Zobrazeno 1 - 10
of 22
pro vyhledávání: '"E. I. Mogilevsky"'
Autor:
E. I. Mogilevsky, T. E. Val’chuk
Publikováno v:
Geomagnetism and Aeronomy. 49:551-556
The discreteness of the time series of the solar-related geophysical phenomena is justified. The balance of the formation and decomposition (neglecting diffusion) of fractal elements during the evolution of the equilibrium systems as applied to the h
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::c7d077a754667105efb86b7c7d8ae029
https://doi.org/10.1134/s0016793209050016
https://doi.org/10.1134/s0016793209050016
Publikováno v:
Geomagnetism and Aeronomy. 47:803-809
Based on the Nimbus-7 (1978–1992) data and the parameters of solar activity (Wolf numbers W, solar radioemission F 10.7) and the ionosphere (f 2 index of the critical frequency of the ionospheric F 2 layer normalized to noon), the fractal dimension
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::e5d1af90c32fea53db312a4bd2c754f0
https://doi.org/10.1134/s001679320706014x
https://doi.org/10.1134/s001679320706014x
Autor:
E. I. Mogilevsky, N. S. Shilova
Publikováno v:
Geomagnetism and Aeronomy. 46:303-308
Solar flare films obtained on the TRACE spacecraft with a resolution of 1″ in the 160-nm (CIV) band with a frame separation of 2 s are examined. It has been indicated that the flare scenario is determined by the dynamics of numerous structures of a
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::8582bc9b0388a0dec4b5009b5568c8e5
https://doi.org/10.1134/s0016793206030030
https://doi.org/10.1134/s0016793206030030
Publikováno v:
Geomagnetism and Aeronomy. 46:139-145
Using the data of 1960–1999 on solar magnetic fields on the source surface and the Higuchi method, the fractal dimension of changes in the solar magnetic field energy at various heliolatitudes and in different time intervals is analyzed. The fracta
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::bf93d7ab0dadb535d8a6466afe467f23
https://doi.org/10.1134/s0016793206020010
https://doi.org/10.1134/s0016793206020010
Publikováno v:
The Astrophysical Journal. 567:1225-1233
Based on Yohkoh/SXT, SOHO/EIT images and movies, as well as on Hα, He I 10830 A heliograms and other relevant data, we analyze an event of 1999 December 28, which is interesting in at least two aspects. (1) A major horseshoe-shaped Hα filament appe
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::453bee49644a027826afaa9893347c0b
https://doi.org/10.1086/338584
https://doi.org/10.1086/338584
Autor:
E. I. Mogilevsky
Publikováno v:
Astronomical & Astrophysical Transactions. 17:337-340
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::59d97847ca5412b0b8eb091867329a0c
https://doi.org/10.1080/10556799808232100
https://doi.org/10.1080/10556799808232100
Publikováno v:
International Astronomical Union Colloquium. 167:393-396
SOHO and YOHKOH images, as well as Hα filtergrams and magnetograms from IZMIRAN have been used to analyze the evolution of the related solar phenomena – filament, active region, and accompanying pair of coronal holes – during six solar rotations
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::509310838275212cfaf4843d539bfad2
https://doi.org/10.1017/s0252921100047989
https://doi.org/10.1017/s0252921100047989
Publikováno v:
Solar Physics. 176:107-121
This paper is aimed at establishing the relationship between the large-scale magnetic fields (LSMF), coronal holes (CH), and active regions (AR) in the Sun. The LSMF structure was analyzed by calculating the vector photospheric magnetic field under a
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::5a2e912647ed3fc17223d2185c45bd1d
https://doi.org/10.1023/a:1004908014970
https://doi.org/10.1023/a:1004908014970
Autor:
E. I. Mogilevsky
Publikováno v:
Stellar Turbulence ISBN: 9783540097372
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::cc81ea9892f3ec4029d07d986f5afe98
https://doi.org/10.1007/3-540-09737-6_42
https://doi.org/10.1007/3-540-09737-6_42
Autor:
K. I. Nikolskaya, E. I. Mogilevsky
Publikováno v:
Proceedings of the International Astronomical Union. 2004:129-130
Solar magnetic field polarity reversal (SMFPR) happens every 10-11 years. However untill now there is no clear understanding in what way this process is carried out. Results represented here are a by-product of the coronal hole study based on taken f
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::30ab30873817d5fa81f33d5126b2e480
https://doi.org/10.1017/s1743921304005381
https://doi.org/10.1017/s1743921304005381