Magnetic Fields and Plasma Heating in the Sun’s Atmosphere

• DOI: 10.3847/1538-4357/ad0780
• Publication Date: 2024-01-09T10:55:32Z
• Authors: P. Judge; L. Kleint; R. Casini; A. G. de Wijn; T. Schad; A. Tritschler
• Keywords: Corona (planetary geology); Photosphere; Polarimeter

Abstract We use the first publicly available data from Daniel K. Inouye Solar Telescope to track magnetic connections solar photosphere into corona. scrutinize relationships between chromospheric magnetism and bright chromospheric, transition region, coronal plasmas. In 2022 June, Visible Spectro-Polarimeter (ViSP) instrument targeted unipolar network within a decaying active region. ViSP acquired rastered scans with longitudinal Zeeman sensitivities of 0.25 Mx cm −2 (Fe i, 630.2 nm) 0.5 (Ca ii, 854.2 nm). was operated in “low” resolution mode (0.″214 slit width, spectral <?CDATA ${ \mathcal R }\approx {\rm{70,000}}$?> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi class="MJX-tex-calligraphic" mathvariant="script">R</mml:mi> <mml:mo>≈</mml:mo> mathvariant="normal">70,000</mml:mi> </mml:math> ) produce polarization maps over common area 105″ × 50″. Data Dynamics Observatory Interface Region Imaging Spectrograph are combined ask: Why is only fraction emerging flux filled heated plasma? What elemental nature plasmas? No correlations were found plasma properties fields derived weak field approximation, on scales below supergranules. Processes hidden our observations control heating. While improved measurements needed, these indicate that “the corona self-regulating forced system.” Heating depends state corona, not simply boundary conditions. models based upon identifiable bipolar fields, including cool loops, tectonics, observable reconnection, refuted for regions fields.