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Start Over Subject sunspot groups

1. A study of activity in interacting sunspot groups

Creator:
Schmieder, B., van Driel-Gesztelyi, L., and Hénoux, J.-C.
Format:
bez média and svazek
Type:
model:article and TEXT
Subject:
heliophysics and sunspot groups
Language:
Czech
Description:
Two interacting active regions of different ages have been studied over two days using white light and Hα observations as well as magnetograma. Different series of homologous flares and the formation of a filament in tbe region were analysed and an interpretation of these events is proposed.
Rights:
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2. Development of sunspot groups related to the solar differential rotation during the early period of a new solar cycle

Creator:
Deszö, L. and Kovács, A.
Format:
bez média and svazek
Type:
model:article and TEXT
Subject:
heliophysics, sunspot groups, and solar differential rotation
Language:
Czech
Description:
The 'Debrecen Photoheliographlc Results’ beginnlng with the year 1977 gives various kinds of posltion and area data of sunspots dally for a single moment, includlng all spot groups vlsible at least on two days.In addition, thls catalogue also indicates tlie magnetlc spot polarities and for each sunspot, wherever reasonable, a special number as a mark of Identification. By these means special features of the spot activity of 1977 have been studied. So, diverse spot distributions and the principal spot motions within the groups, as well as the local solar rotatlon in several regions of spot groups by means of tracers of spot positions have been determlned. The most important characteristlcs found are presented.
Rights:
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3. Does the local dynamo act in sunspot groups?

Creator:
Bumba, V.
Format:
bez média and svazek
Type:
model:article and TEXT
Subject:
astronomy, sunspot groups, and local magnetic field topology
Language:
Czech
Description:
We summarize our previous results concerning the local magnetic field formation, showing that its sunspot groups developing to reach higher typec C, D, E etc. continue their magnetic evolution during the period of new magnetic flux addition immediately after the first magnetically bipolar balanced stage. It is probably a magnetohydrodynamical process of magnetic field strenthening oř a new magnetic flux generation. It is dosely related to a specific singularity in the local magnetic field topology at the inner field boundary not far from the centre of the group, where the gulf of one polarity is compressed inbetween the boundary curvature of the field of opposite polarity and where large radial velocities can be observed. This is the region, where new peaks of both the leading and the following polarities in a speciál orthogonal relation of the new to the old tubes of lines of force develop, where the greatest field gradiente are formed. The flare frequencies and their importances correlate well with the degree of complexity of magnetic field topology in this situation. The important role of the photosphere in all these processes is underlined.
Rights:
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4. Proper motions of the NOAA/USAF 3885 and 3886 regions (1 - 11 September 1982)

Creator:
Csepura, G. and Nagy, I.
Format:
bez média and svazek
Type:
model:article and TEXT
Subject:
sunspot groups, NOAA 3885, and NOAA 3886
Language:
Czech
Description:
In this article we present study of proper motions of the flare active reglons NOAA/USAF 3885 and NOAA/USAF 3886. The 30 flare of 3 - 4 September 1982 (NOAA 3886) appeared to have a close relation to the relatlve motlon of unconnected sunspot pairs of opposite polarity, During the regressive stage of region NOAA 3885 a considerable rotation was observed In the main leader umbra.
Rights:
http://creativecommons.org/publicdomain/mark/1.0/ and policy:public

5. Some evolutionary aspects of solar acrive regions

Creator:
M. J.
Format:
bez média and svazek
Type:
model:article and TEXT
Subject:
heliophysics, large active regions, and sunspot groups
Language:
Czech
Description:
The appearance of isolated sunspot groups as well as clustering in large active regions depends upon a complex dynamo process. Evidence of this dynamo process may be deduced from three different outstanding studies. a) The emergence of new fluxes (spots or flares) is preceded by local cyclonic motions, observed at the photospheric level. In regions of weak magnetic fields ; for example polarity inversion lines, gaps between magnetic "hills" or borders of the facula. This velocity structure is a response with a short scale in time and space to local subphotospheric perturbation and thus creates currents and new magnetic flux. b) Magnetic tracers such as long lived H filaments and sunspots, show that the regions of emergence of new flux (family of sunspot groups, eruptive sites or parasitic polaritics) are related to the existence of limited areas rotating rigidly. These "pivot points" which do not follow dlffcrential rotation, could be anchored more deeply than the active centers themselves. c) A large scale circulation, tied to the global rotation, reflects the motions of the underlying fluid (frozen field). Recent results show the existence of azimuthal rolls which transport upward the deep magnetic field. They move slowly toward the poles, and they appear to govern the cyclicity and to modulate the observed solar rotation. These observational results need to be considered to understand the production and the development of active regions.
Rights:
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6. Sunspot groups as tracers of radial differential rotation

