Description of Maunder-like events from a stochastic Alpha-Omega model

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One of the most impressive solar phenomena is its magnetic activity cycle. The number of sunspots observed in the solar surface varies with a period of approximately 11 years. Superimposed to this cyclic behavior, there are sporadic events such as the Maunder minimum, during which very few sunspots...

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Autor principal: Gómez, Daniel Osvaldo
Otros Autores: Mininni, P.D
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: 2006
Acceso en línea:Registro en Scopus
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Registro en la Biblioteca Digital
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Biblioteca Central Dr. Luis F. Leloir (FCEN) de Universidad de Buenos Aires
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100 1 |a Gómez, Daniel Osvaldo 
245 1 0 |a Description of Maunder-like events from a stochastic Alpha-Omega model 
260 |c 2006 
270 1 0 |m Gómez, D.O.; Instituto de Astronomía y Física del Espacio, CC. 67, Suc. 28, 1428 Buenos Aires, Argentina; email: dgomez@df.uba.ar 
504 |a Beck, J.G., Duvall Jr., T.L., Scherrer, P.H., (1998) Nature, 394, p. 653 
504 |a Beck, J.G., (1999) Sol. Phys., 191, p. 47 
504 |a Beer, J., Blinov, A., Bonani, G., Hofmann, H.J., Finkel, R.C., (1990) Nature, 347, p. 164 
504 |a Beer, J., (2000) Space Sci. Rev., 94, p. 53 
504 |a Caligari, P., Moreno-Insertis, F., Schüssler, M., (1995) ApJ, 441, p. 886 
504 |a Cameron, R., Hopkins, A., (1998) Sol. Phys., 183, p. 263 
504 |a Carbonell, M., Oliver, R., Ballester, J.L., (1994) A&A, 290, p. 983 
504 |a Charbonneau, P., Blais-Laurier, G., St-Jean, C., (2004) ApJ, 616, pp. L183 
504 |a Choudhuri, A.R., (1992) A&A, 253, p. 277 
504 |a Dikpati, M., Charbonneau, P., (1999) ApJ, 518, p. 508 
504 |a Knobloch, E., Tobias, S.M., Weiss, N.O., (1998) MNRAS, 297, p. 1123 
504 |a Krause, F., Rädler, K.-H., (1980) Mean-Field Magnetohydrodynamics and Dynamo Theory, , Pergamon, Oxford 
504 |a Leighton, R.B., (1969) ApJ, 156, p. 1 
504 |a Mininni, P.D., Gómez, D.O., (2002) ApJ, 573, p. 454 
504 |a Mininni, P.D., Gómez, D.O., Mindlin, G.B., (2002) Phys. Rev. Lett., 89, p. 061101 
504 |a Nandy, D., Choudhuri, A.R., (2002) Science, 296, p. 1671 
504 |a Ossendrijver, A.J.H., Hoyng, P., Schmitt, D., (1996) A&A, 313, p. 938 
504 |a Parker, E.N., (1979) Cosmical Magnetic Fields: Their Origin and Their Activity, , Oxford University Press, New York 
504 |a Ribes, J.C., Nesme-Ribes, E., (1993) A&A, 276, p. 549 
504 |a Sokoloff, D., Nesme-Ribes, E., (1994) A&A, 288, p. 293 
504 |a Solanki, S.K., Schüssler, M., Fligge, M., (2000) Nature, 408, p. 445 
504 |a Svensmark, H., (1998) Phys. Rev. Lett., 81, p. 5027 
504 |a Wang, Y.-M., Sheeley, N.R., Nash, A.G., (1991) ApJ, 383, p. 431 
506 |2 openaire  |e Política editorial 
520 3 |a One of the most impressive solar phenomena is its magnetic activity cycle. The number of sunspots observed in the solar surface varies with a period of approximately 11 years. Superimposed to this cyclic behavior, there are sporadic events such as the Maunder minimum, during which very few sunspots were detected. In the present work, an Alpha-Omega dynamo model is proposed to study these phenomena. We use velocity profiles of the solar interior obtained from helioseismology, which include differential rotation (the Ω-effect), a meridional flow and the turbulent velocity field of the convective region (the α-effect). By simulating the helicoidal and disordered flow of the giant cells through a stochastic component in the α coefficient, we reproduce not only the periodic behavior of the solar cycle, but also sporadic events such as the Maunder minimum. This model suggests the existence of a link between giant cell fluctuations and the irregularities observed in the solar cycle, such as north-south asymmetries and secular variations like the Maunder minimum. © 2005 COSPAR.  |l eng 
536 |a Detalles de la financiación: Agencia Nacional de Promoción Científica y Tecnológica 
536 |a Detalles de la financiación: PICT 03-9483, PIP 2693 
536 |a Detalles de la financiación: This work was supported by the Argentinean Grants UBACyT X292, CONICET PIP 2693, and PICT 03-9483 (ANPCyT). D.O.G. is a member of the Carrera del Investigador Cientı´fico, CONICET. 
593 |a Instituto de Astronomía y Física del Espacio, CC. 67, Suc. 28, 1428 Buenos Aires, Argentina 
593 |a Departamento de Física, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, 1428 Buenos Aires, Argentina 
690 1 0 |a MAUNDER MINIMUM 
690 1 0 |a SOLAR CYCLE 
690 1 0 |a COMPUTER SIMULATION 
690 1 0 |a HEAT CONVECTION 
690 1 0 |a MAGNETIC FIELD EFFECTS 
690 1 0 |a MATHEMATICAL MODELS 
690 1 0 |a RANDOM PROCESSES 
690 1 0 |a SURFACE PHENOMENA 
690 1 0 |a VELOCITY 
690 1 0 |a DIFFERENTIAL ROTATION 
690 1 0 |a MAGNETIC ACTIVITY CYCLE 
690 1 0 |a MAUNDER MINIMUM 
690 1 0 |a SOLAR CYCLE 
690 1 0 |a SOLAR SYSTEM 
700 1 |a Mininni, P.D. 
773 0 |d 2006  |g v. 38  |h pp. 856-861  |k n. 5  |p Adv. Space Res.  |x 02731177  |w (AR-BaUEN)CENRE-3577  |t Advances in Space Research 
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856 4 0 |u https://doi.org/10.1016/j.asr.2005.07.032  |y DOI 
856 4 0 |u https://hdl.handle.net/20.500.12110/paper_02731177_v38_n5_p856_Gomez  |y Handle 
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963 |a VARI 
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