Gotowe bibliografie tematyczne / Cosmic ray modulation

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Gotowa bibliografia na temat „Cosmic ray modulation”

Autor: Grafiati

Data publikacji: 6 września 2023

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Artykuły w czasopismach na temat "Cosmic ray modulation"

Mishra, R. A., i R. K. Mishra. "Cosmic ray modulation at neutron monitor energies". Kosmìčna nauka ì tehnologìâ 14, nr 3 (30.05.2008): 19–28. http://dx.doi.org/10.15407/knit2008.03.019.

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Dorman, Lev I. "Cosmic ray modulation". Nuclear Physics B - Proceedings Supplements 22, nr 2 (lipiec 1991): 21–45. http://dx.doi.org/10.1016/0920-5632(91)90005-y.

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Moraal, H. "Cosmic-Ray Modulation Equations". Space Science Reviews 176, nr 1-4 (24.09.2011): 299–319. http://dx.doi.org/10.1007/s11214-011-9819-3.

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Герасимова, Сардаана, Sardaana Gerasimova, Петр Гололобов, Peter Gololobov, Владислав Григорьев, Vladislav Grigoryev, Прокопий Кривошапкин i in. "Heliospheric modulation of cosmic rays: model and observation". Solar-Terrestrial Physics 3, nr 1 (5.05.2017): 78–102. http://dx.doi.org/10.12737/article_58f970f2455545.93154609.

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This paper presents the basic model of cosmic ray modulation in the heliosphere, developed in Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy of the Siberian Branch of RAS. The model has only one free modulation parameter: the ratio of the regular magnetic field to the turbulent one. It may also be applied to the description of cosmic ray intensity variations in a wide energy range from 100 MeV to 100 GeV. Possible mechanisms of generation of the mentioned turbulence field are considered. The primary assumption about the electrical neutrality of the heliosphere appears to be wrong, and the zero potential needed to match the model with observations in the plane of the solar equator can be achieved if the frontal point of the heliosphere, which is flowed around by interstellar gas, lies near the mentioned plane. We have revealed that the abnormal rise of cosmic ray intensity at the end of solar cycle 23 is related to the residual modulation produced by the subsonic solar wind behind the front of a standing shock wave. The model is used to describe features of cosmic ray intensity variations in several solar activity cycles.

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Ferreira, Stefan E. S. "Theory of cosmic ray modulation". Proceedings of the International Astronomical Union 4, S257 (wrzesień 2008): 429–38. http://dx.doi.org/10.1017/s1743921309029664.

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AbstractThis work aims to give a brief overview on the topic of cosmic ray modulation in the heliosphere. The heliosphere, heliospheric magnetic field, transport parameters and the transport equation together with modulation models, which solve this equation in various degree of complexity, are briefly discussed. Results from these models are then presented where first it is shown how cosmic rays are globally distributed in an asymmetrical heliosphere which results from the relative motion between the local interstellar medium and the Sun. Next the focus shifts to low-energy Jovian electrons. The intensities of these electrons, which originate from a point source in the inner heliosphere, exhibit a unique three-dimensional spiral structure where most of the particles are transported along the magnetic field lines. Time-dependent modulation is also discussed where it is shown how drift effects together with propagating diffusion barriers are responsible for modulation over a solar cycle.

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Duldig, M. L. "Australian Cosmic Ray Modulation Research". Publications of the Astronomical Society of Australia 18, nr 1 (2001): 12–40. http://dx.doi.org/10.1071/as01003.

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AbstractAustralian research into variations of the cosmic ray flux arriving at the Earth has played a pivotal role for more than 50 years. The work has been largely led by the groups from the University of Tasmania and the Australian Antarctic Division, and has involved the operation of neutron monitors and muon telescopes from many sites. In this paper, the achievements of the Australian researchers are reviewed and future experiments are described. Particular highlights include: the determination of cosmic ray modulation parameters; the development of techniques for modelling ground-level enhancements; the confirmation of the Tail-In and Loss-Cone sidereal anisotropies; the Spaceship Earth collaboration; and the Solar Cycle latitude survey.

