Asymmetric precipitation in a coronal loop as explanation of a singular observed spectrum
Almost 10 years of solar submillimeter observations have shown new aspects of solar activity, such as the presence of rapid solar spikes associated with the launch of coronal mass ejections and an increasing submillimeter spectral component in flares. We analyse the singular microwave-submillimeter...
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2009
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| Acceso en línea: | https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_02731177_v44_n11_p1314_Cristiani http://hdl.handle.net/20.500.12110/paper_02731177_v44_n11_p1314_Cristiani |
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paper:paper_02731177_v44_n11_p1314_Cristiani2023-06-08T15:25:37Z Asymmetric precipitation in a coronal loop as explanation of a singular observed spectrum Sun: flares Sun: radio radiation Magnetic fields Radio communication Solar energy Coronal magnetic fields Coronal mass ejection Magnetic-field intensity Precipitation rates Spectral components Submillimeter spectra Sun: flares Sun: radio radiation Telescopes Almost 10 years of solar submillimeter observations have shown new aspects of solar activity, such as the presence of rapid solar spikes associated with the launch of coronal mass ejections and an increasing submillimeter spectral component in flares. We analyse the singular microwave-submillimeter spectrum of an M class solar flare on 20 December, 2002. Flux density observations measured by Sun patrol telescopes and the Solar Submillimeter Telescope are used to build the radio spectrum, which is fitted using Ramaty's code. At submillimeter frequencies the spectrum shows a component different from the microwave classical burst. The fitting is achieved proposing two homogeneous sources of emission. This theoretical fitting is in agreement with differential precipitation through a magnetically asymmetric loop or set of loops. From a coronal magnetic field model we infer an asymmetric magnetic structure at the flare location. The model proposed to quantify the differential precipitation rates due to the asymmetry results in a total precipitation ratio Q2 / Q1 ≈ 104 s(-) 105, where Q1 (Q2) represents the total precipitation in the loop foot with the high (low) magnetic field intensity. This ratio agrees with the electron total number ratio of the two sources proposed to fit the radio spectrum. © 2009 COSPAR. 2009 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_02731177_v44_n11_p1314_Cristiani http://hdl.handle.net/20.500.12110/paper_02731177_v44_n11_p1314_Cristiani |
| 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: flares Sun: radio radiation Magnetic fields Radio communication Solar energy Coronal magnetic fields Coronal mass ejection Magnetic-field intensity Precipitation rates Spectral components Submillimeter spectra Sun: flares Sun: radio radiation Telescopes |
| spellingShingle |
Sun: flares Sun: radio radiation Magnetic fields Radio communication Solar energy Coronal magnetic fields Coronal mass ejection Magnetic-field intensity Precipitation rates Spectral components Submillimeter spectra Sun: flares Sun: radio radiation Telescopes Asymmetric precipitation in a coronal loop as explanation of a singular observed spectrum |
| topic_facet |
Sun: flares Sun: radio radiation Magnetic fields Radio communication Solar energy Coronal magnetic fields Coronal mass ejection Magnetic-field intensity Precipitation rates Spectral components Submillimeter spectra Sun: flares Sun: radio radiation Telescopes |
| description |
Almost 10 years of solar submillimeter observations have shown new aspects of solar activity, such as the presence of rapid solar spikes associated with the launch of coronal mass ejections and an increasing submillimeter spectral component in flares. We analyse the singular microwave-submillimeter spectrum of an M class solar flare on 20 December, 2002. Flux density observations measured by Sun patrol telescopes and the Solar Submillimeter Telescope are used to build the radio spectrum, which is fitted using Ramaty's code. At submillimeter frequencies the spectrum shows a component different from the microwave classical burst. The fitting is achieved proposing two homogeneous sources of emission. This theoretical fitting is in agreement with differential precipitation through a magnetically asymmetric loop or set of loops. From a coronal magnetic field model we infer an asymmetric magnetic structure at the flare location. The model proposed to quantify the differential precipitation rates due to the asymmetry results in a total precipitation ratio Q2 / Q1 ≈ 104 s(-) 105, where Q1 (Q2) represents the total precipitation in the loop foot with the high (low) magnetic field intensity. This ratio agrees with the electron total number ratio of the two sources proposed to fit the radio spectrum. © 2009 COSPAR. |
| title |
Asymmetric precipitation in a coronal loop as explanation of a singular observed spectrum |
| title_short |
Asymmetric precipitation in a coronal loop as explanation of a singular observed spectrum |
| title_full |
Asymmetric precipitation in a coronal loop as explanation of a singular observed spectrum |
| title_fullStr |
Asymmetric precipitation in a coronal loop as explanation of a singular observed spectrum |
| title_full_unstemmed |
Asymmetric precipitation in a coronal loop as explanation of a singular observed spectrum |
| title_sort |
asymmetric precipitation in a coronal loop as explanation of a singular observed spectrum |
| publishDate |
2009 |
| url |
https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_02731177_v44_n11_p1314_Cristiani http://hdl.handle.net/20.500.12110/paper_02731177_v44_n11_p1314_Cristiani |
| _version_ |
1768545049809780736 |