The Circular Polarization of the Mn 1 Resonance Lines around 280 nm for Exploring Chromospheric Magnetism

Alemán, T. del Pino; Ballester, Ernest Alsina; Bueno, J. Trujillo

doi:10.3847/1538-4357/ac922c

Cited by 7 publications

(3 citation statements)

References 22 publications

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“…Moreover, the WFA can be applied to the observations using the effective Landé factor calculated assuming LS coupling without HFS (del Pino Alemán et al 2022). All the results shown here regarding the Mg II and Mn I lines in this spectral window agree with previous results (del Pino Alemán et al 2020, 2022Ishikawa et al 2021).…”

Section: Theoretical Circular Polarization Profilessupporting

confidence: 88%

Magnetic Field Information in the Near-ultraviolet Fe ii Lines of the CLASP2 Space Experiment

Afonso Delgado,

del Pino Alemán,

Trujillo Bueno

2023

ApJ

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We investigate theoretically the circular polarization signals induced by the Zeeman effect in the Fe ii lines of the 279.3–280.7 nm spectral range of the CLASP2 space experiment and their suitability to infer solar magnetic fields. To this end, we use a comprehensive Fe ii atomic model to solve the problem of the generation and transfer of polarized radiation in semiempirical models of the solar atmosphere, comparing the region of formation of the Fe ii spectral lines with those of the Mg ii h and k and the Mn i resonance lines. These are present in the same near-ultraviolet (near-UV) spectral region and allowed the mapping of the longitudinal component of the magnetic field (B L) through several layers of the solar chromosphere in an active region plage. We compare our synthetic intensity profiles with observations from the IRIS and CLASP2 missions, proving the suitability of our model atom to characterize these Fe ii spectral lines. The CLASP2 observations show two Fe ii spectral lines at 279.79 and 280.66 nm with significant circular polarization signals. We demonstrate the suitability of the weak-field approximation applied to the Stokes I and V profiles of these Fe ii lines to infer B L in the plage atmosphere. We conclude that the near-UV spectral region of CLASP2 allows us to determine B L from the upper photosphere to the top of the chromosphere of active region plages.

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Section: Theoretical Circular Polarization Profilessupporting

confidence: 88%

Magnetic Field Information in the Near-ultraviolet Fe ii Lines of the CLASP2 Space Experiment

Afonso Delgado,

del Pino Alemán,

Trujillo Bueno

2023

ApJ

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“…2021) first analyzed the data used in this work by applying the WFA to infer B at different heights in the solar atmosphere. The discrete heights of the B values inferred via the WFA are only approximate, with the locations along the LOS based on theoretical investigations (Afonso Delgado et al 2023;del Pino Alemán et al 2022).…”

Section: Inverted Model Atmospherementioning

confidence: 99%

Tomography of a solar plage with the Tenerife Inversion Code

Li¹,

Alemán²,

Bueno³

et al. 2023

Preprint

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We apply the Tenerife Inversion Code (TIC) to the plage spectropolarimetric observations obtained by the Chromospheric LAyer SpectroPolarimeter (CLASP2). These unprecedented data consist of full Stokes profiles in the spectral region around the Mg II h and k lines for a single slit position, with around two thirds of the 200 arcsec slit crossing a plage region and the rest crossing an enhanced network. A former analysis of these data had allowed us to infer the longitudinal component of the magnetic field by applying the weak field approximation (WFA) to the circular polarization profiles, and to assign the inferred magnetic fields to different layers of the solar atmosphere based on the results of previous theoretical radiative transfer investigations. In this work, we apply the recently developed TIC to the same data. We obtain the stratified model atmosphere that fits the intensity and circular polarization profiles at each position along the spectrograph slit and we compare our results for the longitudinal component of the magnetic field with the previously obtained WFA results, highlighting the generally good agreement in spite of the fact that the WFA is known to produce an underestimation when applied to the outer lobes of the Mg II h and k circular polarization profiles. Finally, we use the inverted model atmospheres to give a rough estimation of the energy that could be carried by Alfvén waves propagating along the chromosphere in the plage and network regions, showing that it is sufficient to compensate the estimated energy losses in the chromosphere of solar active regions.

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“…A first analysis of these data enabled an estimate of the longitudinal component of the magnetic field by applying the weak-field approximation (WFA) to the intensity and circular polarization profiles (Ishikawa et al 2021). Based on theoretical radiative transfer investigations, the magnetic field strengths inferred from the Mg II h-k doublet (del Pino Alemán et al 2020;Afonso Delgado et al 2023) and Mn I triplet (del Pino Alemán et al 2022) were assigned to different layers of the solar atmosphere. In particular, the Mg II lines provided the longitudinal component of the magnetic field in the upper and middle chromosphere, while the Mn I lines provided it in the lower chromosphere.…”

Section: Introductionmentioning

confidence: 99%

Tomography of a Solar Plage with the Tenerife Inversion Code

Alemán

Bueno

et al. 2023

ApJ

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We apply the Tenerife Inversion Code (TIC) to the plage spectropolarimetric observations obtained by the Chromospheric LAyer SpectroPolarimeter (CLASP2). These unprecedented data consist of full Stokes profiles in the spectral region around the Mg ii h and k lines for a single slit position, with around two thirds of the 196″ slit crossing a plage region and the rest crossing an enhanced network. A previous analysis of these data had allowed us to infer the longitudinal component of the magnetic field by applying the weak-field approximation (WFA) to the circular polarization profiles, and to assign the inferred magnetic fields to different layers of the solar atmosphere based on the results of previous theoretical radiative transfer investigations. In this work, we apply the recently developed TIC to the same data. We obtain a stratified model atmosphere that fits the intensity and circular polarization profiles at each position along the spectrograph slit and we compare our results for the longitudinal component of the magnetic field with the previously obtained WFA results, highlighting the generally good agreement in spite of the fact that the WFA is known to produce an underestimation when applied to the outer lobes of the Mg ii h and k circular polarization profiles. Finally, we use the inverted model atmospheres to give a rough estimation of the energy that could be carried by Alfvén waves propagating in the chromosphere in the plage and network regions, showing that it is sufficient to compensate for the estimated energy losses in the chromosphere of solar active regions.

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The Circular Polarization of the Mn 1 Resonance Lines around 280 nm for Exploring Chromospheric Magnetism

Cited by 7 publications

References 22 publications

Magnetic Field Information in the Near-ultraviolet Fe ii Lines of the CLASP2 Space Experiment

Magnetic Field Information in the Near-ultraviolet Fe ii Lines of the CLASP2 Space Experiment

Tomography of a solar plage with the Tenerife Inversion Code

Tomography of a Solar Plage with the Tenerife Inversion Code

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