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Manuel, R., S. E. S. Ferreira, M. S. Potgieter, R. D. Strauss i N. E. Engelbrecht. "Time-dependent cosmic ray modulation". Advances in Space Research 47, nr 9 (maj 2011): 1529–37. http://dx.doi.org/10.1016/j.asr.2010.12.007.

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Starodubtsev, Sergei. "Shape of spectrum of galactic cosmic ray intensity fluctuations". Solar-Terrestrial Physics 8, nr 2 (30.06.2022): 71–75. http://dx.doi.org/10.12737/stp-82202211.

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The impact of solar wind plasma on fluxes of galactic cosmic rays (CR) penetrating from the outside into the heliosphere with energies above ~1 GeV leads to temporal variations in the CR intensity in a wide frequency range. Cosmic rays being charged particles, their modulation occurs mainly under impacts of the interplanetary magnetic field. It is well known that the observed spectrum of interplanetary magnetic field (IMF) fluctuations in a wide frequency range ν from ~10–7 to ~10 Hz has a pronounced falling character and consists of three sections: energy, inertial, and dissipative. Each of them is described by the power law PIMF(ν)~ν–α, while the IMF spectrum index α increases with increasing frequency. The IMF fluctuations in each of these sections are also characterized by properties that depend on their nature. Also known are established links between fluctuation spectra of the interplanetary magnetic field and galactic cosmic rays in the case of modulation of the latter by Alfvén or fast magnetosonic waves. The theory predicts that fluctuation spectra of cosmic rays should also be described by the power law PCR(ν)~ν–γ. However, the results of many years of SHICRA SB RAS research into the nature and properties of cosmic ray intensity fluctuations based on data from neutron monitors at stations with different geomagnetic cut-offs RC from 0.5 to 6.3 GV show that the observed spectrum of fluctuations in galactic cosmic ray intensity in the frequency range above 10–4 Hz becomes flat, i.e. it is similar to white noise. This fact needs to be realized and explained. This paper reports the results of research into the shape of the spectrum of galactic cosmic ray intensity fluctuations within a frequency range ν from ~10–6 to ~1 Hz and compares them with model calculations of white noise spectra, using measurement data from the neutron monitor of the Apatity station. A possible physical explanation has been given for the observed shape of the cosmic ray fluctuation spectrum on the basis of the known mechanisms of their modulation in the heliosphere.

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Jokipii, J. R. "The physics of cosmic-ray modulation". Advances in Space Research 9, nr 12 (styczeń 1989): 105–19. http://dx.doi.org/10.1016/0273-1177(89)90317-7.

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Mori, S. "Cosmic-ray modulation ground-based observations". Il Nuovo Cimento C 19, nr 5 (wrzesień 1996): 791–804. http://dx.doi.org/10.1007/bf02506669.

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Rozprawy doktorskie na temat "Cosmic ray modulation"

Vos, Etienne Eben. "Cosmic ray modulation processes in the heliosphere / Vos E.E". Thesis, North-West University, 2011. http://hdl.handle.net/10394/7266.