Creator:
Gesztelyi, L. and Pap, J.
Format:
bez média and svazek
Type:
model:article and TEXT
Subject:
heliophysics, sunspot groups, and rotation
Language:
Czech
Description:
Measurements of the proper niotlons of young blpolar sunspot groups show that these groups rotate faster than the surroundlng photosphere. The results of the tlme series analysis carrled out on the Irradiance records of the SMM/ACRIM radiometer and on the projected areas of the young, active sunspot groups showed a period near U days In 1980, the year of the solar maximum. The main period in the projected areas of the old sunspot groups was 28 days, which corresponded to the mean photospherlc rotatlon. The faster proper motlon of the young sunspot groups as well as the 24 days periodicity of the young active spot areas might indicate that the young sunspots are connected to the deeper regione of the Sun which rotate faster than the photosphere. Thus, the sunspot groups in the early stage of their life would be an indlcator of rotation of the deeper layers of the Sun.
Rights:
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7. The outline of the theory of distribution and occurence of sunspots on the solar disc

Creator:
Kopecký, Miloslav
Format:
bez média and svazek
Type:
model:article and TEXT
Subject:
astrophysics, sunspot groups, and solar disc
Language:
Czech
Description:
(Rezjume) Cel'ju nastojaščego truda javljajetsja obobščenije svedenij iz teorii raspredelenija i pojavlenija solnečnych pjaten na diske Solnca. V etoj svojej rabote avtor ischodit kak iz rjada trudov drugich avtorov, tak i iz svoich sobstvennych trudov, pomeščennych v raznych žurnalach, dopolnjaja eti trudy nekotorymi novymi svedenijami. Eta rabota javljajetsja sozdat' obobščenoje predstavlenije o teorii raspredelenija i pojavlenija solnečnich pjaten na diske Solnca. Nastojaščaja rabota, odnako ne zanimajetsja osveščenijem voprosov etoj teorii s obščej točki zrenija, tak kak boleje obščaja teorija ne byla do sich por v soveršenstve razrabotana. Eta teorija osnovljajetsja na opredelinii uproščennych predpoloženij, iz kotorych samymi prostymi javljajutsja sledujuščije: 1) Vse solnečnyje pjatna pojavljajutsja tol'ko na ekvatore, kotoryj vsegda prochodit po seredine diska Solnca, t. e. čto "korolevskij pojas" pojavljenija solnečnych pjaten možno sebe predstavit' v vide cilindra, na ktoryj smotrim v napravlenii normali i jego poverchnosti. 2) V dejstvitel'nosti predpoložim, čto grupy solnečnych pjaten sostavljajutsja iz odnogo pjatna okrugloj formy. Eti predloženija pozvoljajut nam sozdat' vozmožno polnuju osnovnuju teoriju raspredelenija i pojavlenija pjaten, kotoraja neobchodima dlja ocenki rezul'tatov raznych statistik pjaten i iz kotoroj možno ischodit' dlja sozdanija boleje obščej teorii. Nastojaščaja rabota zanimajetsja prežde vsego sledujuščimi voprosami: opredelenijem osnovnych otnošenij i funkcij, umen'šenijem količestva pjaten v napravlenii k kraju solnečnogo diska, količestvom pojavšichsja i isčeznuvšich pjaten na raznych rasstojanijach ot central'nogo meridiana, podsčetom količestva voznikšich grupp na vsem Solnce i srednej prodolžitel'nosti ich žizni i značenijem etich veličin dlja issledovanija periodičnosti solnečnych pjaten.
Rights:
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