Coronal loop physical parameters from the analysis of multiple observed transverse oscillations

Bibcode
2013A&A...554A...7A
DOI
10.1051/0004-6361/201321428
Asensio-Ramos, A.; Arregui, I.
Bibliographical reference

Astronomy and Astrophysics, Volume 554, id.A7, 9 pp.

Advertised on:
6
2013
Journal
Astronomy and Astrophysics
Number of authors
2
IAC number of authors
2
Citations
18
Refereed citations
18
Description
The analysis of quickly damped transverse oscillations of solar coronal loops using magneto-hydrodynamic seismology allows us to infer physical parameters that are difficult to measure otherwise. Under the assumption that such damped oscillations are due to the resonant conversion of global modes into Alfvén oscillations of the tube surface, we carry out a global seismological analysis of a large set of coronal loops. A Bayesian hierarchical method is used to obtain distributions for coronal loop physical parameters by means of a global analysis of a large number of observations. The resulting distributions summarize global information and constitute data-favoured information that can be used for the inversion of individual events. The results strongly suggest that internal Alfvén travel times along the loop are longer than 100 s and shorter than 540 s with 95% probability. Likewise, the density contrast between the loop interior and the surrounding is larger than 2.3 and below 6.9 with 95% probability.
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Solar and Stellar Magnetism

Magnetic fields are at the base of star formation and stellar structure and evolution. When stars are born, magnetic fields brake the rotation during the collapse of the mollecular cloud. In the end of the life of a star, magnetic fields can play a key role in the form of the strong winds that lead to the last stages of stellar evolution. During

Tobías
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In progress
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Magnetism, Polarization and Radiative Transfer in Astrophysics

Magnetic fields pervade all astrophysical plasmas and govern most of the variability in the Universe at intermediate time scales. They are present in stars across the whole Hertzsprung-Russell diagram, in galaxies, and even perhaps in the intergalactic medium. Polarized light provides the most reliable source of information at our disposal for the

Tanausú del
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In progress
Type
Refereed
Methods
Solar Physics (FS)

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