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The solar minimum of 2009 has been identified as an exceptional event with regard to cosmic ray (CR)modulation, since conditions in the heliosphere have reached unprecedented quiet levels. This unique minimum has been observed by the Earth–orbiting satellite, PAMELA, launched in June, 2006, from which vast sets of accurate proton and electron preliminary observations have been made available. These simultaneous measurements from PAMELA provide the ideal opportunity to conduct an in–depth study of CR modulation, in particular charge–sign dependent modulation. In utilizing this opportunity, a three–dimensional, steady–state modulation model was used to reproduce a selection of consecutive PAMELA proton and electron spectra from 2006 to 2009. Thiswas done by assuming full drifts and simplified diffusion coefficients, where the rigidity dependence and absolute value of themean free paths for protons and electrons were sequentially adjusted below 3 GV and 300 MV, respectively. Care has been taken in calculating yearly–averaged current–sheet tilt angle and magnetic field values that correspond to the PAMELA spectra. Following this study where the numerical model was used to investigate the individual effects resulting from changes in the tilt angle, diffusion coefficients, and global drifts, it was found that all these modulation processes played significant roles in contributing to the total increase in CR intensities from 2006 to 2009, as was observed by PAMELA. Furthermore, the effect that drifts has on oppositely charged particles was also evident from the difference between the peak–shaped time profiles of protons and the flatter time profiles of electrons, as is expected for an A < 0 polarity cycle. Since protons, which drift into the heliosphere along the heliospheric current–sheet, haven’t yet reached maximum intensity levels by 2008, their intensities increased notably more than electrons toward the end of 2009. The time and energy dependence of the electron to proton ratios were also studied in order to further illustrate and quantify the effect of drifts during this remarkable solar minimum period.
Thesis (M.Sc. (Physics))--North-West University, Potchefstroom Campus, 2012.

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KO, CHUNG-MING. "COSMIC-RAY MODIFIED STELLAR WINDS (ACCELERATION, MODULATION, DIFFUSION, TRANSONIC SOLUTION)". Diss., The University of Arizona, 1986. http://hdl.handle.net/10150/183980.

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A two fluid hydrodynamical model describing the modification of a stellar wind flow due to its interaction with galactic cosmic-rays is investigated. The two fluids consist of the thermal stellar wind gas and the galactic cosmic-rays. A polytropic one fluid model is used to describe the stellar wind gas, and the cosmic-rays modify the wind via their pressure gradient. The cosmic-rays are considered to be a hot low density gas of negligible mass flux, but with a significant pressure and energy flux compared to the thermal gas. The equations used are essentially those employed in two fluid hydrodynamical models of cosmic-ray shock acceleration by the first order Fermi mechanism, but suitably modified to apply in a spherical geometry and including the effects of gravity on the flow. The stellar wind consists of a transonic flow with a termination shock, and subsonic flow outside the shock. The model shows the deceleration of the wind upstream of the shock by the positive galactic cosmic-ray pressure gradient. The dissertation first discusses the fluid polytropic stellar winds and how to insert shocks in the flow. The hydrodynamical equations governing cosmic-ray modified winds are then introduced followed by a discussion of the physics of the interaction between the thermal stellar wind and the cosmic-rays. A description of the singularities of the equations is also presented. The system of equations is first solved by a finite difference method in the test particle approximation in which the cosmic-rays do not modify the flow, with appropriate boundary conditions applied at infinity, at the wind termination shock, and at the star. A perturbation scheme to determine the modification of the wind by the cosmic-rays is then developed. This scheme applies when the modification of the wind by the cosmic-rays is sufficiently small. Finally a numerical iteration is employed to exactly solve the equations. This latter method has the advantage that it can be applied when there is a considerable modification of the wind by the cosmic-rays.

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Gieseler, Jan [Verfasser]. "Understanding Galactic Cosmic Ray Modulation: Observations and Theory / Jan Gieseler". Kiel : Universitätsbibliothek Kiel, 2018. http://d-nb.info/1155760816/34.

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Ngobeni, Mabedle Donald. "Aspects of the modulation of cosmic rays in the outer heliosphere / by Mabedle Donald Ngobeni". Thesis, North-West University, 2006. http://hdl.handle.net/10394/97.

