere applying modelling techniques never used done before. We also explore some of the applications of these tools. We developed a study about the radial dependence of electron peak intensities and anisotropy, we simulate observations of EPD/EPT instrument on board Solar Orbiter using Helios data and finally we studied the expected cumulated fluence and the fluence spectra computed using SEPEM for Solar Orbiter mission. In conclusion, the obtained results as well as the developed tools will be very useful for the study and interpretation of the future scientific data coming from Parker Solar Probe, Solar Orbiter and BepiColombo.
El Sol és la principal font de partícules que podem trobar al medi interplanetari del sistema solar, i els esdeveniments solars de partícules energètiques són la principal font de radiació dins de l'heliosfera. L'estudi i predicció d'aquest tipus d'esdeveniments i les seves causes i conseqüències ha esdevingut una àrea d'especial interès per la seva importància enfront dels perills que suposa aquesta radiació per a les telecomunicacions i la salut durant missions espacials tripulades. En aquesta tesi exposem el treball que hem desenvolupat en aquest camp, dividit en 3 àmbits diferents: i) estudi observacional d'esdeveniments de partícules fent servir dades observacionals de missions espacials com STEREO i Helios, i eines com SEPEM; ii) desenvolupament d'eines i modalització d'instruments de partícules per fer-los servir conjuntament amb els models preexistents per la simulació d'esdeveniments; iii) simulació d'esdeveniments de partícules mitjançant models de transport, tant adaptant eines prèviament desenvolupades pel nostre grup, com SEPInversion, com nou programari capaç de realitzar inversions totals, es a dir, tenint en compte la resposta angular i energètica dels instruments. Les eines desenvolupades ens han permès estudiar les condicions de radiació a l'heliosfera interior com no s'havia fet fins ara. Els resultats obtinguts així com aquestes eines seran molt útils per a l'estudi i interpretació de les dades científiques provinents de les futures missions espacials com Parker Solar Probe o Solar Orbiter. A més a més, les eines desenvolupades ens permetran fer un ús efectiu d'aquestes dades tan aviat com estiguin disponibles.

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Книги з теми "Inner-Heliosphere":

1

Schwenn, Rainer, and Eckart Marsch, eds. Physics of the Inner Heliosphere I. Berlin, Heidelberg: Springer Berlin Heidelberg, 1990. http://dx.doi.org/10.1007/978-3-642-75361-9.

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2

Schwenn, Rainer, and Eckart Marsch, eds. Physics of the Inner Heliosphere II. Berlin, Heidelberg: Springer Berlin Heidelberg, 1991. http://dx.doi.org/10.1007/978-3-642-75364-0.

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3

Robinson, Ian Michael. Injection and propagation of energetic electrons within the inner heliosphere. Birmingham: University of Birmingham, 2002.

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4

United States. National Aeronautics and Space Administration., ed. [Physics of the inner heliosphere: Mechanisms, models and observational signatures: semiannual progress reports, 1 May 1986 -30 Apr. 1987. [Washington, DC: National Aeronautics and Space Administration, 1987.

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5

International IGPP Conference (5th 2006 Honolulu, Hawaii). Physics of the inner heliosheath: Voyager observations, theory, and future prospects : 5th annual IGPP International Astrophysics Conference. Edited by Heerikhuisen Jacob, American Institute of Physics, and University of California, Riverside. Institute of Geophysics and Planetary Physics. Melville, New York: American Institute of Physics, 2006.

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6

Physics of the inner heliosphere. Berlin: Springer-Verlag, 1991.

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7

Salem, Chadi, and Olga Panasenco. Physics of the Solar Corona and Inner Heliosphere. Wiley & Sons, Limited, John, 2018.

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8

Marsch, Eckart, and Rainer Schwenn. Physics of the Inner Heliosphere I: Large-Scale Phenomena. Springer London, Limited, 2012.

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9

Marsch, Eckart, and Rainer Schwenn. Physics of the Inner Heliosphere I: Large-Scale Phenomena. Springer London, Limited, 2011.

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10

Marsch, Eckart, and Rainer Schwenn. Physics of the Inner Heliosphere II: Particles, Waves and Turbulence. Springer, 2012.

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Частини книг з теми "Inner-Heliosphere":

1

Suess, S. T., J. L. Phillips, D. J. McComas, B. E. Goldstein, M. Neugebauer, and S. Nerney. "The Solar Wind — Inner Heliosphere." In Cosmic Rays in the Heliosphere, 75–86. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-017-1189-0_7.

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2

Balogh, A. "Magnetic Fields in the Inner Heliosphere." In Cosmic Rays in the Heliosphere, 93–104. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-017-1189-0_9.

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3

Ponyavin, Dmitri I. "Geomagnetic Tracing of the Inner Heliosphere." In The 3-D Heliosphere at Solar Maximum, 225–28. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-017-3230-7_36.

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4

Webber, W. R., and J. A. Lockwood. "The Inner Heliosphere — Outer Heliosphere Comparison for Cosmic Ray Modulation." In Cosmic Rays in the Heliosphere, 159–67. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-017-1189-0_14.

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5

Marsch, Eckart, and Rainer Schwenn. "Introduction." In Physics of the Inner Heliosphere I, 1–12. Berlin, Heidelberg: Springer Berlin Heidelberg, 1990. http://dx.doi.org/10.1007/978-3-642-75361-9_1.

