[PDF] Top 20 Radial evolution of the electron distribution functions in the fast solar wind between 0.3 and 1.5 AU
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Radial evolution of the electron distribution functions in the fast solar wind between 0.3 and 1.5 AU
... [ 1 ] Observed electron distribution functions of the solar wind permanently exhibit three different components: a thermal core and a suprathermal halo, ... Voir le document complet
10
The solar wind at solar maximum: comparisons of EISCAT IPS and in situ observations
... success of the MHD model in mapping data from in situ measurements at 300 R S to 30 R S during CR 1976 is im- portant, as we hope to use this model to extend our study closer into the ... Voir le document complet
20
Anticorrelation between the Bulk Speed and the Electron Temperature in the Pristine Solar Wind: First Results from the Parker Solar Probe and Comparison with Helios
... for the full Helios data set, the solar wind bulk speed as a function of the heliocentric distance one can note that, while the fastest solar wind flows are ... Voir le document complet
24
Latitudinal distribution of the solar wind properties in the low- and high-pressure regimes: Wind observations
... Dept. of ESA, ESTEC, 2200 AG Noordwijk, The Netherlands 3 CESR/CNRS, Universite Paul Sabatier, BP 4346, 31029 Toulouse, France Received: 29 November 1999 / Revised: 27 March 2000 / Accepted: 6 April ... Voir le document complet
15
Radial and latitudinal dependencies of discontinuities in the solar wind between 0.3 and 19 AU and ?80° and +10°
... from 5 missions at 7 different locations between 0.3 and 19 AU and −80 ◦ and + 10 ◦ in the 3D heliosphere are investigated during mini- mum solar ...activity. ... Voir le document complet
15
Alpha particle thermodynamics in the inner heliosphere fast solar wind
... reprocessed the original Helios positive ion distribution functions, isolated the alpha particle population, and computed the alpha particle number density, velocity, and ... Voir le document complet
8
A study of magnetic fluctuations and their anomalous scaling in the solar wind: the Ulysses fast-latitude scan
... bulk solar wind ve- locity and magnetic field intensity using Helios data to anal- yse the probability distribution functions (PDFs) of the fluc- tuations while ... Voir le document complet
19
Radial evolution of intermittent heat flux in solar coronal holes
... that the source of ion heat- ing in solar coronal holes is small-scale reconnection events (microflares) at the coronal ...base. The microflares launch in- termittent heat ... Voir le document complet
11
Propagation of electron and proton shock-induced aurora and the role of the interplanetary magnetic field and solar wind
... by the calculated time delay) and the HP for the 28 April 2001 ...= 0 corresponds to the arrival of the shock on the front of the magnetosphere ... Voir le document complet
19
Structure of electron and ion distribution functions near a reconnection line
... L’archive ouverte pluridisciplinaire HAL, est destinée au dépôt et à la diffusion de documents scientifiques de niveau recherche, publiés ou non, émanant des établissements d’enseignemen[r] ... Voir le document complet
10
Rapid density fluctuations in the solar wind
... Abstract. Electron density fluctuations (up to 2.5 Hz) in the solar wind have been studied, using the EFW experiment on the Cluster spacecraft, which measures density ... Voir le document complet
10
Estimating random transverse velocities in the fast solar wind from EISCAT Interplanetary Scintillation measurements
... scattering the phase changes are large and the scattered waves interfere with both the scattered and inci- dent ...that the final scattering pattern is a linear sum of all ... Voir le document complet
14
A 1-2-3-4 result for the 1-2-3 Conjecture in 5-regular graphs
... goal in this paper is to improve the bound on the parameter χ e Σ for 5-regular graphs (which are obviously all nice), by showing that their index is bounded above by ...every 5-regular ... Voir le document complet
15
Inverse spectral problem for radial Schrödinger operator on [0, 1]
... is the key point for such an inverse spectral ...Guillot and Ralston for a = ...with the first Bessel functions into scalar products with trigonometric ...used in [ 2 ] and [ 4 ... Voir le document complet
23
EISCAT measurements of the solar wind
... Department of Electrical and Computer Engineering, University of California, San Diego, USA 3 EISCAT, Sodankyla¨ SF-99600, Suomi/Finland, EU Received: 24 January 1996/Revised 24 April: ... Voir le document complet
12
The cusp: a window for particle exchange between the radiation belt and the solar wind
... effect of the dipole tilt angle on the cusp trapping re- gion can also be evaluated based on the T96 ...Figure 5 shows the shape of the “cusp minimum plane” during ... Voir le document complet
8
Polar observations of electron density distribution in the Earth's magnetosphere. 1. Statistical results
... Introduction The total electron number density is a key parameter needed for both characterizing and understanding the structure and dynamics of the Earth’s ... Voir le document complet
15
The evolution of the ultraviolet and infrared luminosity densities in the universe at 0
... is the complexity of the MIR SED of ...complex and continuous interpolation requires some kind of galaxy SED model which is no longer free of assumptions, often not ... Voir le document complet
11
Modeling of short scale turbulence in the solar wind
... distributions The nonlinear solution is an exact solution for waves prop- agating in one ...For the superposition of the right and the left propagating waves the ... Voir le document complet
8
On the fast response of the Southern Ocean to changes in the zonal wind
... Time evolution of the momentum balance terms In the above discussion it was implied that the extra pressure force on the deep topog- 10 raphy was equal to the extra ... Voir le document complet
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