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A time-dependent two-dimensional (2D) modulation model including drifts, the solar wind tennination shock (TS) with diffusive shock acceleration and a heliosheath based on the Parker (1965) transport equation is used to study the modulation of galactic cosmic rays (GCRs) and the anomalous component of cosmic rays (ACRs) in the heliosphere. In particular, the latitude dependence of the TS compression ratio and injection efficiency of the ACRs (source strength) based on the hydrodynamic modeling results of Scherer et al. (2006) is used for the first time in a modulation model. The subsequent effects on differential intensities for both GCRs and ACRs are illustrated, comparing them to the values without a latitude dependence for these parameters. It is found that the latitude dependence of these parameters is important and that it enables an improved description of the modulation of ACRs beyond the TS. With this modeling approach (without fitting observations) to the latitude dependence of the two parameters, it is possible to obtain a TS spectrum for ACRs at a polar angle of B = 55" that qualitatively approximates the main features of the Voyager 1 observations. This positive result has to be investigated further. Additionally, it is shown that the enhancement of the cosmic ray intensity just below the cut-off energy found for the ACR at the TS in an A < 0 magnetic polarity cycle in the equatorial plane with the latitude independent scenario, disappears in this region when the latitude dependence of the compression ratio and injection efficiency is assumed. Subsequent effects of these scenarios are illustrated on the global anisotropy vector of both GCRs and ACRs as the main theme of this work. For this purpose the radial and latitudinal gradients for GCRs and ACRs were accurately computed. The radial and latitudinal anisotropy components were then computed as a function of energy, radial distance and polar angle. It is also the first time that the anisotropy vector is comprehensively calculated in such a global approach to cosmic ray modeling in the heliosphere, in particular for ACRs. It is shown that the anisotropy vector inside (up-stream) and outside (down-stream) the TS behaves in a complicated way, so care must be taken in interpreting it. It is found that the latitude dependence of the two mentioned parameters can alter the direction (sign) of the anisotropy vector. Its behaviour beyond the TS is markedly different from inside the TS, mainly because of the slower solar wind velocity, with less dependence on the magnetic polarity cycles.
Thesis (M.Sc. (Physics))--North-West University, Potchefstroom Campus, 2007.

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Krüger, Tjaart Petrus Jakobus. "The effect of a Fisk-Parker hybrid magnetic field on cosmic rays in the heliosphere / Tjaart P.J. Krüger". Thesis, North-West University, 2005. http://hdl.handle.net/10394/1205.

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The existence of a Fisk-type heliospheric magnetic field (HMF) is one of the most debated questions in cosmic-ray modulation. Recently, Burger and Hitge [2004] developed a divergence-free Fisk-Parker hybrid magnetic field model to demonstrate the behaviour of cosmic rays in the heliosphere due to such a field. This approach has been refined and the properties of the consequent field are investigated. It is found that randomly directed magnetic field diffusion in and above the photosphere significantly influences the solar magnetic field both at the solar poles and near the polar coronal hole boundary. The solar cycle dependence of this field is investigated, a study which is of particular importance for studies of the long-term behaviour of cosmic rays, such as those undertaken at the SANAE base in Antarctica. The amplitudes of the 26-day recurrent cosmic-ray variations are modelled as function of both latitudinal gradient and heliolatitude and are found to agree qualitatively and in some cases quantitatively with the observational results reported by Zhang 119971 and Paizis et al. 119991. Although magnetic field data do not clearly indicate the existence of the Fisk field [see, e.g., Fursyth et al., 20021, this study supports the existence of a Fisk-type HMF.
Thesis (M.Sc. (Physics))--North-West University, Potchefstroom Campus, 2006.

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Krüger, Helena. "A calibration neutron monitor for long-term cosmic ray modulation studies / H. Krüger". Thesis, North-West University, 2006. http://hdl.handle.net/10394/1023.

