Coronal Heating Rate in the Slow Solar Wind

0576566 - ASÚ 2024 RIV US eng J - Článek v odborném periodiku
Telloni, D. - Romoli, M. - Velli, M. - Heinzel, Petr … celkem 62 autorů
Coronal Heating Rate in the Slow Solar Wind.
Astrophysical Journal Letters. Roč. 955, č. 1 (2023), č. článku L4. ISSN 2041-8205. E-ISSN 2041-8213
Institucionální podpora: RVO:67985815
Klíčová slova: magnetohydrodynamics * interplanetary turbulence * solar corona
Obor OECD: Astronomy (including astrophysics,space science)
Impakt faktor: 7.9, rok: 2022
Způsob publikování: Open access

This Letter reports the first observational estimate of the heating rate in the slowly expanding solar corona. The analysis exploits the simultaneous remote and local observations of the same coronal plasma volume, with the Solar Orbiter/Metis and the Parker Solar Probe instruments, respectively, and relies on the basic solar wind magnetohydrodynamic equations. As expected, energy losses are a minor fraction of the solar wind energy flux, since most of the energy dissipation that feeds the heating and acceleration of the coronal flow occurs much closer to the Sun than the heights probed in the present study, which range from 6.3 to 13.3 R & ODOT. The energy deposited to the supersonic wind is then used to explain the observed slight residual wind acceleration and to maintain the plasma in a nonadiabatic state. As derived in the Wentzel-Kramers-Brillouin limit, the present energy transfer rate estimates provide a lower limit, which can be very useful in refining the turbulence-based modeling of coronal heating and subsequent solar wind acceleration.
Trvalý link: https://hdl.handle.net/11104/0347336