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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Autores principales: Mandrini, C.H., Jain, R., Innes D.E., Lagg A., Solanki S.K., Danesy D.
Formato: CONF
Materias:
Approximation theory
Extrapolation
Magnetometers
Telescopes
X rays
Coronal flux tubes
Michelson Doppler Imager
Soft X-ray loops
Solar active regions
Magnetic field effects
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_03796566_v_n596_p85_Mandrini
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
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spelling todo:paper_03796566_v_n596_p85_Mandrini2023-10-03T15:33:36Z On the scaling of magnetic field strength with loop length in solar active regions Mandrini, C.H. Jain, R. Innes D.E. Lagg A. Solanki S.K. Danesy D. 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. CONF info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar 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
Mandrini, C.H.
Jain, R.
Innes D.E.
Lagg A.
Solanki S.K.
Danesy D.
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.
format CONF
author Mandrini, C.H.
Jain, R.
Innes D.E.
Lagg A.
Solanki S.K.
Danesy D.
author_facet Mandrini, C.H.
Jain, R.
Innes D.E.
Lagg A.
Solanki S.K.
Danesy D.
author_sort Mandrini, C.H.
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
url http://hdl.handle.net/20.500.12110/paper_03796566_v_n596_p85_Mandrini
work_keys_str_mv AT mandrinich onthescalingofmagneticfieldstrengthwithlooplengthinsolaractiveregions
AT jainr onthescalingofmagneticfieldstrengthwithlooplengthinsolaractiveregions
AT innesde onthescalingofmagneticfieldstrengthwithlooplengthinsolaractiveregions
AT lagga onthescalingofmagneticfieldstrengthwithlooplengthinsolaractiveregions
AT solankisk onthescalingofmagneticfieldstrengthwithlooplengthinsolaractiveregions
AT danesyd onthescalingofmagneticfieldstrengthwithlooplengthinsolaractiveregions
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