Results 201 to 210 of about 3,998,903 (250)

Efficient acceleration of energetic electrons upstream of Earth's bow shock. [PDF]

open access: yesNat Commun
Liu YY   +9 more
europepmc   +1 more source

Chang'E-6 reveals solar wind-dependent H<sup>-</sup> ions on the Moon. [PDF]

open access: yesSci Adv
Zhong T   +15 more
europepmc   +1 more source

The abundances of carbon and nitrogen in the atmospheres of classical Be stars. [PDF]

open access: yesAstrophys Space Sci
Peters GJ   +4 more
europepmc   +1 more source

A hot white dwarf merger remnant revealed by an ultraviolet detection of carbon. [PDF]

open access: yesNat Astron
Sahu S   +9 more
europepmc   +1 more source

Ionic Reactant Orientation Inhibits Ion-Neutral Reactions at Low Temperatures. [PDF]

open access: yesJACS Au
Peng Y   +9 more
europepmc   +1 more source

In Situ Observations of Interstellar Plasma with Voyager 1

Science, 2013
Finally Out Last summer, it was not clear if the Voyager 1 spacecraft had finally crossed the heliopause—the boundary between the heliosphere and interstellar space. Gurnett et al. (p.
William Kurth
exaly   +4 more sources

Radio Propagation Through the Turbulent Interstellar Plasma

Annual Review of Astronomy and Astrophysics, 1990
Article de synthese traitant de la diffusion interstellaire et des plasmas turbulents dans le milieu ...
B J Rickett
exaly   +3 more sources

Interstellar scintillation and the interstellar turbulent plasma

Astronomical and Astrophysical Transactions, 2002
Data on interstellar diffractive and refractive scintillation of pulsars are analyzed. The comparison between the theory and the observational data shows that two types of spectra for electron density fluctuations are realized in the interstellar medium: simple power law and piecewise with a break. The distribution of turbulent plasma in the Galaxy has
V I Shishov
exaly   +2 more sources

The outer turbulence scale in the interstellar plasma

Astronomy Reports, 2002
The structure function for phase fluctuations on spatial scales from 106 to 1017 m is constructed using data on diffractive and refractive scintillation of pulsars, scattering angles, variations in pulse arrival times, and differences in dispersion measures observed for close pairs of pulsars in globular clusters.
V. Shishov, T. Smirnova
semanticscholar   +2 more sources

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