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The propagation of high-energy cosmic rays is influenced by the time-varying heliospheric magnetic field embedded in the solar wind, and by the geomagnetic field. To penetrate through this geomagnetic field, they must have a rigidity that exceeds the geomagnetic cutoff rigidity for a given position on the earth. In the atmosphere, the primary cosmic rays interact with atmospheric nuclei, to form a cascade of secondary particles. Neutron monitors record these secondary cosmic rays, mainly the neutrons, with energies about a decade higher than detected by most spacecraft. Since neutron monitors are integral detectors, each with its own detection efficiency, energy spectra cannot readily be derived from their observations. One way to circumvent this is by conducting latitudinal surveys with mobile neutron monitors. Another way is to use the worldwide stationary neutron monitor network, but then the counting rates of these monitors must be normalised sufficiently accurate against one another. For this reason two portable calibration neutron monitors were built at the Potchefstroom campus of the North-West University and completed in 2002. To achieve sufficient calibration accuracy, several properties of the calibrator are investigated in this work. Effects such as atmospheric pressure variations, diurnal variations, short-term scintillations, and multiplicity, contribute to the fluctuations of the counting rate of a neutron monitor. Due to these effects, the coefficient of variation of the calibrator is determined to be -40% larger than the Poisson deviation. The energy response of the calibrator over the cutoff rigidity interval from the poles to the equator is investigated, with the result that it is almost 4% larger than that of a standard 3NM64 neutron monitor. It is also determined that not only the calibrator, but also the stationary NM64 and IGY neutron monitors, have fairly large instrumental temperature sensitivity, which must be accounted for in calibration procedures. Furthermore, the calibrator has a large sensitivity to the type of surface beneath it, influencing its counting rate by as much as 5%. This investigation is incomplete and requires further experimentation before the calibration of the stationary neutron monitors can start. When calibrations of a significant number of the worldwide neutron monitors are done, their intensity spectra as derived from differential response functions, will provide experimental data for modulation studies at rigidities above 1 GV.
Thesis (Ph.D. (Physics))--North-West University, Potchefstroom Campus, 2006.

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Nndanganeni, Rendani Rejoyce. "Modelling of galactic cosmic ray electrons in the heliosphere / Nndanganeni, R.R". Thesis, North-West University, 2012. http://hdl.handle.net/10394/7034.

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The Voyager 1 spacecraft is now about 25 AU beyond the heliospheric termination shock and soon it should encounter the outer boundary of the heliosphere, the heliopause. This is set to be at 120 AU in the modulation model used for this study. This implies that Voyager 1, and soon afterwards also Voyager 2, should be able to measure the heliopause spectrum, to be interpreted as the lowest possible local interstellar spectrum, for low energy galactic electrons (1 MeV to 120 MeV). This could give an answer to a long outstanding question about the spectral shape (energy dependence) of the galactic electron spectrum at these low energies. These in situ electron observations from Voyager 1, until the year 2010 when it was already beyond 112 AU, are used for a comparative study with a comprehensive three dimensional numerical model for the solar modulation of galactic electrons from the inner to the outer heliosphere. A locally developed steady state modulation model which numerically solves the relevant heliospheric transport equation is used to compute and study modulated electron spectra from Earth up to the heliopause. The issue of the spectral shape of the local interstellar spectrum at these low energies is specifically addressed, taking into account modulation in the inner heliosheath, up to the heliopause, including the effects of the transition of the solar wind speed from supersonic to subsonic in the heliosheath. Modulated electron spectra from the inner to the outer heliosphere are computed, together with radial and latitudinal profiles, focusing on 12 MeV electrons. This is compared to Voyager 1 observations for the energy range 6–14 MeV. A heliopause electron spectrum is computed and presented as a new plausible local interstellar spectrum from 30 GeV down to 10 MeV. The comparisons between model predictions and observations from Voyager 1 and at Earth (e.g. from the PAMELA mission and from balloon flights) and in the inner heliosphere (e.g. from the Ulysses mission) are made. This enables one to make conclusions about diffusion theory applicable to electrons in the heliosphere, in particular the rigidity dependence of diffusion perpendicular and parallel to the local background solar magnetic field. A general result is that the rigidity dependence of both parallel and perpendicular diffusion coefficients needs to be constant below P < 0.4 GV and only be allowed to increase above this rigidity to assure compatibility between the modeling and observations at Earth and especially in the outer heliosphere. A modification in the radial dependence of the diffusion coefficients in the inner heliosheath is required to compute realistic modulation in this region. With this study, estimates of the intensity of low energy galactic electrons at Earth can be made. A new local interstellar spectrum is computed for these low energies to improve understanding of the modulation galactic electrons as compared to previous results described in the literature.
Thesis (M.Sc. (Physics))--North-West University, Potchefstroom Campus, 2012.

