Arregui, I.
Bibliographical reference
Advances in Space Research, Volume 61, Issue 2, p. 655-672.
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1
2018
Journal
Citations
33
Refereed citations
32
Description
In contrast to the situation in a laboratory, the study of the solar
atmosphere has to be pursued without direct access to the physical
conditions of interest. Information is therefore incomplete and
uncertain and inference methods need to be employed to diagnose the
physical conditions and processes. One of such methods, solar
atmospheric seismology, makes use of observed and theoretically
predicted properties of waves to infer plasma and magnetic field
properties. A recent development in solar atmospheric seismology
consists in the use of inversion and model comparison methods based on
Bayesian analysis. In this paper, the philosophy and methodology of
Bayesian analysis are first explained. Then, we provide an account of
what has been achieved so far from the application of these techniques
to solar atmospheric seismology and a prospect of possible future
extensions.
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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
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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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