Results 1 to 10 of about 2,359,939 (384)
The evolution of the solar wind. [PDF]
Living Rev Sol Phys, 2021 How has the solar wind evolved to reach what it is today? In this review, I discuss the long-term evolution of the solar wind, including the evolution of observed properties that are intimately linked to the solar wind: rotation, magnetism and activity.
Vidotto AA.
europepmc +9 more sources
The Solar Wind Energy Flux [PDF]
Solar Physics, 2012 The solar-wind energy flux measured near the ecliptic is known to be independent of the solar-wind speed. Using plasma data from Helios, Ulysses, and Wind covering a large range of latitudes and time, we show that the solar-wind energy flux is independent of the solar-wind speed and latitude within 10%, and that this quantity varies weakly over the ...
Chat, G. Le +2 more
arxiv +18 more sources
Directly comparing coronal and solar wind elemental fractionation [PDF]
A&A 640, A28 (2020), 2020 As the solar wind propagates through the heliosphere, dynamical processes irreversibly erase the signatures of the near-Sun heating and acceleration processes. The elemental fractionation of the solar wind should not change during transit however, making it an ideal tracer of these processes.
Baker, D. +3 more
arxiv +3 more sources
Journal of Research of the National Bureau of Standards, Section D: Radio Propagation, 1961 >Hydrodynamic expansion of the solar corona is the basis for solar corpuscular radiation. The quiet day coronal temperatures of 1 to 2 x 10/sup 6/ deg K yield a solar wind of several hundred km/sec and a density of 5 to 50 particles/cm/sup 3/ at the orbit of Earth.
E. N. Parker
openalex +3 more sources
Quantifying the latitudinal representivity of in situ solar wind observations [PDF]
Journal of Space Weather and Space Climate, 2020 Advanced space-weather forecasting relies on the ability to accurately predict near-Earth solar wind conditions. For this purpose, physics-based, global numerical models of the solar wind are initialized with photospheric magnetic field and coronagraph ...
Owens Mathew J. +4 more
doaj +3 more sources
On slow solar wind with high Alfvénicity: from composition and microphysics to spectral properties [PDF]
Monthly notices of the Royal Astronomical Society, 2018 Alfv\'enic fluctuations are very common features in the solar wind and are found especially within the main portion of fast wind streams while the slow wind usually is less Alfv\'enic and more variable. In general, fast and slow wind show many differences which span from the large scale structure to small scale phenomena including also a different ...
R. D’Amicis, L. Matteini, R. Bruno
arxiv +3 more sources
Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes [PDF]
The Astrophysical Journal, 2023 We investigate the origin of mesoscale structures in the solar wind called microstreams, defined as enhancements in the solar wind speed and temperature that last several hours.
Bahaeddine Gannouni +2 more
doaj +2 more sources
Neutral Solar Wind Generated by Lunar Exospheric Dust at the Terminator [PDF]
, 2008 We calculate the flux of neutral solar wind observed on the lunar surface at the terminator due to solar wind protons penetrating exospheric dust grains with (1) radii greater than 0.1 microns and (2) radii greater than 0.01 microns. For grains with radii larger than 0.1 microns, the ratio of the neutral solar wind flux produced by exospheric dust to ...
Abramowitz +53 more
arxiv +3 more sources
The influence of solar wind variability on magnetospheric ULF wave power [PDF]
Annales Geophysicae, 2015 Magnetospheric ultra-low frequency (ULF) oscillations in the Pc 4–5 frequency range play an important role in the dynamics of Earth's radiation belts, both by enhancing the radial diffusion through incoherent interactions and through the coherent ...
D. Pokhotelov +3 more
doaj +4 more sources
Proton and Electron Temperatures in the Solar Wind and Their Correlations with the Solar Wind Speed
The Astrophysical Journal, 2023 The heating and acceleration of the solar wind remains one of the unsolved fundamental problems in heliophysics. It is usually observed that the proton temperature T _i is highly correlated with the solar wind speed V _SW , while the electron temperature
Chen Shi +10 more
doaj +4 more sources