Results 171 to 180 of about 16,769 (212)

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.
europepmc   +1 more source

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
europepmc   +1 more source

The extreme depletion of ionospheric electron density and its hemispheric asymmetry during the May 2024 storm. [PDF]

Natl Sci Rev
Chen Y, Aa E, Yuan T, Zhang S, Shen H, Yue X, Xu H, Liu S, Wang X, Huang W, Li H, Luo B, Zhang Q, Wang C.   +13 more
europepmc   +1 more source

Observation of super-Alfvénic slippage of reconnecting magnetic field lines on the Sun. [PDF]

Nat Astron
Lörinčík J, Dudík J, Sainz Dalda A, Aulanier G, Polito V, De Pontieu B.   +5 more
europepmc   +1 more source

Contribution of Tearing Instability to Solar Coronal Heating

Contribution of Tearing Instability to Solar Coronal Heating
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Scaling of heating rates in solar coronal loops

Nature, 1995
THE gas of the solar corona is at a temperature of several million degrees, orders of magnitude hotter than the underlying photosphere. The nature of the physical process that heats the solar corona (and the coronae of solar-type stars more generally) has been a long-standing puzzle.
James A. Klimchuk, Lisa J. Porter
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Solar flares, microflares, nanoflares, and coronal heating

Solar Physics, 1991
Solar flare occurrence follows a power-law distribution against total flare energy W: dN/dW ∼ W−α with an index α ∼ 1.8 as determined by several studies. This implies (a) that microflares must have a different, steeper distribution if they are energetically significant, and (b) there must be a high-energy cutoff of the observed distribution.
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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
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Unveiling the mystery of solar-coronal heating

Physics Today, 2023
Miniature flares recently discovered by probes that have approached the Sun’s surface are helping physicists understand how the Sun’s corona reaches temperatures of millions of kelvin.
Leonardo Di G. Sigalotti, Fidel Cruz
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Solar coronal heating by plasma waves

Journal of Plasma Physics, 2009
AbstractThe solar coronal plasma is maintained at temperatures of millions of degrees, much hotter than the photosphere, which is at a temperature of just 6000 K. In this paper, the plasma particle heating based on the kinetic theory of wave–particle interactions involving kinetic Alfvén waves and lower-hybrid drift modes is presented.
Bingham, R., Shukla, P.K., Eliasson, Bengt, Stenflo, L.   +3 more
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