Results 261 to 270 of about 27,444 (310)

The Amerigo Vespucci as a traveling laboratory for studying the cosmic-ray fluxes at sea level. [PDF]

Sci Rep
Cerasole D, Cuna F, De Palma G, Di Tria R, Di Venere L, Gargano F, Giliberti M, Licciulli F, Liguori A, Loizzo P, Loparco F, Lorusso L, Mazziotta MN, Panzarini G, Pillera R, Serini D.   +15 more
europepmc   +1 more source

Ultrafast Sulfur Redox Dynamics Enabled by a PPy@N-TiO₂ Z-Scheme Heterojunction Photoelectrode for Photo-Assisted Lithium-Sulfur Batteries. [PDF]

Nanomicro Lett
Zhao F, He Y, Li X, Yang K, Chen S, Jiang Y, Wang XS, Song C, Liu X.   +8 more
europepmc   +1 more source

Evolution of the Magnetic Field Distribution of Solar Active Regions

, 2017
openaire   +1 more source

Some of the next articles are maybe not open access.

Related searches:

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
openaire   +1 more source

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
openaire   +1 more source

Twist of magnetic fields in solar active regions

Astronomy Reports, 2002
We study the twist properties of photospheric magnetic fields in solar active regions using magnetographic data on 422 active regions obtained at the Huairou Solar Observing Station in 1988–1997. We calculate the mean twist (force-free field αf) of the active regions and compare it with the mean current-helicity density of these same active regions, h
Hongqi Zhang, Shudong Bao, Kirill M. Kuzanyan   +2 more
openaire   +1 more source

Solar Flare Acceleration of Solar Wind: Influence of Active Region Magnetic Field

Science, 1981
The direction of the photospheric magnetic field at the site of a solar flare is a good predictor of whether the flare will accelerate solar wind plasma. If the field has a southward component, high-speed solar wind plasma is usually observed near the earth about 4 days later. If the field has a northward component, such high-speed solar wind is almost
H, Lundstedt, J M, Wilcox, P H, Scherrer
openaire   +2 more sources

Photographic maps of magnetic fields of solar active regions

Chinese Astronomy, 1979
This paper describes our daily photography of maps of the strong magnetic fields in solar active regions. In one case, the isogauss line at 2000 G in a complex magnetic region is seen to coincide with the optical outline of a sunspot umbra.
null Ding You-ji, null Peng Fang-lin, null Zhong Shu-hua, null Li Bo-shu, null Ye Hui-lian, null Luan Di   +5 more
openaire   +1 more source

Coronal Magnetic Field Structure in Solar Active Regions

PLANETARY RADIO EMISSIONS VII, 2011
We analyzed the structure of the magnetic field in active regions at coronal altitudes, determined using multiwavelength observations of polarized radio emission in the microwave range at the radiotelescope RATAN-600. The observations were compared with the current-free magnetic field extrapolation of the photospheric field.
openaire   +1 more source

Relation between the active region magnetic field and solar flares

Geomagnetism and Aeronomy, 2013
A weak active region (NOAA 11158) appeared on the solar disk near the eastern limb. This region increased rapidly and, having reached the magnetic flux higher than 1022 Mx, produced an X-class flare. Only weak field variations at individual points were observed during the flare.
A. I. Podgorny, I. M. Podgorny, N. S. Meshalkina   +2 more
openaire   +1 more source