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Engelbrecht, Nicholas Eugéne. "On the heliospheric diffusion tensor and its effect on 26-day recurrent cosmic-ray variations / N.E. Engelbrecht". Thesis, North-West University, 2008. http://hdl.handle.net/10394/2052.

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Nkosi, Godfrey Sibusiso. "A study of cosmic ray anisotropies in the heliosphere / Godfrey Sibusiso Nkosi". Thesis, North-West University, 2006. http://hdl.handle.net/10394/1627.

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Strauss, Roelf du Toit. "Modelling of cosmic ray modulation in the heliosphere by stochastic processes / Roelf du Toit Strauss". Thesis, North-West University, 2013. http://hdl.handle.net/10394/10217.

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The transport of cosmic rays in the heliosphere is studied by making use of a newly developed modulation model. This model employes stochastic differential equations to numerically solve the relevant transport equation, making use of this approach’s numerical advantages as well as the opportunity to extract additional information regarding cosmic ray transport and the processes responsible for it. The propagation times and energy losses of galactic electrons and protons are calculated for different drift cycles. It is confirmed that protons and electrons lose the same amount of rigidity when they experience the same transport processes. These particles spend more time in the heliosphere, and also lose more energy, in the drift cycle where they drift towards Earth mainly along the heliospheric current sheet. The propagation times of galactic protons from the heliopause to Earth are calculated for increasing heliospheric tilt angles and it is found that current sheet drift becomes less effective with increasing solar activity. Comparing calculated propagation times of Jovian electrons with observations, the transport parameters are constrained to find that 50% of 6 MeV electrons measured at Earth are of Jovian origin. Charge-sign dependent modulation is modelled by simulating the proton to anti-proton ratio at Earth and comparing the results to recent PAMELA observations. A hybrid cosmic ray modulation model is constructed by coupling the numerical modulation model to the heliospheric environment as simulated by a magneto-hydrodynamic model. Using this model, it is shown that cosmic ray modulation persists beyond the heliopause. The level of modulation in this region is found to exhibit solar cycle related changes and, more importantly, is independent of the magnitude of the individual diffusion coefficients, but is rather determined by the ratio of parallel to perpendicular diffusion.
PhD (Space Physics), North-West University, Potchefstroom Campus, 2013

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Książki na temat "Cosmic ray modulation"

S, Potgieter M., COSPAR Scientific Assembly i COSPAR Scientific Commission D, red. Heliospheric cosmic ray transport, modulation and turbulence. Kidlington, Oxford: Published for the Committee on Space Research [by] Elsevier, 2005.

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F, Burlaga L., i Goddard Space Flight Center, red. Cosmic ray modulation and turbulent interaction regions near 11 AU. Greenbelt, MD: National Aeronautics and Space Administration, Goddard Space Flight Center, 1985.

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Usoskin, Ilya G. Solar activity changes and modulation of cosmic rays. Oulu: University of Oulu, 2000.

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Części książek na temat "Cosmic ray modulation"

Moraal, H. "Cosmic-Ray Modulation Equations". W Cosmic Rays in the Heliosphere, 299–319. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4614-9200-9_22.

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McDonald, Frank B. "Cosmic-Ray Modulation in the Heliosphere". W Cosmic Rays in the Heliosphere, 33–50. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-017-1189-0_4.

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Fisk, L. A., K. P. Wenzel, A. Balogh, R. A. Burger, A. C. Cummings, P. Evenson, B. Heber i in. "Global Processes that Determine Cosmic Ray Modulation". W Cosmic Rays in the Heliosphere, 179–214. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-017-1189-0_16.

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Mckibben, R. B., J. J. Connell, C. Lopate, J. A. Simpson i M. Zhang. "Cosmic Ray Modulation in the 3-D Heliosphere". W The High Latitude Heliosphere, 367–78. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-011-0167-7_62.

