Numerical Simulations and Observations of Mg ii in the Solar Chromosphere

The Mg ii h and k lines are among the best diagnostic tools of the upper solar chromosphere. This region of the atmosphere is of particular interest, as it is the lowest region of the Sun’s atmosphere where the magnetic field is dominant in the energetics and dynamics, defining its structure. While...
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Gespeichert in:

Autor*in:	Viggo H. Hansteen [verfasserIn] Juan Martinez-Sykora [verfasserIn] Mats Carlsson [verfasserIn] Bart De Pontieu [verfasserIn] Milan Gošić [verfasserIn] Souvik Bose [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Solar chromosphere Solar chromospheric heating Solar magnetic flux emergence Radiative magnetohydrodynamics

Übergeordnetes Werk:	In: The Astrophysical Journal - IOP Publishing, 2022, 944(2023), 2, p 131
Übergeordnetes Werk:	volume:944 ; year:2023 ; number:2, p 131

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4357/acb33c

Katalog-ID:	DOAJ089162110

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source	In The Astrophysical Journal 944(2023), 2, p 131 volume:944 year:2023 number:2, p 131
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authorswithroles_txt_mv	Viggo H. Hansteen @@aut@@ Juan Martinez-Sykora @@aut@@ Mats Carlsson @@aut@@ Bart De Pontieu @@aut@@ Milan Gošić @@aut@@ Souvik Bose @@aut@@
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callnumber-first	Q - Science
author	Viggo H. Hansteen
spellingShingle	Viggo H. Hansteen misc QB460-466 misc Solar chromosphere misc Solar chromospheric heating misc Solar magnetic flux emergence misc Radiative magnetohydrodynamics misc Astrophysics Numerical Simulations and Observations of Mg ii in the Solar Chromosphere
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topic_title	QB460-466 Numerical Simulations and Observations of Mg ii in the Solar Chromosphere Solar chromosphere Solar chromospheric heating Solar magnetic flux emergence Radiative magnetohydrodynamics
topic	misc QB460-466 misc Solar chromosphere misc Solar chromospheric heating misc Solar magnetic flux emergence misc Radiative magnetohydrodynamics misc Astrophysics
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title	Numerical Simulations and Observations of Mg ii in the Solar Chromosphere
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title_full	Numerical Simulations and Observations of Mg ii in the Solar Chromosphere
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title_sort	numerical simulations and observations of mg ii in the solar chromosphere
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title_auth	Numerical Simulations and Observations of Mg ii in the Solar Chromosphere
abstract	The Mg ii h and k lines are among the best diagnostic tools of the upper solar chromosphere. This region of the atmosphere is of particular interest, as it is the lowest region of the Sun’s atmosphere where the magnetic field is dominant in the energetics and dynamics, defining its structure. While highly successful in the photosphere and lower to mid-chromosphere, numerical models have produced synthetic Mg ii lines that do not match the observations well. We present a number of large-scale models with magnetic field topologies representative of the quiet Sun, ephemeral flux regions and plage, and also models where the numerical resolution is high and where we go beyond the MHD paradigm. The results of this study show models with a much improved correspondence with IRIS observations in terms of both intensities and widths, especially underscoring the importance of chromospheric mass loading and of capturing the magnetic field topology and evolution in simulations. This comes in addition to the importance of capturing the generation of small-scale velocity fields and including nonequilibrium ionization and ion−neutral interaction effects. However, it should be noted that difficulties in achieving a good correspondence remain, especially when considering the width of Mg ii h and k lines in plage. Understanding and modeling all these effects and their relative importance is necessary in order to reproduce observed spectral features and in isolating the missing pieces necessary to fully comprehend Mg ii formation.
abstractGer	The Mg ii h and k lines are among the best diagnostic tools of the upper solar chromosphere. This region of the atmosphere is of particular interest, as it is the lowest region of the Sun’s atmosphere where the magnetic field is dominant in the energetics and dynamics, defining its structure. While highly successful in the photosphere and lower to mid-chromosphere, numerical models have produced synthetic Mg ii lines that do not match the observations well. We present a number of large-scale models with magnetic field topologies representative of the quiet Sun, ephemeral flux regions and plage, and also models where the numerical resolution is high and where we go beyond the MHD paradigm. The results of this study show models with a much improved correspondence with IRIS observations in terms of both intensities and widths, especially underscoring the importance of chromospheric mass loading and of capturing the magnetic field topology and evolution in simulations. This comes in addition to the importance of capturing the generation of small-scale velocity fields and including nonequilibrium ionization and ion−neutral interaction effects. However, it should be noted that difficulties in achieving a good correspondence remain, especially when considering the width of Mg ii h and k lines in plage. Understanding and modeling all these effects and their relative importance is necessary in order to reproduce observed spectral features and in isolating the missing pieces necessary to fully comprehend Mg ii formation.
abstract_unstemmed	The Mg ii h and k lines are among the best diagnostic tools of the upper solar chromosphere. This region of the atmosphere is of particular interest, as it is the lowest region of the Sun’s atmosphere where the magnetic field is dominant in the energetics and dynamics, defining its structure. While highly successful in the photosphere and lower to mid-chromosphere, numerical models have produced synthetic Mg ii lines that do not match the observations well. We present a number of large-scale models with magnetic field topologies representative of the quiet Sun, ephemeral flux regions and plage, and also models where the numerical resolution is high and where we go beyond the MHD paradigm. The results of this study show models with a much improved correspondence with IRIS observations in terms of both intensities and widths, especially underscoring the importance of chromospheric mass loading and of capturing the magnetic field topology and evolution in simulations. This comes in addition to the importance of capturing the generation of small-scale velocity fields and including nonequilibrium ionization and ion−neutral interaction effects. However, it should be noted that difficulties in achieving a good correspondence remain, especially when considering the width of Mg ii h and k lines in plage. Understanding and modeling all these effects and their relative importance is necessary in order to reproduce observed spectral features and in isolating the missing pieces necessary to fully comprehend Mg ii formation.
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title_short	Numerical Simulations and Observations of Mg ii in the Solar Chromosphere
url	https://doi.org/10.3847/1538-4357/acb33c https://doaj.org/article/99deab86000a4f25b36edf163aaf749f https://doaj.org/toc/1538-4357
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Numerical Simulations and Observations of Mg ii in the Solar Chromosphere

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