Multiple Stokes I inversions for inferring magnetic fields in the spectral range around Cr I 5782 angstrom

0548204 - ASÚ 2022 RIV FR eng J - Článek v odborném periodiku
Kuckein, C. - Balthasar, H. - Quintero Noda, C. - Diercke, A. - Trelles Arjona, J. C. - Ruiz Cobo, B. - Felipe, T. - Denker, C. - Verma, M. - Kontogiannis, I. - Sobotka, Michal
Multiple Stokes I inversions for inferring magnetic fields in the spectral range around Cr I 5782 angstrom.
Astronomy & Astrophysics. Roč. 653, September (2021), č. článku A165. ISSN 0004-6361. E-ISSN 1432-0746
GRANT EU: European Commission(XE) 824135 - SOLARNET
Institucionální podpora: RVO:67985815
Klíčová slova: 3-dimensional structure * oscillator-strengths * height dependence
Obor OECD: Astronomy (including astrophysics,space science)
Impakt faktor: 6.240, rok: 2021
Způsob publikování: Open access s časovým embargem
https://doi.org/10.1051/0004-6361/202140596

In this work, we explore the spectral window containing Fraunhofer lines formed in the solar photosphere, around the magnetically sensitive Cr i lines at 5780.9, 5781.1, 5781.7, 5783.0, and 5783.8 angstrom, with Lande g-factors between 1.6 and 2.5. The goal is to simultaneously analyze 15 spectral lines, comprising Cr i, Cu i, Fe i, Mn i, and Si i lines, without the use of polarimetry, to infer the thermodynamic and magnetic properties in strongly magnetized plasmas using an inversion code. The 15 simultaneously inverted intensity profiles (Stokes I) delivered accurate temperatures and Doppler velocities when compared with the simulations. The derived magnetic fields and inclinations achieve the best level of accuracy when the fields are oriented along the line-of-sight (LOS) and less accurate when the fields are transverse to the LOS. In general, the results appear similar to what is reported in the HMI vector-field data, although some discrepancies exist. The analyzed spectral range has the potential to deliver thermal, dynamic, and magnetic information for strongly magnetized features on the Sun, such as pores and sunspots, even without the use of polarimetry. The highest sensitivity of the lines is found in the lower photosphere, on average, around log tau = 1. The multiple-line inversions provide smooth results across the whole field of view (FOV). The presented spectral range and inversion strategy will be used for future VTT observing campaigns.
Trvalý link: http://hdl.handle.net/11104/0324308