IAA authors:
del Toro Iniesta, J. C.;Orozco Suárez, D.;Strecker, H.
Authors:
Chitta, L. P.;Solanki, S. K.;del Toro Iniesta, J. C.;Woch, J.;Calchetti, D.;Gandorfer, A.;Hirzberger, J.;Kahil, F.;Valori, G.;Orozco Suárez, D.;Strecker, H.;Appourchaux, T.;Volkmer, R.;Peter, H.;Mandal, S.;Aznar Cuadrado, R.;Teriaca, L.;Schühle, U.;Berghmans, D.;Verbeeck, C.;Zhukov, A. N.;Priest, E. R.
Journal:
Astrophysical Journal Letters
Abstract:
Arch-like loop structures filled with million Kelvin hot plasma form the building blocks of the quiet-Sun corona. Both high-resolution observations and magnetoconvection simulations show the ubiquitous presence of magnetic fields on the solar surface on small spatial scales of ~100 km. However, the question of how exactly these quiet-Sun coronal loops originate from the photosphere and how the magnetic energy from the surface is channeled to heat the overlying atmosphere is a long-standing puzzle. Here we report high-resolution photospheric magnetic field and coronal data acquired during the second science perihelion of Solar Orbiter that reveal a highly dynamic magnetic landscape underlying the observed quiet-Sun corona. We found that coronal loops often connect to surface regions that harbor fleeting weaker, mixed-polarity magnetic field patches structured on small spatial scales, and that coronal disturbances could emerge from these areas. We suggest that weaker magnetic fields with fluxes as low as 10<SUP>15</SUP> Mx and/or those that evolve on timescales less than 5 minutes are crucial to understanding the coronal structuring and dynamics.
URL:
https://ui.adsabs.harvard.edu/#abs/2023ApJ...956L...1C/abstract
Keywords:
Solar extreme ultraviolet emission;Solar photosphere;Solar coronal heating;Solar magnetic fields;Solar magnetic reconnection;Magnetohydrodynamics;Solar coronal loops;1493;1518;1989;1503;1504;1964;1485;Astrophysics - Solar and Stellar Astrophysics;Physics - Plasma Physics;Physics - Space Physics