Results 11 to 20 of about 4,073 (163)

Measuring the magnetic fields in the chromospheres of low-mass stars. [PDF]

Nat Commun
Cang T, Petit P, Donati JF, Tian H, Fu J, Li H, Bellotti S, Hu X, Ma X, Lopez Ariste A, Xing K, Morin J, Lu H, Zong W.   +13 more
europepmc   +4 more sources

Numerical Experiment on the Influence of Granulation-induced Waves on Solar Chromosphere Heating and Plasma Outflows in a Magnetic Arcade

The Astrophysical Journal
This paper offers a fresh perspective on solar chromosphere heating and plasma outflows, focusing on the contribution of waves generated by solar granulation.
M. Kumar, K. Murawski, B. Kuźma, E. K. J. Kilpua, S. Poedts, R. Erdélyi   +5 more
doaj   +2 more sources

Constraints on Acoustic Wave Energy Fluxes and Radiative Losses in the Solar Chromosphere from Non-LTE Inversions

The Astrophysical Journal
Accurately assessing the balance between acoustic wave energy fluxes and radiative losses is critical for understanding how the solar chromosphere is thermally regulated.
J. M. da Silva Santos, M. Molnar, I. Milić, M. Rempel, K. Reardon, J. de la Cruz Rodríguez   +5 more
doaj   +2 more sources

Moreton waves and EUV waves in the solar atmosphere

地球与行星物理论评, 2023
Solar eruptions, which generate various types of wave phenomena in the solar atmosphere, are sources of space weather perturbations. These waves not only transport a large amount of energy, but also illuminate the properties of the magnetic field and ...
Pengfei Chen
doaj   +1 more source

Review of Fast Solar Jets and Coronal Mass Ejections [PDF]

Iranian Journal of Astronomy and Astrophysics, 2023
The Sun is a magnetically active star. It has a powerful magnetic field that shifts slightly from year to year until it reverses about every eleven years. The sun's magnetic field has many effects, the collection of which is called solar activity such as,
Sima Zeighami, Ehsan Tavabi
doaj   +1 more source

Inferring depth-dependent plasma motions from surface observations using the DeepVel neural network

Journal of Space Weather and Space Climate, 2021
Coverage of plasma motions is limited to the line-of-sight component at the Sun’s surface. Multiple tracking and inversion methods were developed to infer the transverse motions from observational data.
Tremblay Benoit, Cossette Jean-François, Kazachenko Maria D., Charbonneau Paul, Vincent Alain   +4 more
doaj   +1 more source

Subarcsecond Imaging of a Solar Active Region Filament With ALMA and IRIS

Frontiers in Astronomy and Space Sciences, 2022
Quiescent filaments appear as absorption features on the solar disk when observed in chromospheric lines and at continuum wavelengths in the millimeter (mm) range. Active region (AR) filaments are their small-scale, low-altitude analogues, but they could
J. M. da Silva Santos, S. M. White, K. Reardon, G. Cauzzi, S. Gunár, P. Heinzel, J. Leenaarts   +6 more
doaj   +1 more source

An ALMA Observation of Time Variations in Chromospheric Temperature of a Solar Plage Region

Frontiers in Astronomy and Space Sciences, 2022
Nanoflares and the shock formation of magnetohydrodynamic waves in the solar chromosphere have been considered as key physical mechanisms of the heating of the chromosphere and corona.
Masashi Abe, Masashi Abe, Toshifumi Shimizu, Toshifumi Shimizu, Masumi Shimojo, Masumi Shimojo   +5 more
doaj   +1 more source

Incoherent Solar Radio Emission

Frontiers in Astronomy and Space Sciences, 2020
Incoherent solar radio radiation comes from the free-free, gyroresonance, and gyrosynchrotron emission mechanisms. Free-free is primarily produced from Coulomb collisions between thermal electrons and ions.
Alexander Nindos
doaj   +1 more source

SPATIAL AND TEMPORAL VARIATIONS OF K Ca II LINE PROFILE SHAPES IN DIFFERENT STRUCTURES OF THE SOLAR CHROMOSPHERE. II. DETERMINATION TECHNIQUE AND CORRELATION RELATIONSHIPS BETWEEN THE K CA II LINE PARAMETERS FOR K₁ AND K₂ FEATURES

Solar-Terrestrial Physics, 2020
We have studied two regions located at the base of a coronal hole. For the K₁ intensity minima and K₂ peaks, which form between the upper photosphere and the lower chromosphere and in the lower chromosphere respectively, a number of Ca II line parameters
I.P. Turova, S.A. Grigoryeva, O.A. Ozhogina   +2 more
doaj   +1 more source