Energy input flux in the global quiet-sun corona
We present first results of a novel technique that provides, for the first time, constraints on the energy input flux at the coronal base (r ∼ 1.025 R o) of the quiet Sun at a global scale. By combining differential emission measure tomography of EUV images, with global models of the coronal magneti...
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| Acceso en línea: | http://hdl.handle.net/20.500.12110/paper_0004637X_v843_n1_p_MacCormack |
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todo:paper_0004637X_v843_n1_p_MacCormack2023-10-03T14:02:43Z Energy input flux in the global quiet-sun corona Mac Cormack, C. Vásquez, A.M. López Fuentes, M. Nuevo, F.A. Landi, E. Frazin, R.A. Sun: corona Sun: fundamental parameters Sun: magnetic fields Sun: UV radiation We present first results of a novel technique that provides, for the first time, constraints on the energy input flux at the coronal base (r ∼ 1.025 R o) of the quiet Sun at a global scale. By combining differential emission measure tomography of EUV images, with global models of the coronal magnetic field, we estimate the energy input flux at the coronal base that is required to maintain thermodynamically stable structures. The technique is described in detail and first applied to data provided by the Extreme Ultraviolet Imager instrument, on board the Solar TErrestrial RElations Observatory mission, and the Atmospheric Imaging Assembly instrument, on board the Solar Dynamics Observatory mission, for two solar rotations with different levels of activity. Our analysis indicates that the typical energy input flux at the coronal base of magnetic loops in the quiet Sun is in the range ∼0.5-2.0 105 (erg s-1 cm-2), depending on the structure size and level of activity. A large fraction of this energy input, or even its totality, could be accounted for by Alfvén waves, as shown by recent independent observational estimates derived from determinations of the non-thermal broadening of spectral lines in the coronal base of quiet-Sun regions. This new tomography product will be useful for the validation of coronal heating models in magnetohydrodinamic simulations of the global corona. © 2017. The American Astronomical Society. All rights reserved. Fil:Vásquez, A.M. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:López Fuentes, M. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Nuevo, F.A. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_0004637X_v843_n1_p_MacCormack |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
| collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
Sun: corona Sun: fundamental parameters Sun: magnetic fields Sun: UV radiation |
| spellingShingle |
Sun: corona Sun: fundamental parameters Sun: magnetic fields Sun: UV radiation Mac Cormack, C. Vásquez, A.M. López Fuentes, M. Nuevo, F.A. Landi, E. Frazin, R.A. Energy input flux in the global quiet-sun corona |
| topic_facet |
Sun: corona Sun: fundamental parameters Sun: magnetic fields Sun: UV radiation |
| description |
We present first results of a novel technique that provides, for the first time, constraints on the energy input flux at the coronal base (r ∼ 1.025 R o) of the quiet Sun at a global scale. By combining differential emission measure tomography of EUV images, with global models of the coronal magnetic field, we estimate the energy input flux at the coronal base that is required to maintain thermodynamically stable structures. The technique is described in detail and first applied to data provided by the Extreme Ultraviolet Imager instrument, on board the Solar TErrestrial RElations Observatory mission, and the Atmospheric Imaging Assembly instrument, on board the Solar Dynamics Observatory mission, for two solar rotations with different levels of activity. Our analysis indicates that the typical energy input flux at the coronal base of magnetic loops in the quiet Sun is in the range ∼0.5-2.0 105 (erg s-1 cm-2), depending on the structure size and level of activity. A large fraction of this energy input, or even its totality, could be accounted for by Alfvén waves, as shown by recent independent observational estimates derived from determinations of the non-thermal broadening of spectral lines in the coronal base of quiet-Sun regions. This new tomography product will be useful for the validation of coronal heating models in magnetohydrodinamic simulations of the global corona. © 2017. The American Astronomical Society. All rights reserved. |
| format |
JOUR |
| author |
Mac Cormack, C. Vásquez, A.M. López Fuentes, M. Nuevo, F.A. Landi, E. Frazin, R.A. |
| author_facet |
Mac Cormack, C. Vásquez, A.M. López Fuentes, M. Nuevo, F.A. Landi, E. Frazin, R.A. |
| author_sort |
Mac Cormack, C. |
| title |
Energy input flux in the global quiet-sun corona |
| title_short |
Energy input flux in the global quiet-sun corona |
| title_full |
Energy input flux in the global quiet-sun corona |
| title_fullStr |
Energy input flux in the global quiet-sun corona |
| title_full_unstemmed |
Energy input flux in the global quiet-sun corona |
| title_sort |
energy input flux in the global quiet-sun corona |
| url |
http://hdl.handle.net/20.500.12110/paper_0004637X_v843_n1_p_MacCormack |
| work_keys_str_mv |
AT maccormackc energyinputfluxintheglobalquietsuncorona AT vasquezam energyinputfluxintheglobalquietsuncorona AT lopezfuentesm energyinputfluxintheglobalquietsuncorona AT nuevofa energyinputfluxintheglobalquietsuncorona AT landie energyinputfluxintheglobalquietsuncorona AT frazinra energyinputfluxintheglobalquietsuncorona |
| _version_ |
1807322208185352192 |