Multiple cycles of magnetic activity in the Sun and Sun-like stars and their evolution
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摘要
The wavelet transform method for high-quality time-frequency analysis is applied to sets of observations of relative sunspot numbers and stellar chromosphere fluxes of 10 Sun-like stars.Wavelet analysis of solar data shows that in a certain interval of time there are several cycles of activity with periods of duration which vary considerably from each other:from quasi-biennial cycles to 100-yr cycles.Cyclic activity was detected in almost all Sun-like stars that we examined,even those that previously were not considered as stars with cyclic activity according to analysis using a Scargle periodogram.The durations of solar and stellar cycles significantly change during the observation period.
The wavelet transform method for high-quality time-frequency analysis is applied to sets of observations of relative sunspot numbers and stellar chromosphere fluxes of 10 Sun-like stars.Wavelet analysis of solar data shows that in a certain interval of time there are several cycles of activity with periods of duration which vary considerably from each other:from quasi-biennial cycles to 100-yr cycles.Cyclic activity was detected in almost all Sun-like stars that we examined,even those that previously were not considered as stars with cyclic activity according to analysis using a Scargle periodogram.The durations of solar and stellar cycles significantly change during the observation period.
The wavelet transform method for high-quality time-frequency analysis is applied to sets of observations of relative sunspot numbers and stellar chromosphere fluxes of 10 Sun-like stars.Wavelet analysis of solar data shows that in a certain interval of time there are several cycles of activity with periods of duration which vary considerably from each other:from quasi-biennial cycles to 100-yr cycles.Cyclic activity was detected in almost all Sun-like stars that we examined,even those that previously were not considered as stars with cyclic activity according to analysis using a Scargle periodogram.The durations of solar and stellar cycles significantly change during the observation period.
引文
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Zhao,J.-K.,Oswalt,T.D.,Chen,Y.-Q.,et al.2015,RAA(Research in Astronomy and Astrophysics),15,1282
Bludova,N.G.,Obridko,V.N.,&Badalyan,O.G.2014,Sol.Phys.,289,1013
Bruevich,E.A.,Katsova,M.M.,&Sokolov,D.D.2001,Astronomy Reports,45,718
Bruevich,E.A.,&Alekseev,I.Y.2007,Astrophysics,50,187
Bruevich,E.A.,&Kononovich,E.V.2011,Moscow University Physics Bulletin,66,72
Bruevich,E.A.,Bruevich,V.V.,&Yakunina,G.V.2014,Sun and Geosphere,8,91
Bruevich,E.A.,&Yakunina,G.V.2015,Moscow University Physics Bulletin,70,282
Daubechies,I.1990,IEEE Transactions on Information Theory,36,961
Frick,P.,Baliunas,S.L.,Galyagin,D.,Sokoloff,D.,&Soon,W.1997,Ap J,483,426
Garca,R.A.,Mathur,S.,Salabert,D.,et al.2010,Science,329,1032
Kollth,Z.,&Ol′ah,K.2009,A&A,501,695
Lockwood,G.W.,Skiff,B.A.,Henry,G.W.,et al.2007,Ap JS,171,260
Metcalfe,T.S.,Monteiro,M.J.P.F.G.,Thompson,M.J.,et al.2010,Ap J,723,1583
Morgenthaler,A.,Petit,P.,Morin,J.,et al.2011,Astronomische Nachrichten,332,866
Nagovitsyn,Y.A.,Tlatov,A.G.,&Nagovitsyna,E.Y.2016,Astronomy Reports,60,831
Noyes,R.W.,Hartmann,L.W.,Baliunas,S.L.,Duncan,D.K.,&Vaughan,A.H.1984,Ap J,279,763
Olah,K.,Kollath,Z.,Granzer,T.,et al.2009,A&A,501,703Scargle,J.D.1982,Ap J,263,835
Shimanovskaya,E.,Bruevich,V.,&Bruevich,E.2016,RAA(Research in Astronomy and Astrophysics),16,148
Svalgaard,L.,Lockwood,M.,&Beer,J.2011,Longterm reconstruction of Solar and Solar Wind Parameters,http://www.leif.org/research/Svalgaard ISSI Proposal Base.pdf.
Vaughan,A.H.,&Preston,G.W.1980,PASP,92,385
Vitinskij,Y.I.,Kopetskij,M.,&Kuklin,G.V.1986,Statistics of the Spot-forming Activity of the Sun(Nauka,Moskva.In Russian)
Zhao,J.-K.,Oswalt,T.D.,Chen,Y.-Q.,et al.2015,RAA(Research in Astronomy and Astrophysics),15,1282