1 a b cc b * 1 Helioseismology * * r/r r/r a 1.3 FTD 9 11 Ω B ϕ α B p FTD 2 b Ω * 1 r, θ, ϕ ϕ * 2 *

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448 8542 1 e-mail: ymasada@auecc.aichi-edu.ac.jp 1. 400 400 1.1 10 1 1 5 1 11 2 3 4 656 2015 10

1 a b cc b 22 5 1.2 * 1 Helioseismology * 2 6 8 * 3 1 0.7 r/r 1.0 2 r/r 0.7 3 4 2a 1.3 FTD 9 11 Ω B ϕ α B p FTD 2 b Ω * 1 r, θ, ϕ ϕ * 2 * 3 108 10 657

2 a O 10 2 R b c Ω B p B ϕ d α α 2 c 2 d Ω FTD 10 5 G * 4 α FTD MHD* 5 2 a FTD 3 FTD FTD FTD * 4 sub-adiabatic * 5 Magneto-Hydro-Dynamics MHD 658 2015 10

3 a b a 29 b 30 4 3 FTD 10 5 G * 6 FTD 10 4 G 12 * 7 FTD 2. FTD FTD FTD 13 14 2.1 MHD 4 MHD 4 * 6 * 7 flux tube explosion 28 10 4 G 108 10 659

xy 20 21 xy Ω FTD 5 B x B y t cv 200t cv B x B y π/2 5 a B x, b B y t cv d CZ/v z,rms ( B = πρ 2 eq 4 v ) 660 2015 10

2.2 70 80 Moffatt 15 16 B B M δb B M δb B t M = [ u B + ε η B ], M M 0 M u M η 0 ε ε αb M γ B M η t B M, α, γ, η t α Ω u M B M α α FTD α u M 0 Ω α, γ, η t * 8 6 * 9 5 6 a B x 6 b B y B x B y 6 c π/2 6 c α 2.3 α * 8 First-Order Smoothing Approximation FOSA Second-Order Correlation Approximation SOCA * 9 α 11 108 10 661

6 a B x, b B y c α 2 τ c H 11 α 1 3 τ c. δu δu ( δu), α 20 21 7a 7 a b α 19 21 662 2015 10

7a 7b α 19 B y u z δb x δb x α B M exp ik z z iσt α σ =± + iαk z, z k z σ α α α α 80 17 18 3. 3.1 α α 108 10 663

3.2 α 2.2 α O 10 12 MHD 24 27 25 26 3.3 23 8 MHD 8 a B ϕ 8 b 8 b α 8 MHD 23 a B ϕ b 664 2015 10

MHD 13 14 23 1 Schwabe H., 1844, AN 21, 233 2 Carrington R. C., 1859, MNRAS 20, 13 3 Hale G. E., et al., 1919, ApJ 49, 153 4 Hale G. E., Nicholson S. B., 1925, ApJ 62, 270 5 Babcock H. D., 1959, ApJ 130, 363 6 Christensen-Dalsgaard J., et al., 1996, Science 272, 1286 7 Christensen-Dalsgaard J., 2002, RvMP 74, 1073 8 Thompson M. J., et al., 2003, ARA&A 41, 599 9 Dikpati M., Charbonneau P., 1999, ApJ 518, 508 10 Dikpati M., Gilman G. A., 2009, SSRv 144, 67 11 Charbonneau P., 2010, LRSP 7, 3 12 Rempel M., 2006, ApJ 647, 662 13 Masada Y., Sano T., 2014, PASJ 66, S27 14 Masada Y., Sano T., 2014, ApJL 794, L6 15 Moffatt H. K., 1978, Cambridge University Press 16 Krause F., Rädler K.-H., 1980, Oxford Pergamon Press 17 Baryshnikova I., Shukurov A., 1987, AN 308, 89 18 Raedler K.-H., Braeuer H.-J., 1987, AN 308, 101 19 Parker E. N., 1955, ApJ 122, 293 20 Spruit H. C., et al., 1990, ARA&A 28, 263 21 Miesch M. S., 2005, LRSP 2, 1 22 Mitra D., et al., 2010, ApJL 719, L1 23 Mabuchi J., Masada Y., Kageyama A., 2015, ApJ 806, 10 24 Hotta H., et al., 2014, ApJ 786, 24 25 Ghizaru M., et al., 2010, ApJL 715, L133 26 Käpylä P. J., et al., 2012, ApJL 755, L22 27 Nelson N. J., et al., 2013, ApJ 762, 73 28 Rempel M., Schüssler M., 2001, ApJL 552, L171 29 Schüssler M., Baumann I., 2006, A&A 459, 945 30 Guerrero G., de Gouveia Dal Pino E. M., 2007, A&A 464, 341 Coherent Magnetic Fields Organized in Turbulent Thermal Convections Exploring the Origin of Sunspots Youhei Masada Department of Physics and Astronomy, Aichi University of Education, Kariya, Aichi 448 8542, Japan Abstract: Solar activities, as is typified by flares and coronal-mass ejections, are caused by explosive releases of massive magnetic energy stored in sunspots, which are the sites of large-scale well-organized magnetic fields generated in the solar interior. Understanding the solar dynamo, which is responsible for the sunspot formation, is one of the outstanding problem in solar physics and is a milestone toward a coherent understanding of magnetic activities in the astrophysical plasma. Here we provide an overview of observed solar magnetic cycles and most promising dynamo model standard scenario which can successfully explain important aspects of the solar cycle. Then we report our recent study on the spontaneous formation of large-scale magnetic fields in turbulent thermal convections, which raises a question about the standard solar dynamo senario based on a hypothesis that large-scale magnetic fields can not be generated in the convection zone. 108 10 665