Zobrazeno 1 - 8
of 8
pro vyhledávání: '"M. I. Pishkalo"'
Autor:
M. I. Pishkalo, U. M. Leiko
Publikováno v:
Odessa Astronomical Publications, Vol 28, Iss 2, Pp 272-273 (2016)
It is known that polar magnetic field of the Sun changes its sign at the maximum of solar cycle. These changes were called as polar field reversals. We investigated dynamics of high-latitude solar magnetic fields separately in northern and southern h
Externí odkaz:
https://doaj.org/article/4b0be6b9648643e79dd837e03d272e19
Autor:
I. E. Vasiljeva, M. I. Pishkalo
Publikováno v:
Kinematika i fizika nebesnyh tel (Online). 37:60-78
The paper provides a short historical overview of sunspot observations from their discovery until the present. The review goes beyond collecting all known historical information about the study of sunspots but highlights the research of five scientis
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_dedup___::0a9a4e030a1e56bdb830ac0574b9ec4f
https://doi.org/10.15407/kfnt2021.04.060
https://doi.org/10.15407/kfnt2021.04.060
Autor:
M. I. Pishkalo
Publikováno v:
Kinematics and Physics of Celestial Bodies. 37:27-32
Solar activity changes with about 11-year periodicity, two 11-year cycles form a complete 22-year magnetic cycle of the Sun. Solar cycle 25 has recently begun, and it is important to know in advance what and when it will be at its maximum. The paper
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::3c5f290da7bce22db16b2e3807e89fe1
https://doi.org/10.3103/s0884591321010050
https://doi.org/10.3103/s0884591321010050
Autor:
M. I. Pishkalo, U. M. Leiko
Publikováno v:
Kinematics and Physics of Celestial Bodies. 32:78-85
Data on the value and sign of the circumpolar magnetic field of the Sun at a maximum of its activity in cycle 24 have been analyzed. The data were obtained from observations at the Wilcox Solar Observatory and from synoptic maps of the magnetic field
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::c7e0607459b4bac03a9489f8fead627f
https://doi.org/10.3103/s0884591316020069
https://doi.org/10.3103/s0884591316020069
Autor:
M. I. Pishkalo
Publikováno v:
Kinematics and Physics of Celestial Bodies. 29:37-43
Correlations are investigated between the pattern of solar activity described by the smoothed monthly relative sunspot numbers (Wolf numbers) near the minimum of a solar cycle and the cycle amplitude. The closest correlation is found between the ampl
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::bdb69eea6d86dee493f9cbbbf87f60e4
https://doi.org/10.3103/s0884591313010054
https://doi.org/10.3103/s0884591313010054
Autor:
U. M. Leiko, M. I. Pishkalo
Publikováno v:
Odessa Astronomical Publications; Том 28, № 2 (2015); 272-273
Odessa Astronomical Publications, Vol 28, Iss 2, Pp 272-273 (2016)
Odessa Astronomical Publications, Vol 28, Iss 2, Pp 272-273 (2016)
It is known that polar magnetic field of the Sun changes its sign at the maximum of solar cycle. These changes were called as polar field reversals. We investigated dynamics of high-latitude solar magnetic fields separately in northern and southern h
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_dedup___::7dc82e7e70c80adf1330b0ecf0231a18
http://oap.onu.edu.ua/article/view/71123
http://oap.onu.edu.ua/article/view/71123
Autor:
M. I. Pishkalo
Publikováno v:
Kinematics and Physics of Celestial Bodies. 24:242-247
The correlation between various parameters of solar cycles 1–23 is investigated. The derived regressions are used to make predictions of solar cycles 24 and 25. It is expected that solar cycle 24 will reach its maximum amplitude of 110.2 ± 33.4 in
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::98f2c2e99b43c68d266b21a835c76428
https://doi.org/10.3103/s0884591308050036
https://doi.org/10.3103/s0884591308050036
Autor:
M. I. Pishkalo
Publikováno v:
Astronomische Nachrichten. 315:391-397
Hα profiles of chromospheric spicules computed for a variety of rotational behavior are compared with an observed profile, which was derived by averaging 11 Hα profiles taken near times of maximum spicule intensity. If turbulent velocity is small o
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::0f34c4d4835131c9d763f107af809746
https://doi.org/10.1002/asna.2103150508
https://doi.org/10.1002/asna.2103150508