Solar and Solar-type Stars Atmosphere's Activity at 11-year and Quasi-biennial Time Scales

Бруевич, Е. А.; Kononovich, E. V.

doi:10.48550/arxiv.1102.3976

Cited by 3 publications

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“…Table 1 and Table 2 present the results of our calculation of the periods of variations of chromospheric radiation of the stars (Bruevich & Kononovich 2011). The method of fast Fourier transform was used to determine periods of the cyclicity of stars.…”

Section: "Hk-project" Of Mount Wilson Observatorymentioning

confidence: 99%

Cycles of the magnetic activity of the Sun and solar-type stars and simulation of their fluxes

Bruevich,

Rozgacheva

2012

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The application of the Wavelet analysis and Fourier analysis to the dataset of variations of radiation fluxes of solar-like stars and the Sun is examined. In case of the Sun the wavelet-analysis helped us to see a set of values of periods of cycles besides "11-year" cycle: the long-duration cycles of 22-year, 40-50 year and 100-120 year and short-duration cycles of 2-3,5 years and 1,3-year. We present a method of the chromospheric flux simulation using the 13 late-type stars, which have well-determined cyclic flux variations similar to the 11-year solar activity cycle. Our flux prediction is based on the chromospheric calcium emission time series measurements from the Mount Wilson Observatory and comparable solar dataset. We show that solar three -component modeling well explains the stellar chromospheric observations.

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Section: "Hk-project" Of Mount Wilson Observatorymentioning

confidence: 99%

Cycles of the magnetic activity of the Sun and solar-type stars and simulation of their fluxes

Bruevich,

Rozgacheva

2012

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“…The quasi-biennial fluxes variation are widely spread phenomenon for star's (not only for Sun) observations too. The periods of star's fluxes variations on the quasi-biennial time scale vary from 2,2 to 3,5 years [7].…”

Section: Introductionmentioning

confidence: 99%

Solar Activity Indices in 21, 22 and 23 Cycles

Bruevich,

Yakunina

2011

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The monthly average values of the main solar activity indices such as Wolf numbers (W), 10,7 cm radio flux F 10,7 , 0,1-0,8 nm background, total solar irradiance and Mg II UV-index (280 nm core to wing ratio) were studied for 23 activity cycle. The correlation coefficients of linear regression for main solar activity indices versus F 10,7 were analyzed for every year of 23 activity cycle. All the correlation coefficients for 23 activity cycle have the minimum values in 2001. We also analyzed the connection between monthly average values of the most popular indices W and F 10,7 for 21, 22 and 23 solar activity cycles. The values of every year linear regression correlation coefficients for W versus F 10,7 show the cyclic variations with period closed to half path of so-called 11-year period of solar activity.KEYWORDS: Sun, solar activity indices, monthly average values variations, correlation coefficients of linear regression for main solar activity indices

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“…The αΩ -dynamo theory which is based on the hypothesis about the generation of the magnetic field due to the differential rotation of the Sun in the turbulent convective shell can describe the main features of solar magnetic activity [5,6]. Solar cycle models based on what is now called the Babcock-Leighton mechanism: 1) generation of toroidal field from the poloidal field due to the differential rotation of the convective shell (Ω-effect); 2) generation of poloidal field from bipolar magnetic regions of toroidal field due to the differential rotation and the turbulent viscosity (α-effect).…”

Section: Introductionmentioning

confidence: 99%

“…The periods of cycles of activity are given according to the calculations of cyclic periodicities of HK-project stars by the authors of this work with help of Fourier analysis of light curves of stars [5]. We also used the earlier definition of "11-year" periods by the authors of HK-project (T HK 11 ) [11] for a sample of 52 stars and the Sun.…”

Section: Introductionmentioning

confidence: 99%

Can Rossby waves explain the cyclic magnetic activity of the Sun and solar-type stars?

Bruevich,

Rozgacheva

2013

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Magnetic activity is a global property of the Sun; the complex processes of solar activity are connected with the solar magnetic fields. For solar-type stars and the Sun magnetic activity depends on the physical parameters of the star. In this article we study the relationships between the duration of activity cycle and effective temperature for solar-type stars and the Sun. We've tried to explain these relationships due to the existence of layer of laminar convection near the bottom of the convective zone of the star. In this layer the Rossby waves are formed. They generate the primary poloidal magnetic field, which is the source of energy of the complex phenomena of magnetic activity.

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Solar and Solar-type Stars Atmosphere's Activity at 11-year and Quasi-biennial Time Scales

Cited by 3 publications

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Cycles of the magnetic activity of the Sun and solar-type stars and simulation of their fluxes

Cycles of the magnetic activity of the Sun and solar-type stars and simulation of their fluxes

Solar Activity Indices in 21, 22 and 23 Cycles

Can Rossby waves explain the cyclic magnetic activity of the Sun and solar-type stars?

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