On the scaling of magnetic field strength with loop length in solar active regions
Recognizing that loops are the main structures of the solar corona, we investigate how the magnetic field strength of coronal flux tubes depends on the end-to-end length of the tube for a sample of active regions. We use photospheric magnetograms from the Michelson Doppler Imager, aboard the Solar a...
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2005
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| Acceso en línea: | https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03796566_v_n596_p85_Mandrini http://hdl.handle.net/20.500.12110/paper_03796566_v_n596_p85_Mandrini |
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paper:paper_03796566_v_n596_p85_Mandrini2023-06-08T15:40:45Z On the scaling of magnetic field strength with loop length in solar active regions Approximation theory Extrapolation Magnetometers Telescopes X rays Coronal flux tubes Michelson Doppler Imager Soft X-ray loops Solar active regions Magnetic field effects Recognizing that loops are the main structures of the solar corona, we investigate how the magnetic field strength of coronal flux tubes depends on the end-to-end length of the tube for a sample of active regions. We use photospheric magnetograms from the Michelson Doppler Imager, aboard the Solar and Heliospheric Observatory, and compute potential and linear force-free extrapolation models. The free parameter of the models is adjusted so as to match the soft X-ray loops observed by the Solar X-ray Telescope that flew aboard Yohkoh. For each model, we determine the average coronal field strength, < B >, in approximately one thousand individual flux tubes with regularly spaced footpoints, and obtain scatter plots of < B > versus length, L. We determine the dependence of < B > with L for a wide range of flux-tube lengths and, then, we restrict to the range which is meaningful for the soft X-ray emission. For this range we find that < B >∼ L δ with δ = -1.3 ± 0.5. We compare our results with those of Mandrini et al. (2000), and find that both are fully consistent. Such studies have important implications for solar coronal heating models. 2005 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03796566_v_n596_p85_Mandrini http://hdl.handle.net/20.500.12110/paper_03796566_v_n596_p85_Mandrini |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
| collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
Approximation theory Extrapolation Magnetometers Telescopes X rays Coronal flux tubes Michelson Doppler Imager Soft X-ray loops Solar active regions Magnetic field effects |
| spellingShingle |
Approximation theory Extrapolation Magnetometers Telescopes X rays Coronal flux tubes Michelson Doppler Imager Soft X-ray loops Solar active regions Magnetic field effects On the scaling of magnetic field strength with loop length in solar active regions |
| topic_facet |
Approximation theory Extrapolation Magnetometers Telescopes X rays Coronal flux tubes Michelson Doppler Imager Soft X-ray loops Solar active regions Magnetic field effects |
| description |
Recognizing that loops are the main structures of the solar corona, we investigate how the magnetic field strength of coronal flux tubes depends on the end-to-end length of the tube for a sample of active regions. We use photospheric magnetograms from the Michelson Doppler Imager, aboard the Solar and Heliospheric Observatory, and compute potential and linear force-free extrapolation models. The free parameter of the models is adjusted so as to match the soft X-ray loops observed by the Solar X-ray Telescope that flew aboard Yohkoh. For each model, we determine the average coronal field strength, < B >, in approximately one thousand individual flux tubes with regularly spaced footpoints, and obtain scatter plots of < B > versus length, L. We determine the dependence of < B > with L for a wide range of flux-tube lengths and, then, we restrict to the range which is meaningful for the soft X-ray emission. For this range we find that < B >∼ L δ with δ = -1.3 ± 0.5. We compare our results with those of Mandrini et al. (2000), and find that both are fully consistent. Such studies have important implications for solar coronal heating models. |
| title |
On the scaling of magnetic field strength with loop length in solar active regions |
| title_short |
On the scaling of magnetic field strength with loop length in solar active regions |
| title_full |
On the scaling of magnetic field strength with loop length in solar active regions |
| title_fullStr |
On the scaling of magnetic field strength with loop length in solar active regions |
| title_full_unstemmed |
On the scaling of magnetic field strength with loop length in solar active regions |
| title_sort |
on the scaling of magnetic field strength with loop length in solar active regions |
| publishDate |
2005 |
| url |
https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03796566_v_n596_p85_Mandrini http://hdl.handle.net/20.500.12110/paper_03796566_v_n596_p85_Mandrini |
| _version_ |
1768546726263652352 |