Advanced Forward Modeling and Inversion of Stokes Profiles Resulting from the Joint Action of the Hanle and Zeeman Effects

Ramos, A. Asensio; Bueno, J. Trujillo; Degl’Innocenti, E. Landi

doi:10.1086/589433

Cited by 144 publications

(34 citation statements)

References 47 publications

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“…[125][126][127][128][129]). They serve especially to map flows and magnetic fields from full-Stokes line profiles.…”

Section: (Viii) Inversion Modellingmentioning

confidence: 99%

The quiet-Sun photosphere and chromosphere

Rutten

2012

Phil. Trans. R. Soc. A.

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The overall structure and the fine structure of the solar photosphere outside active regions are largely understood, except possibly the important roles of a turbulent near-surface dynamo at its bottom, internal gravity waves at its top and small-scale vorticity. Classical one-dimensional static radiation-escape modelling has been replaced by three-dimensional time-dependent magento-hydrodynamic simulations that come closer to reality. The solar chromosphere, in contrast, remains little understood, although its pivotal role in coronal mass and energy loading makes it a principal research area. Its fine structure defines its overall structure, so that hard-to-observe and hard-to-model small-scale dynamical processes are key to understanding. However, both chromospheric observation and chromospheric simulation presently mature towards the required sophistication. Open-field features seem of greater interest than easier-to-see closed-field features.

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“…[125][126][127][128][129]). They serve especially to map flows and magnetic fields from full-Stokes line profiles.…”

Section: (Viii) Inversion Modellingmentioning

confidence: 99%

The quiet-Sun photosphere and chromosphere

Rutten

2012

Phil. Trans. R. Soc. A.

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“…A first-order NLTE correction was applied to obtain the temperature stratification of the chromosphere of the QS and active region (Beck et al 2013(Beck et al , 2015. However, the development of NLTE radiative transfer codes, such as HAZEL (Asensio Ramos et al 2008), HELIX + (Lagg et al 2009), andNICOLE (SocasNavarro et al 2015), combined with the increased computational power available, also make NLTE inversions possible (see the review by de la Cruz Rodríguez & van Noort 2016).…”

Section: Introductionmentioning

confidence: 99%

Spectroscopic Inversions of the Ca ii 8542 Å Line in a C-class Solar Flare

Kuridze

Henriques

Mathioudakis

et al. 2017

ApJ

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We study the C8.4-class solar flare SOL2016-05-14T11:34 UT using high-resolution spectral imaging in the Ca II 8542 Å line obtained with the CRISP imaging spectropolarimeter on the Swedish 1 m Solar Telescope. Spectroscopic inversions of the Ca II 8542 Å line using the non-LTE code NICOLE are used to investigate the evolution of the temperature and velocity structure in the flaring chromosphere. A comparison of the temperature stratification in flaring and non-flaring areas reveals strong footpoint heating during the flare peak in the lower atmosphere. The temperature of the flaring footpoints between log 2.5 and 3.5 500 t » --, where τ 500 is the continuum optical depth at 500 nm, is 5 6.5 kK -close to the flare peak, reducing gradually to 5 kK . The temperature in the middle and upper chromosphere, between log 3.5 500 t » -and −5.5, is estimated to be ∼6.5-20 kK, decreasing to preflare temperatures, ∼5-10 kK, after approximately 15 minutes. However, the temperature stratification of the non-flaring areas is unchanged. The inverted velocity fields show that the flaring chromosphere is dominated by weak downflowing condensations at the formation height of Ca II 8542 Å.

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“…We used the HAZEL inversion code (Asensio Ramos et al 2008) to infer the thermodynamical and magnetic properties of our observed prominence. The code solves the forward problem by integrating the radiative transfer equation for polarized light on a slab of constant physical properties.…”

Section: Spectro-polarimetric Inversionsmentioning

confidence: 99%

On the Magnetism and Dynamics of Prominence Legs Hosting Tornadoes

González

Ramos

Arregui

et al. 2016

ApJ

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Solar tornadoes are dark vertical filamentary structures observed in the extreme ultraviolet associated with prominence legs and filament barbs. Their true nature and relationship to prominences requires an understanding of their magnetic structure and dynamic properties. Recently, a controversy has arisen: is the magnetic field organized forming vertical, helical structures or is it dominantly horizontal? And concerning their dynamics, are tornadoes really rotating or is it just a visual illusion? Here we analyze four consecutive spectro-polarimetric scans of a prominence hosting tornadoes on its legs, which helps us shed some light on their magnetic and dynamical properties. We show that the magnetic field is very smooth in all the prominence, which is probably an intrinsic property of the coronal field. The prominence legs have vertical helical fields that show slow temporal variation that is probably related to the motion of the fibrils. Concerning the dynamics, we argue that (1) if rotation exists, it is intermittent, lasting no more than one hour, and (2) the observed velocity pattern is also consistent with an oscillatory velocity pattern (waves).

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Advanced Forward Modeling and Inversion of Stokes Profiles Resulting from the Joint Action of the Hanle and Zeeman Effects

Cited by 144 publications

References 47 publications

The quiet-Sun photosphere and chromosphere

The quiet-Sun photosphere and chromosphere

Spectroscopic Inversions of the Ca ii 8542 Å Line in a C-class Solar Flare

On the Magnetism and Dynamics of Prominence Legs Hosting Tornadoes

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