skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: THE FORMATION OF IRIS DIAGNOSTICS. VI. THE DIAGNOSTIC POTENTIAL OF THE C ii LINES AT 133.5 nm IN THE SOLAR ATMOSPHERE

Abstract

We use 3D radiation magnetohydrodynamic models to investigate how the thermodynamic quantities in the simulation are encoded in observable quantities, thus exploring the diagnostic potential of the C ii 133.5 nm lines. We find that the line core intensity is correlated with the temperature at the formation height but the correlation is rather weak, especially when the lines are strong. The line core Doppler shift is a good measure of the line-of-sight velocity at the formation height. The line width is both dependent on the width of the absorption profile (thermal and non-thermal width) and an opacity broadening factor of 1.2–4 due to the optically thick line formation with a larger broadening for double peak profiles. The C ii 133.5 nm lines can be formed both higher and lower than the core of the Mg ii k line depending on the amount of plasma in the 14–50 kK temperature range. More plasma in this temperature range gives a higher C ii 133.5 nm formation height relative to the Mg ii k line core. The synthetic line profiles have been compared with Interface Region Imaging Spectrograph observations. The derived parameters from the simulated line profiles cover the parameter range seen inmore » observations but, on average, the synthetic profiles are too narrow. We interpret this discrepancy as a combination of a lack of plasma at chromospheric temperatures in the simulation box and too small non-thermal velocities. The large differences in the distribution of properties between the synthetic profiles and the observed ones show that the C ii 133.5 nm lines are powerful diagnostics of the upper chromosphere and lower transition region.« less

Authors:
; ;  [1];  [2]
  1. Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029 Blindern, NO-0315 Oslo (Norway)
  2. The Institute for Solar Physics, AlbaNova University Center, SE-106 91 Stockholm (Sweden)
Publication Date:
OSTI Identifier:
22525364
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 811; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; CARBON IONS; CHROMOSPHERE; COMPARATIVE EVALUATIONS; COMPUTERIZED SIMULATION; CORRELATIONS; DOPPLER EFFECT; LINE WIDTHS; MAGNESIUM IONS; MAGNETOHYDRODYNAMICS; OPACITY; PLASMA; RADIANT HEAT TRANSFER; SUN; ULTRAVIOLET RADIATION; VELOCITY

Citation Formats

Rathore, Bhavna, Carlsson, Mats, Pontieu, Bart De, and Leenaarts, Jorrit, E-mail: bhavna.rathore@astro.uio.no, E-mail: mats.carlsson@astro.uio.no, E-mail: bdp@lmsal.com, E-mail: jorrit.leenaarts@astro.su.se. THE FORMATION OF IRIS DIAGNOSTICS. VI. THE DIAGNOSTIC POTENTIAL OF THE C ii LINES AT 133.5 nm IN THE SOLAR ATMOSPHERE. United States: N. p., 2015. Web. doi:10.1088/0004-637X/811/2/81.
Rathore, Bhavna, Carlsson, Mats, Pontieu, Bart De, & Leenaarts, Jorrit, E-mail: bhavna.rathore@astro.uio.no, E-mail: mats.carlsson@astro.uio.no, E-mail: bdp@lmsal.com, E-mail: jorrit.leenaarts@astro.su.se. THE FORMATION OF IRIS DIAGNOSTICS. VI. THE DIAGNOSTIC POTENTIAL OF THE C ii LINES AT 133.5 nm IN THE SOLAR ATMOSPHERE. United States. doi:10.1088/0004-637X/811/2/81.
Rathore, Bhavna, Carlsson, Mats, Pontieu, Bart De, and Leenaarts, Jorrit, E-mail: bhavna.rathore@astro.uio.no, E-mail: mats.carlsson@astro.uio.no, E-mail: bdp@lmsal.com, E-mail: jorrit.leenaarts@astro.su.se. Thu . "THE FORMATION OF IRIS DIAGNOSTICS. VI. THE DIAGNOSTIC POTENTIAL OF THE C ii LINES AT 133.5 nm IN THE SOLAR ATMOSPHERE". United States. doi:10.1088/0004-637X/811/2/81.
@article{osti_22525364,
title = {THE FORMATION OF IRIS DIAGNOSTICS. VI. THE DIAGNOSTIC POTENTIAL OF THE C ii LINES AT 133.5 nm IN THE SOLAR ATMOSPHERE},
author = {Rathore, Bhavna and Carlsson, Mats and Pontieu, Bart De and Leenaarts, Jorrit, E-mail: bhavna.rathore@astro.uio.no, E-mail: mats.carlsson@astro.uio.no, E-mail: bdp@lmsal.com, E-mail: jorrit.leenaarts@astro.su.se},
abstractNote = {We use 3D radiation magnetohydrodynamic models to investigate how the thermodynamic quantities in the simulation are encoded in observable quantities, thus exploring the diagnostic potential of the C ii 133.5 nm lines. We find that the line core intensity is correlated with the temperature at the formation height but the correlation is rather weak, especially when the lines are strong. The line core Doppler shift is a good measure of the line-of-sight velocity at the formation height. The line width is both dependent on the width of the absorption profile (thermal and non-thermal width) and an opacity broadening factor of 1.2–4 due to the optically thick line formation with a larger broadening for double peak profiles. The C ii 133.5 nm lines can be formed both higher and lower than the core of the Mg ii k line depending on the amount of plasma in the 14–50 kK temperature range. More plasma in this temperature range gives a higher C ii 133.5 nm formation height relative to the Mg ii k line core. The synthetic line profiles have been compared with Interface Region Imaging Spectrograph observations. The derived parameters from the simulated line profiles cover the parameter range seen in observations but, on average, the synthetic profiles are too narrow. We interpret this discrepancy as a combination of a lack of plasma at chromospheric temperatures in the simulation box and too small non-thermal velocities. The large differences in the distribution of properties between the synthetic profiles and the observed ones show that the C ii 133.5 nm lines are powerful diagnostics of the upper chromosphere and lower transition region.},
doi = {10.1088/0004-637X/811/2/81},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 811,
place = {United States},
year = {2015},
month = {10}
}