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Webber, W. R., i J. A. Lockwood. "The Inner Heliosphere — Outer Heliosphere Comparison for Cosmic Ray Modulation". W 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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Cliver, E. W., I. G. Richardson i A. G. Ling. "Solar Drivers of 11-yr and Long-Term Cosmic Ray Modulation". W Cosmic Rays in the Heliosphere, 3–19. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4614-9200-9_2.

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Jokipii, J. R. "Effects of Three-Dimensional Heliospheric Structures on Cosmic-Ray Modulation". W Astrophysics and Space Science Library, 375–87. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4612-5_45.

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Heber, B., i R. G. Marsden. "Cosmic Ray Modulation Over the Poles at Solar Maximum: Observations". W The 3-D Heliosphere at Solar Maximum, 309–19. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-017-3230-7_50.

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Wibberenz, G., H. V. Cane, I. G. Richardson i T. T. Von Rosenvinge. "The Influence of Tilt Angle and Magnetic Field Variations on Cosmic Ray Modulation". W The 3-D Heliosphere at Solar Maximum, 343–47. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-017-3230-7_55.

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Toptygin, I. N. "Modulation of Galactic Cosmic Rays". W Cosmic Rays in Interplanetary Magnetic Fields, 290–331. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5257-7_5.

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Streszczenia konferencji na temat "Cosmic ray modulation"

Munini, Riccardo. "SOLAR MODULATION OF GALACTIC-COSMIC RAY ANTIPROTONS". W 37th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2021. http://dx.doi.org/10.22323/1.395.1328.

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Munini, Riccardo, Driaan Bisschoff, Mirko Boezio, Alex Lenni, Wolfgang Menn, Nadir Marcelli, Marius Potgieter i O. Aslam. "Isotope solar modulation with the PAMELA experiment". W 36th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2019. http://dx.doi.org/10.22323/1.358.1130.

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Solanik, Michal, Pavol Bobik i Jan Genci. "Cosmic rays modulation in heliosphere models on GPU". W 37th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2021. http://dx.doi.org/10.22323/1.395.1320.

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Aslam, Ottupara Muhammed, Driaan Bisschoff i Marius Potgieter. "The solar modulation of protons and anti-protons". W 36th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2019. http://dx.doi.org/10.22323/1.358.1054.

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Song, Xiaojian. "Study Galactic Cosmic Ray Modulation with AMS-02 observation". W 37th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2021. http://dx.doi.org/10.22323/1.395.1354.

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Mykhailenko, Viacheslav, i Pavol Bobik. "Cosmic ray modulation error for 2D SDE SOLARPROP model". W 27th European Cosmic Ray Symposium. Trieste, Italy: Sissa Medialab, 2023. http://dx.doi.org/10.22323/1.423.0042.

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Cane, H. V. "ENERGETIC PARTICLES IN THE SOLAR WIND: PROPAGATION, ACCELERATION, AND MODULATION". W 25th International Cosmic Ray Conference. WORLD SCIENTIFIC, 1998. http://dx.doi.org/10.1142/9789814529044_0008.

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Mykhailenko, Viacheslav, i Pavol Bobik. "Statistical error for cosmic rays modulation evaluation by 1D model". W 37th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2021. http://dx.doi.org/10.22323/1.395.1325.

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Miyake, Shoko, Yotaro Migita, Yoichi Asaoka, Yosui Akaike, Shoji Torii, Toshio Terasawa, Ryuho Kataoka i Kenichi Sakai. "Solar Modulation of Galactic Cosmic-Ray Electrons Measured with CALET". W 36th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2019. http://dx.doi.org/10.22323/1.358.1126.

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Kuhlen, Marco, i Philipp Mertsch. "Solar modulation of cosmic rays in a semi-analytical framework". W 36th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2019. http://dx.doi.org/10.22323/1.358.1100.

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Raporty organizacyjne na temat "Cosmic ray modulation"

Cliver, E. W., I. G. Richardson i A. G. Ling. Solar Drivers of 11-yr and Long-Term Cosmic Ray Modulation (PostPrint). Fort Belvoir, VA: Defense Technical Information Center, marzec 2012. http://dx.doi.org/10.21236/ada561709.

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