Results 21 to 30 of about 5,676 (305)

The dynamics of eruptive prominences

, 2014
This chapter discusses the dynamical properties of eruptive prominences in relation to coronal mass ejections (CMEs). The fact that eruptive prominences are a part of CMEs is emphasized in terms of their physical association and kinematics. The continued
Gopalswamy, Nat
core   +1 more source

Hα Doppler shifts in a tornado in the solar corona [PDF]

, 2016
Context. High resolution movies in 193 Å from the Atmospheric Imaging Assembly (AIA) on the Solar Dynamic Observatory (SDO) show apparent rotation in the leg of a prominence observed during a coordinated campaign. Such structures are commonly referred to
Labrosse, N., Levens, P.J., Mein, N., Mein, P., Ofman, L., Schmieder, B.   +5 more
core   +4 more sources

Statistical Analyses of Solar Prominences and Active Region Features in 304 Å Filtergrams Detected via Deep Learning

The Astrophysical Journal Supplement Series
Solar active regions (ARs) are areas on the Sun with very strong magnetic fields where various activities take place. Prominences are one of the typical solar features in the solar atmosphere, whose eruptions often lead to solar flares and coronal mass ...
T. Zhang, Q. Hao, P. F. Chen
doaj   +1 more source

Data-constrained Magnetohydrodynamic Simulation of an Intermediate Solar Filament Eruption

The Astrophysical Journal, 2023
Solar eruptive activities could occur in weak magnetic field environments and over large spatial scales, which are especially relevant to eruptions involving intermediate or quiescent solar filaments.
Yang Guo, Jinhan Guo, Yiwei Ni, M. D. Ding, P. F. Chen, Chun Xia, Rony Keppens, Kai E. Yang   +7 more
doaj   +1 more source

