Bibcode
Arregui, I.; Asensio Ramos, A.
Referencia bibliográfica
Highlights on Spanish Astrophysics IX, Proceedings of the XII Scientific Meeting of the Spanish Astronomical Society held on July 18-22, 2016, in Bilbao, Spain, ISBN 978-84-606-8760-3. S. Arribas, A. Alonso-Herrero, F. Figueras, C. Hernández-Monteagudo, A. Sánchez-Lavega, S. Pérez-Hoyos (eds.), 2017 , p. 587-592
Advertised on:
3
2017
Número de citas
0
Número de citas referidas
0
Descripción
We applied Bayesian techniques to the problem of inferring the magnetic
field strength in transversely oscillating solar coronal loops from
observed periods and damping times. This was done by computing the
marginal posterior probability density for parameters such as the
waveguide density, the density contrast, the transverse inhomogeneity
length scale, and the magnetic field strength under the assumption that
the observed waves can be modelled as standing or propagating
magnetohydrodynamic (MHD) kink modes of magnetic flux tubes. Our results
indicate that the magnetic field strength can be inferred, even if the
densities inside and outside the structure are largely unknown. When
information on plasma density is available, the method enables to
self-consistently include this knowledge to further constrain the
inferred magnetic field strength. The inclusion of the observed
oscillation damping enables to obtain information on the transverse
density structuring and considerably alters the obtained posterior for
the magnetic field strength.