Results 181 to 190 of about 16,482 (212)

Super-Intense Geomagnetic Storm on 10-11 May 2024: Possible Mechanisms and Impacts. [PDF]

Space Weather
Tulasi Ram S, Veenadhari B, Dimri AP, Bulusu J, Bagiya M, Gurubaran S, Parihar N, Remya B, Seemala G, Singh R, Sripathi S, Singh SV, Vichare G.   +12 more
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Direct imaging of magnetohydrodynamic wave mode conversion near a 3D null point on the sun. [PDF]

Nat Commun
Kumar P, Nakariakov VM, Karpen JT, Cho KS.   +3 more
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Electromotive field in space and astrophysical plasmas. [PDF]

Rev Mod Plasma Phys
Bourdin PA, Narita Y.
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Jets Downstream of Collisionless Shocks: Recent Discoveries and Challenges. [PDF]

Space Sci Rev
Krämer E, Koller F, Suni J, LaMoury AT, Pöppelwerth A, Glebe G, Mohammed-Amin T, Raptis S, Vuorinen L, Weiss S, Xirogiannopoulou N, Archer M, Blanco-Cano X, Gunell H, Hietala H, Karlsson T, Plaschke F, Preisser L, Roberts O, Simon Wedlund C, Temmer M, Vörös Z.   +21 more
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Forecasting solar energetic particles using multi-source data from solar flares, CMEs, and radio bursts with machine learning approaches. [PDF]

Sci Rep
Ali MA, Abdelkawy AGA, Shaltout AMK, Beheary MM.   +3 more
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Partially ionized plasma of the solar atmosphere: recent advances and future pathways. [PDF]

Philos Trans A Math Phys Eng Sci
Hillier AS, Snow B, Luna M.
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Simultaneous Occurrence of Magnetospheric Fluctuations at Different Discrete Frequencies ( f ≈ 1 - 5 mHz): A Review. [PDF]

Space Sci Rev
Di Matteo S, Villante U.
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Mapping the Sun's coronal magnetic field using the Zeeman effect. [PDF]

Sci Adv
Schad TA, Petrie GJD, Kuhn JR, Fehlmann A, Rimmele T, Tritschler A, Woeger F, Scholl I, Williams R, Harrington D, Paraschiv AR, Szente J.   +11 more
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Parametric resonance of Alfvén waves driven by ionization-recombination waves in the weakly ionized solar atmosphere. [PDF]

Philos Trans A Math Phys Eng Sci
Ballai I, Forgács-Dajka E, McMurdo M.
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Solar coronal heating by magnetosonic waves

Monthly Notices of the Royal Astronomical Society, 2001
Solar coronal heating by magnetohydrodynamic (MHD) waves is investigated. ultraviolet (UV) and X-ray emission lines of the corona show non-thermal broadenings. The wave rms velocities inferred from these observations are of the order of 25–60 km s−1. Assuming that these values are not negligible, we solved MHD equations in a quasi-linear approximation,
Pekunlu, ER, Cakirli, O, Ozetken, E
openaire   +2 more sources