Results 181 to 190 of about 5,382 (223)

Photovoltaic-Related "Black Swan" Hypothesis for Electric Power System: Phenomenology, Simulations, Experiences, and Prevention. [PDF]

Sensors (Basel)
Sladic S, Zivic E.
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Exo-Geoscience Perspectives Beyond Habitability. [PDF]

Space Sci Rev
Spohn T, Roberge A, Way MJ, Duarte JC, Miozzi F, Baumeister P, Byrne P, Lineweaver CH.   +7 more
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Magnetic star-planet interaction in the young exoplanet system DS Tucanae Ab

Santos Ld, Owen J, Duvvuri G, Loyd ROP, Vidotto A, Presa A, Bourrier V, King G, Airapetian V, Ehrenreich D, France K, Lendl M, Lothringer J, Nielsen L.   +13 more
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Polarimetric calibration of the Tunable Magnetograph for the Sunrise III mission

Campos-Jara A, Álvarez-Herrero A, García-Parejo P, Garranzo-García D, Guerrero PS, Bailén FJ, Feller A, Gandorfer A, Orozco-Suárez D, Iniesta JCdT.   +9 more
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Evolution of the Magnetic Field Distribution of Solar Active Regions

, 2017
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Computational modeling of magnetic fields in solar active regions

Space Science Reviews, 1989
The magnetic field plays an important role in various solar activities. This paper reviews techniques for computational modeling of magnetic fields in solar active regions. The input data are photospheric magnetic fields supplied by magnetograph observations.
Takashi Sakurai
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Twist of magnetic fields in solar active regions

Journal of Astrophysics and Astronomy, 2000
Extended abstractIn the solar atmosphere, the magnetic and current helicity have played an important role in the study of twisted magnetic field. Current helicity parameterh∥=B∥· (∇ ×B)∥and force free factorcan be used to analyze the distribution of twisted field (current helicity) in the photosphere (Seehafer 1990; Pevtsovet al.1995; Bao &amp ...
Hongqi Zhang, Lirong Tian, Shudong Bao, Mei Zhang   +3 more
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Investigation of magnetic fields in solar active regions

Astronomy Reports, 2000
The magnetic-field structure in solar active regions outside spots is studied. The line-of-sight fields were measured using the new Crimean digital magnetograph in three spectral lines—Fe I 5253 A, Fe II 5234 A, and Ti I 5193 A. Observations in the Fe II 5234 A line indicate systematically higher field strengths than those in the Fe I 5253 A line.
S. I. Gopasyuk, O. S. Gopasyuk, I. P. Zalesov, D. V. Karkach, V. V. Svistel’nikov   +4 more
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