Počet záznamů: 1
Evaluating the Reliability of a Simple Method to Map the Magnetic Field Azimuth in the Solar Chromosphere
- 1.
SYSNO ASEP 0548095 Druh ASEP J - Článek v odborném periodiku Zařazení RIV J - Článek v odborném periodiku Poddruh J Článek ve WOS Název Evaluating the Reliability of a Simple Method to Map the Magnetic Field Azimuth in the Solar Chromosphere Tvůrce(i) Jurčák, Jan (ASU-R) RID, ORCID
Štěpán, Jiří (ASU-R) RID, ORCID
Trujillo Bueno, J. (ES)Číslo článku 23 Zdroj.dok. Astrophysical Journal - ISSN 0004-637X
Roč. 911, č. 1 (2021)Poč.str. 6 s. Forma vydání Online - E Jazyk dok. eng - angličtina Země vyd. US - Spojené státy americké Klíč. slova solar chromosphere ; polarimetry ; astronomy data analysis Vědní obor RIV BN - Astronomie a nebeská mechanika, astrofyzika Obor OECD Astronomy (including astrophysics,space science) CEP GA19-20632S GA ČR - Grantová agentura ČR Způsob publikování Open access Institucionální podpora ASU-R - RVO:67985815 UT WOS 000639521900001 EID SCOPUS 85104664192 DOI 10.3847/1538-4357/abe402 Anotace The Zeeman effect is of limited utility for probing the magnetism of the quiet solar chromosphere. The Hanle effect in some spectral lines is sensitive to such magnetism, but the interpretation of the scattering polarization signals requires taking into account that the chromospheric plasma is highly inhomogeneous and dynamic (i.e., that the magnetic field is not the only cause of symmetry breaking). Here we investigate the reliability of a well-known formula for mapping the azimuth of chromospheric magnetic fields directly from the scattering polarization observed in the Ca ii 8542 A line, which is typically in the saturation regime of the Hanle effect. To this end, we use the Stokes profiles of the Ca ii 8542 A line computed with the PORTA radiative transfer code in a three-dimensional (3D) model of the solar chromosphere, degrading them to mimic spectropolarimetric observations for a range of telescope apertures and noise levels. The simulated observations are used to obtain the magnetic field azimuth at each point of the field of view, which we compare with the actual values within the 3D model. We show that, apart from intrinsic ambiguities, the method provides solid results. Their accuracy depends more on the noise level than on the telescope diameter. Large-aperture solar telescopes, like DKIST and EST, are needed to achieve the required polarimetric sensitivity using reasonable exposure times. Pracoviště Astronomický ústav Kontakt Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Rok sběru 2022 Elektronická adresa http://hdl.handle.net/11104/0324210
Počet záznamů: 1