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| Campo DC | Valor | Lengua/Idioma |
|---|---|---|
| dc.provenance | Facultad de Ciencias Exactas y Naturales de la UBA | - |
| dc.contributor | <div class="autor_fcen" id="5788">Mininni, P.D.</div> | - |
| dc.contributor | <div class="autor_fcen" id="3802">Gómez, D.O.</div> | - |
| dc.creator | <div class="autor_fcen" id="5788">Mininni, P.D.</div> | - |
| dc.creator | <div class="autor_fcen" id="3802">Gómez, D.O.</div> | - |
| dc.date.accessioned | 2018-05-04T22:08:31Z | - |
| dc.date.accessioned | 2018-05-28T15:47:24Z | - |
| dc.date.available | 2018-05-04T22:08:31Z | - |
| dc.date.available | 2018-05-28T15:47:24Z | - |
| dc.date.issued | 2004 | - |
| dc.identifier.uri | http://10.0.0.11:8080/jspui/handle/bnmm/68289 | - |
| dc.description | We present a new technique suitable for a detailed comparison between solar dynamo models and observations. The method is based on the technique of dynamo spectroscopy proposed by Hoyng & Schutgens (1995) and bi-orthogonal decomposition of solar data. This decomposition provides a representation of the mean and fluctuating components of the flows, yielding relevant information for the comparison. To illustrate the method, we use a simple kinematic dynamo model of the solar cycle. Irregularities are introduced in the evolution of the magnetic fields modeling the turbulent behavior of the solar convective region with a random perturbation on the external source for the poloidal field. After fine tuning the parameters of the model we obtain solar like solutions displaying a magnetic cycle of 22 years, with fluctuations in its period and amplitude. In addition, the model generates Maunder-like events with a time span of 60-100 years. | - |
| dc.description | Fil:Mininni, P.D. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. | - |
| dc.description | Fil:Gómez, D.O. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. | - |
| dc.format | application/pdf | - |
| dc.language | eng | - |
| dc.rights | info:eu-repo/semantics/openAccess | - |
| dc.rights | http://creativecommons.org/licenses/by/2.5/ar | - |
| dc.source | Astron. Astrophys. 2004;426(3):1065-1073 | - |
| dc.source.uri | http://digital.bl.fcen.uba.ar/Download/paper/paper_00046361_v426_n3_p1065_Mininni.pdf | - |
| dc.subject | Magnetohydrodynamics (MHD) | - |
| dc.subject | Sun: magnetic fields | - |
| dc.subject | Sun: sunspots | - |
| dc.subject | Astrophysics | - |
| dc.subject | Chaos theory | - |
| dc.subject | Kinematics | - |
| dc.subject | Magnetic fields | - |
| dc.subject | Magnetohydrodynamics | - |
| dc.subject | Random processes | - |
| dc.subject | Satellite observatories | - |
| dc.subject | Spectroscopy | - |
| dc.subject | Solar cycle | - |
| dc.subject | Stochasticity | - |
| dc.subject | Sun: magnetic fields | - |
| dc.subject | Sun: sunspots | - |
| dc.subject | Sun | - |
| dc.title | A new technique for comparing solar dynamo models and observations | - |
| dc.type | info:eu-repo/semantics/article | - |
| dc.type | info:ar-repo/semantics/artículo | - |
| dc.type | info:eu-repo/semantics/publishedVersion | - |
| Aparece en las colecciones: | FCEN - Facultad de Ciencias Exactas y Naturales. UBA | |
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