Magnetic-Field Concentration and the Twisted Solar Coronal Loops
The magnetostatic equilibrium of axisymmetric, cylindrical magnetic flux ropes in the solar corona is considered. The conditions for the concentration of strong (hundreds of gauss) magnetic fields in neutralized (shielded) and non-neutralized (unshielded) flux ropes in which the azimuthal component...
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| Published in | Geomagnetism and Aeronomy Vol. 61; no. 7; pp. 1052 - 1056 |
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| Main Authors | , , |
| Format | Journal Article |
| Language | English |
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Moscow
Pleiades Publishing
01.12.2021
Springer Nature B.V |
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| Abstract | The magnetostatic equilibrium of axisymmetric, cylindrical magnetic flux ropes in the solar corona is considered. The conditions for the concentration of strong (hundreds of gauss) magnetic fields in neutralized (shielded) and non-neutralized (unshielded) flux ropes in which the azimuthal component of the magnetic field in the outer region is either, respectively, zero or continuous on the boundary lateral surface, are discussed. On the example of the generalized, force-free, magnetic Gold–Hoyle configuration, it is shown that non-neutralized flux ropes, in contrast to neutralized ones, are capable of providing a magnetic-field concentration tens of times higher than the background field values at a relatively low (<10) number of turns of magnetic-field lines around the tube axis. The origin of twisted magnetic fields in the solar corona is discussed based on the results. |
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| AbstractList | The magnetostatic equilibrium of axisymmetric, cylindrical magnetic flux ropes in the solar corona is considered. The conditions for the concentration of strong (hundreds of gauss) magnetic fields in neutralized (shielded) and non-neutralized (unshielded) flux ropes in which the azimuthal component of the magnetic field in the outer region is either, respectively, zero or continuous on the boundary lateral surface, are discussed. On the example of the generalized, force-free, magnetic Gold–Hoyle configuration, it is shown that non-neutralized flux ropes, in contrast to neutralized ones, are capable of providing a magnetic-field concentration tens of times higher than the background field values at a relatively low (<10) number of turns of magnetic-field lines around the tube axis. The origin of twisted magnetic fields in the solar corona is discussed based on the results. |
| Author | Tsap, Yu. T. Kopylova, Yu. G. Stepanov, A. V. |
| Author_xml | – sequence: 1 givenname: Yu. T. surname: Tsap fullname: Tsap, Yu. T. email: yur_crao@mail.ru organization: Crimean Astronomical Observatory, Russian Academy of Sciences – sequence: 2 givenname: A. V. surname: Stepanov fullname: Stepanov, A. V. email: stepanov@gaoran.ru organization: Central Astronomical Observatory at Pulkovo, Russian Academy of Sciences – sequence: 3 givenname: Yu. G. surname: Kopylova fullname: Kopylova, Yu. G. email: yul@gaoran.ru organization: Central Astronomical Observatory at Pulkovo, Russian Academy of Sciences |
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| SubjectTerms | Corona Coronal loops Earth and Environmental Science Earth Sciences Fluctuations Geophysics/Geodesy Magnetic fields Magnetic flux Magnetism Solar corona Solar magnetic field |
| Title | Magnetic-Field Concentration and the Twisted Solar Coronal Loops |
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