Net radiative cooling rates and partial ionization in cool coronal condensations

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F25%3A00637344" target="_blank" >RIV/67985815:_____/25:00637344 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0368251" target="_blank" >https://hdl.handle.net/11104/0368251</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202553909" target="_blank" >10.1051/0004-6361/202553909</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Net radiative cooling rates and partial ionization in cool coronal condensations

Popis výsledku v původním jazyce

We provide tabulated net radiative cooling rates (NRCRs) in the plasma of cool coronal condensations, together with the electron densities and ionization degrees describing its partial ionization. These readily applicable rates result from combined effects of the radiative cooling and radiative heating in the dominant atomic transitions in hydrogen, Mg II , and Ca II . Methods. These NRCRs represent realistic estimates based on 1D non-LTE (i.e. departures from the local thermodynamic equilibrium) radiative transfer modelling that uses 1D isothermal and isobaric prominence models. To construct easy-to-use NRCR tables, we employed the concept of voxels (volume pixels), which allowed us to incorporate the essential information about the location of the modelled plasma with respect to the source of illumination. We provide tabulated values of NRCRs, electron densities, and ionization degrees for a broad range of plasma parameters representing a wide variety of cool coronal condensations, such as prominences, cool coronal loops, spicules, jets, and coronal rain. Results. The accuracy of the provided voxel-based NRCRs, when tested against non-LTE calculations, is high, often showing a difference of only a few per cent. However, in some cases, the differences increase by up to a factor of two, which is the consequence of the assumptions and simplifications adopted here. Despite such differences, the voxel-based NRCRs that incorporate both the optically thick and thin radiative processes are a significant improvement, compared to the optically thin radiative loss formulas, when dealing with the cool plasmas at temperatures below 30 000 K. Conclusions. The provided NRCRs are tabulated for three different scenarios of the orientation of the modelled structure with respect to the source of illumination: (i) a vertical orientation where a surface receives illumination from one half of the solar disc, (ii) a horizontal orientation where the bottom surface receives illumination from the entire solar disc, and (iii) a horizontal orientation where the top surface does not receive any illumination from the solar disc. This allows the voxel-based NRCRs to be implemented even in complex multi-dimensional simulations of cool coronal condensations.

Název v anglickém jazyce

Net radiative cooling rates and partial ionization in cool coronal condensations

Popis výsledku anglicky

We provide tabulated net radiative cooling rates (NRCRs) in the plasma of cool coronal condensations, together with the electron densities and ionization degrees describing its partial ionization. These readily applicable rates result from combined effects of the radiative cooling and radiative heating in the dominant atomic transitions in hydrogen, Mg II , and Ca II . Methods. These NRCRs represent realistic estimates based on 1D non-LTE (i.e. departures from the local thermodynamic equilibrium) radiative transfer modelling that uses 1D isothermal and isobaric prominence models. To construct easy-to-use NRCR tables, we employed the concept of voxels (volume pixels), which allowed us to incorporate the essential information about the location of the modelled plasma with respect to the source of illumination. We provide tabulated values of NRCRs, electron densities, and ionization degrees for a broad range of plasma parameters representing a wide variety of cool coronal condensations, such as prominences, cool coronal loops, spicules, jets, and coronal rain. Results. The accuracy of the provided voxel-based NRCRs, when tested against non-LTE calculations, is high, often showing a difference of only a few per cent. However, in some cases, the differences increase by up to a factor of two, which is the consequence of the assumptions and simplifications adopted here. Despite such differences, the voxel-based NRCRs that incorporate both the optically thick and thin radiative processes are a significant improvement, compared to the optically thin radiative loss formulas, when dealing with the cool plasmas at temperatures below 30 000 K. Conclusions. The provided NRCRs are tabulated for three different scenarios of the orientation of the modelled structure with respect to the source of illumination: (i) a vertical orientation where a surface receives illumination from one half of the solar disc, (ii) a horizontal orientation where the bottom surface receives illumination from the entire solar disc, and (iii) a horizontal orientation where the top surface does not receive any illumination from the solar disc. This allows the voxel-based NRCRs to be implemented even in complex multi-dimensional simulations of cool coronal condensations.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA25-18282S" target="_blank" >GA25-18282S: Kosmické koronografy ESA s českou účastí</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2025

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

699

Číslo periodika v rámci svazku

July

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

29

Strana od-do

A89

Kód UT WoS článku

001522098000002

EID výsledku v databázi Scopus

2-s2.0-105009896301