Physics of Solar Prominences: II - Magnetic Structure and Dynamics

, 2010
Observations and models of solar prominences are reviewed. We focus on non-eruptive prominences, and describe recent progress in four areas of prominence research: (1) magnetic structure deduced from observations and models, (2) the dynamics of ...
A. Canou, A. Hood, A. López Ariste, A. López Ariste, A. López Ariste, A. López Ariste, A. López Ariste, A.A. Ballegooijen van, A.A. Ballegooijen van, A.A. Ballegooijen van, A.A. Ballegooijen van, A.A. Ballegooijen van, A.A. Pevtsov, A.A. Pevtsov, A.H. McAllister, A.I. Poland, A.J. Díaz, A.J. Díaz, A.J. Díaz, A.R. Winebarger, A.R. Yeates, A.R. Yeates, A.R. Yeates, A.R. Yeates, A.W. Hood, B. Pontieu De, B. Rekowski Von, B. Schmieder, B. Schmieder, B. Schmieder, B. Schmieder, B. Schmieder, B. Schmieder, B. Schmieder, B.C. Low, B.C. Low, B.C. Low, B.C. Low, B.T. Welsch, B.W. Hindman, B.W. Lites, B.W. Lites, C. Foullon, C. Mercier, C. Zwaan, C.-H. An, C.J. Schrijver, C.L. Hyder, C.M. Korendyke, C.R. DeVore, C.R. DeVore, D. Banerjee, D. H. Mackay, D.A.N. Müller, D.A.N. Müller, D.C. Kendall, D.H. Mackay, D.H. Mackay, D.H. Mackay, D.H. Mackay, D.H. Mackay, D.H. Mackay, D.H. Mackay, D.H. Mackay, D.H. Mackay, D.H. Mackay, D.H. Mackay, D.M. Rust, D.M. Rust, D.M. Rust, E. Tandberg-Hanssen, E. Wiehr, E.E. Benevolenskaya, E.R. Priest, E.R. Priest, F. Moreno-Insertis, F. Paletou, F. Paletou, F. Tang, G. Aulanier, G. Aulanier, G. Aulanier, G. Aulanier, G. Aulanier, G. Aulanier, G. Aulanier, G. Aulanier, G. Aulanier, G. Kilper, G. Pouget, G. Roumeliotis, G.W. Pneuman, H. Lin, H. Pecseli, H. Wang, H.E. Ramsey, H.P. Furth, H.P. Jones, H.R. Gilbert, H.R. Gilbert, H.R. Gilbert, H.W. Babcock, I. Arregui, J. Chae, J. Chae, J. Chae, J. Chae, J. Chae, J. Chae, J. Chae, J. Dudik, J. Jing, J. Jing, J. Kubota, J. Kuijpers, J. L. Ballester, J. T. Karpen, J. Terradas, J. Terradas, J. Trujillo Bueno, J.-L. Leroy, J.-L. Leroy, J.-L. Leroy, J.-M. Malherbe, J.-M. Malherbe, J.A. Klimchuk, J.B. Zirker, J.B. Zirker, J.B. Zirker, J.B. Zirker, J.B. Zirker, J.E. Leake, J.T. Karpen, J.T. Karpen, J.T. Karpen, J.T. Karpen, J.T. Karpen, J.V. Hollweg, K. Galsgaard, K. Galsgaard, K. Saito, K. Saito, K.L. Harvey, K.O. Kiepenheuer, K.S. Balasubramaniam, L. d’Azambuja, L. Léger, L. Ofman, M. Aschwanden, M. Bianda, M. Carbonell, M. Collados, M. Goossens, M. Goossens, M. Kuperus, M. Kuperus, M. Minarovjech, M. Ruderman, M.G. Bobra, M.J. Martres, M.J. Murray, M.L. Khodachenko, M.L. Khodachenko, N. Labrosse, O. Engvold, O. Engvold, O. Engvold, O. Engvold, O. Engvold, O. Engvold, P. Ambrož, P. Forteza, P. Forteza, P. Foukal, P. Foukal, P. Heinzel, P. Heinzel, P. Heinzel, P. Heinzel, P. Heinzel, P. Schwartz, P.A. Sturrock, P.C. Martens, P.N. Bernasconi, P.S. Joarder, P.S. McIntosh, R. Casini, R. Casini, R. Kippenhahn, R. Lionello, R. Molowny-Horas, R. Oliver, R. Oliver, R. Oliver, R. Ramelli, R. Soler, R. Soler, R.B. Dahlburg, R.R. McMath, S. Blanco, S. Eto, S. Gunár, S. Gunár, S. Patsourakos, S. Rondi, S. Régnier, S. Régnier, S. Régnier, S. Régnier, S. Régnier, S. Serio, S.B. Pikel’ner, S.E. Gibson, S.F. Martin, S.F. Martin, S.F. Martin, S.F. Martin, S.F. Martin, S.F. Martin, S.F. Martin, S.F. Martin, S.H.B. Livi, S.K. Antiochos, S.K. Antiochos, S.K. Antiochos, S.K. Antiochos, T. Hirayama, T. Magara, T. Magara, T. Roudier, T. Sakurai, T. Tsubaki, T. Yokoyama, T.A. Kucera, T.A. Kucera, T.E. Berger, T.J. Okamoto, T.J. Okamoto, T.J. Okamoto, T.J. Okamoto, U. Anzer, V. Archontis, V. Archontis, V. Archontis, V. Bommier, V. Gaizauskas, V. Gaizauskas, V. Gaizauskas, V. Gaizauskas, V. Gaizauskas, V. Gaizauskas, V.C.A. Ferraro, W. Manchester IV, W.T. Thompson, Y. Deng, Y. Deng, Y. Fan, Y. Lin, Y. Lin, Y. Lin, Y. Lin, Y. Lin, Y. Lin, Y. Liu, Y. Mok, Y. Su, Y.-H. Fan, Y.-H. Fan, Y.-M. Wang, Y.-M. Wang, Y.-M. Wang, Y.-M. Wang, Y.E. Litvinenko, Y.E. Litvinenko, Y.E. Litvinenko, Y.E. Litvinenko, Y.H. Fan, Z. Mouradian, Z. Ning, Z. Yi, Z. Yi   +280 more
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Diagnostics of Coronal Magnetic Fields Through the Hanle Effect in UV and IR Lines [PDF]

