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DC Field | Value | Language |
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dc.contributor.author | Wandurraga, Paula C. | - |
dc.contributor.author | Navarro, Anamaria | - |
dc.contributor.author | Lora-Clavijo, Fabio D. | - |
dc.date.accessioned | 2022-06-23T00:13:59Z | - |
dc.date.available | 2022-06-23T00:13:59Z | - |
dc.date.issued | 2021-03-26 | - |
dc.identifier.issn | 0370-3908 | spa |
dc.identifier.uri | https://repositorio.accefyn.org.co/handle/001/1274 | - |
dc.description.abstract | Existen observaciones que indican que el campo magnético en la atmósfera solar tiene twist, esto cumple un papel muy importante en diferentes fenómenos solares como la reconexión magnética, las fulguraciones solares, entre otros. Sin embargo, su influencia en este tipo de fenómenos aún no es clara. Con esa motivación, en este artículo se estudia, mediante varias simulaciones numéricas 3D, el efecto del twist del campo magnético en la propagación de ondas torsionales de Alfvén y magnetoacústicas a lo largo de la fotosfera y la cromosfera baja de un Sol con poca actividad. Con la finalidad de simular la dinámica de estas ondas magnetohidrodinámicas (MHD), se solucionaron numéricamente las ecuaciones linealizadas de la MHD ideal en tres dimensiones, asumiendo un Sol con poca actividad, el cual fue alterado con una perturbación inicial tipo twist en el campo de velocidades, para seis valores diferentes del parámetro de twist y tres magnitudes del campo magnético en equilibrio. Particularmente, se analizó la morfología 3D de las líneas de los campos de velocidad y magnético, y el perfil espacial de la componente transversal de estos campos, asociada con las ondas torsionales de Alfvén. Los resultados de las simulaciones numéricas, revelan la amplificación del campo magnético debido al parámetro de twist. Específicamente, se observó que esta cantidad aumenta cuando el parámetro de twist aumenta y es menor para grandes magnitudes del campo magnético en equilibrio. Además, se mostró que el valor máximo de la amplificación en función del twist exhibe un comportamiento exponencial. Finalmente, se observó que el vector de flujo de Poynting es mayor si el twist es mayor y se reduce para campos magnéticos iniciales más intensos. | spa |
dc.description.abstract | Observations indicate that the magnetic field in the solar atmosphere is twisted, playing an important role in different solar phenomena, such as magnetic reconnection or solar flaring activity, among others. However its influence on these kind of phenomena remains unclear. Motivated by this, we study, through several 3D numerical simulations, the effect of the magnetic field twist on the propagation of torsional Alfv´ en and magneto-acoustic waves moving along the photosphere and the lower chromosphere in the quiet Sun. In order to simulate the dynamics of these magnetohydrodynamic (MHD) waves, we solve numerically the ideal 3D linearized MHD equations by assuming a quiet Sun, which is excited by an initial twist perturbation in the velocity vector field, for six different values of the twist parameter and three equilibrium magnetic field strengths. Particularly, we analyze the 3D morphology of the velocity and magnetic fields lines, and the spatial profiles of the transversal component of these fields associated with the torsional Alfv´én waves. The results of our numerical simulations reveal the magnetic field amplification due to the twist parameter. Specifically, we have observed that this quantity increases as the twist parameter increases and decreases for larger values of the equilibrium magnetic strength. Moreover, we show that the maximum of amplification as function of the twist has an exponential behavior. Finally, we notice that the Poynting vector flux is greater for larger values of the initial twist but is smaller for more intense equilibrium magnetic fields. | eng |
dc.format.mimetype | application/pdf | spa |
dc.language.iso | spa | spa |
dc.publisher | Academia Colombiana de Ciencias Exactas, Físicas y Naturales | spa |
dc.title | Propagación de ondas de Alfvén atmósfera solar estratificada | spa |
dc.type | Artículo de revista | spa |
dcterms.audience | Estudiantes, Profesores, Comunidad científica. | spa |
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dc.rights.accessrights | info:eu-repo/semantics/openAccess | spa |
dc.type.driver | info:eu-repo/semantics/article | spa |
dc.type.version | info:eu-repo/semantics/updatedVersion | spa |
dc.rights.creativecommons | Atribución 4.0 Internacional (CC BY 4.0) | spa |
dc.identifier.doi | https://doi.org/10.18257/raccefyn.1245 | - |
dc.subject.proposal | MHD | spa |
dc.subject.proposal | MHD | eng |
dc.subject.proposal | atmósfera solar | spa |
dc.subject.proposal | Solar Atmosphere | eng |
dc.subject.proposal | Métodos Numéricos | spa |
dc.subject.proposal | Numerical Methods | eng |
dc.type.coar | http://purl.org/coar/resource_type/c_6501 | spa |
dc.relation.ispartofjournal | Revista de la Academia Colombiana de Ciencias Exactas, Físicas y Naturales | spa |
dc.relation.citationvolume | 45 | spa |
dc.relation.citationstartpage | 52 | spa |
dc.relation.citationendpage | 66 | spa |
dc.contributor.corporatename | Academia Colombiana de Ciencias Exactas, Físicas y Naturales | spa |
dc.identifier.eissn | 2382-4980 | spa |
dc.relation.citationissue | 174 | spa |
dc.type.content | Text | spa |
dc.type.redcol | http://purl.org/redcol/resource_type/ART | spa |
oaire.accessrights | http://purl.org/coar/access_right/c_abf2 | spa |
oaire.version | http://purl.org/coar/version/c_970fb48d4fbd8a85 | spa |
Appears in Collections: | BA. Revista de la Academia Colombiana de Ciencias Exactas Físicas y Naturales |
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