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6

Bird, Michael K., and Peter Edenhofer. "Remote Sensing Observations of the Solar Corona." In Physics of the Inner Heliosphere I, 13–97. Berlin, Heidelberg: Springer Berlin Heidelberg, 1990. http://dx.doi.org/10.1007/978-3-642-75361-9_2.

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7

Schwenn, Rainer. "Large-Scale Structure of the Interplanetary Medium." In Physics of the Inner Heliosphere I, 99–181. Berlin, Heidelberg: Springer Berlin Heidelberg, 1990. http://dx.doi.org/10.1007/978-3-642-75361-9_3.

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8

Mariani, Franco, and Fritz M. Neubauer. "The Interplanetary Magnetic Field." In Physics of the Inner Heliosphere I, 183–206. Berlin, Heidelberg: Springer Berlin Heidelberg, 1990. http://dx.doi.org/10.1007/978-3-642-75361-9_4.

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9

Leinert, Christoph, and Eberhard Grün. "Interplanetary Dust." In Physics of the Inner Heliosphere I, 207–75. Berlin, Heidelberg: Springer Berlin Heidelberg, 1990. http://dx.doi.org/10.1007/978-3-642-75361-9_5.

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Simnett, George M. "Studies of Energetic Ions in the Inner Heliosphere." In Energetic Particles in the Heliosphere, 89–119. Cham: Springer International Publishing, 2016. http://dx.doi.org/10.1007/978-3-319-43495-7_5.

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Тези доповідей конференцій з теми "Inner-Heliosphere":

1

FERREIRA, S. E. S., and E. MAGIDIMISHA. "COSMIC RAYS IN THE INNER HELIOSPHERE." In Proceedings of the MG12 Meeting on General Relativity. WORLD SCIENTIFIC, 2012. http://dx.doi.org/10.1142/9789814374552_0087.

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2

Romashets, E. "Interaction Of Magnetic Clouds In The Inner Heliosphere." In SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP, 2003. http://dx.doi.org/10.1063/1.1618712.

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3

Riley, Pete, M. Maksimovic, K. Issautier, N. Meyer-Vernet, M. Moncuquet, and F. Pantellini. "The Three-Dimensional Structure of the Inner Heliosphere." In TWELFTH INTERNATIONAL SOLAR WIND CONFERENCE. AIP, 2010. http://dx.doi.org/10.1063/1.3395865.

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4

Gulisano, Adriana Maria, Pascal Démoulin, Sergio Dasso, Maria Emilia Ruiz, Eckart Marsch, M. Maksimovic, K. Issautier, N. Meyer-Vernet, M. Moncuquet, and F. Pantellini. "Evolution of magnetic clouds in the inner heliosphere." In TWELFTH INTERNATIONAL SOLAR WIND CONFERENCE. AIP, 2010. http://dx.doi.org/10.1063/1.3395884.

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5

Wiedenbeck, M. E. "How Common is Energetic 3He in the Inner Heliosphere?" In SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP, 2003. http://dx.doi.org/10.1063/1.1618679.

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6

Romashets, Eugene. "Propagation of a Toroidal Magnetic Cloud through the Inner Heliosphere." In SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP, 2003. http://dx.doi.org/10.1063/1.1618571.

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7

Ruzmaikin, Alexander. "Multi-Angle Viewing of the Sun and the Inner Heliosphere." In SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP, 2003. http://dx.doi.org/10.1063/1.1618718.

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8

Iju, Tomoya, Munetoshi Tokumaru, and Ken'ichi Fujiki. "Kinematics of interplanetary coronal mass ejections in the inner heliosphere." In SOLAR WIND 13: Proceedings of the Thirteenth International Solar Wind Conference. AIP, 2013. http://dx.doi.org/10.1063/1.4811018.

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9

Bravar, Ulisse, Paul J. Bruillard, Erwin O. Flueckiger, Alec L. MacKinnon, John R. Macri, Procheta C. Mallik, Mark L. McConnell, Michael R. Moser, and James M. Ryan. "Imaging solar neutrons below 10 MeV in the inner heliosphere." In Optics & Photonics 2005, edited by Silvano Fineschi and Rodney A. Viereck. SPIE, 2005. http://dx.doi.org/10.1117/12.617392.

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10

Ruiz, M. E., S. Dasso, W. H. Matthaeus, E. Marsch, J. M. Weygand, M. Maksimovic, K. Issautier, N. Meyer-Vernet, M. Moncuquet, and F. Pantellini. "Anisotropy of the magnetic correlation function in the inner heliosphere." In TWELFTH INTERNATIONAL SOLAR WIND CONFERENCE. AIP, 2010. http://dx.doi.org/10.1063/1.3395826.

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Звіти організацій з теми "Inner-Heliosphere":

1

Manoharan, P. K., K. Mahalakshmi, A. Johri, B. V. Jackson, D. Ravikumar, K. Kalyanasundaram, S. P. Subramanian, and A. K. Mittal. Current State of Reduced Solar Activity: Intense Space Weather Events in the Inner Heliosphere. Balkan, Black sea and Caspian sea Regional Network for Space Weather Studies, December 2018. http://dx.doi.org/10.31401/sungeo.2018.02.03.

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