, 2016
The plasma thermodynamics in the solar upper atmosphere, particularly in the corona, are dominated by the magnetic field, which controls the flow and dissipation of energy.
Fineschi, S., Gibson, S., Raouafi, N. E., Riley, P., Solanki, S. K.   +4 more
core   +2 more sources

Cu‐Based MOF/TiO2 Composite Nanomaterials for Photocatalytic Hydrogen Generation and the Role of Copper

Advanced Functional Materials, EarlyView.
HKUST‐1/TiO2 composite materials show a very high photocatalytic hydrogen evolution rate which increases as a function of the irradiation time until reaching a plateau and even surpasses the performance of the 1%Pt/TiO2 material after three photocatalytic cycles.
Alisha Khan, Marie Le Pivert, Alireza Ranjbari, Diana Dragoe, Daniel Bahena‐Uribe, Christophe Colbeau‐Justin, Christian Herrero, Dorota Rutkowska‐Zbik, Johnny Deschamps, Hynd Remita   +9 more
wiley   +1 more source

Solar Prominence Diagnostics [PDF]

International Astronomical Union Colloquium, 1998
AbstractThis paper reviews the diagnostic techniques currently used to establish estimates of the physical properties of prominences. Most often the fine structure of prominences cannot be resolved. Because of this and the complex structures and the varied forms of prominences, it is difficult to establish definitive values for temperature, density ...
openaire   +1 more source

Copper‐based Materials for Photo and Electrocatalytic Process: Advancing Renewable Energy and Environmental Applications

Advanced Functional Materials, EarlyView.
Cu‐based catalysts as a cornerstone in advancing sustainable energy technologies are fully reviewed in this manuscript, highlighting their potential in photo‐ and electrocatalysis. It includes metallic copper, copper oxides, copper sulfides, copper halide perovskites, copper‐based metal–organic frameworks (MOFs), and covalent organic frameworks (COFs),
Jéssica C. de Almeida, Yanjie Wang, Thais A. Rodrigues, Paulo H. H. Nunes, Vagner R. de Mendonça, Paulo H. E. Falsetti, Leticia V. Savazi, Tao He, Alexandra V. Bardakova, Aida V. Rudakova, Jie Tian, Alexei V. Emeline, Osmando F. Lopes, Antonio Otavio T. Patrocínio, Jia Hong Pan, Caue Ribeiro, Detlef W. Bahnemann   +16 more
wiley   +1 more source

On the structure and evolution of a polar crown prominence/filament system

, 2014
Polar crown prominences are made of chromospheric plasma partially circling the Suns poles between 60 and 70 degree latitude. We aim to diagnose the 3D dynamics of a polar crown prominence using high cadence EUV images from the Solar Dynamics Observatory
A.A. van Ballegooijen, A.M. Vásquez, B. Schmieder, B. Schmieder, B.C. Low, B.C. Low, C.R. DeVore, D.F. Webb, D.H. Mackay, D.H. Mackay, D.H. Mackay, D.H. Mackay, D.J. Schmit, D.J. Schmit, E.R. Priest, G. Aulanier, G. Aulanier, G. Del Zanna, H. Wang, H.R. Gilbert, H.S. Hudson, J. Chae, J. Chae, J. Dudík, J. Schou, J.B. Zirker, J.L. Leroy, J.R. Lemen, J.W. Harvey, L. Li, L.A. Rachmeler, M. Kuperus, M. Kuperus, M. Minarovjech, N. Labrosse, N.K. Panesar, P. Heinzel, P. Heinzel, P. Heinzel, P.C. Martens, P.S. McIntosh, R.A. Howard, R.B. Dahlburg, S. Parenti, S. Régnier, S.E. Gibson, S.E. Gibson, S.E. Gibson, S.F. Martin, S.F. Martin, S.K. Antiochos, S.R. Habbal, T. Berger, T. Hirayama, T.A. Kucera, T.A. Kucera, T.E. Berger, T.E. Berger, U. Anzer, U. Anzer, U. Ba̧k-Stȩślicka, V. Gaizauskas, Y. Lin, Y. Su, Y.M. Wang   +64 more
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