A solar coronal loop in a box: Energy generationand heating (<i>Corrigendum</i>)

Breu, C.; Peter, H.; Cameron, R.; Solanki, S. K.; D., Przybylski,; Rempel, M.; Chitta, L. P.

doi:10.1051/0004-6361/202141451e

Cited by 1 publication

(3 citation statements)

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“…In the MURaM simulations, the vertical Poynting flux at 1 t = is just above the S z,thr value from Withbroe & Noyes (1977). This is consistent with existing MURaM simulations, where the hot corona is maintained by photospheric magnetoconvection (Rempel 2017;Breu et al 2022Breu et al , 2023. However, we find that in IMaX observations, there is not enough Poynting flux whether we use the ideal MHD method or PDFI_SS, unless we consider only strong B-field pixels in the ideal MHD case (Figure 8).…”

Section: Discussionsupporting

confidence: 88%

“…However, those simulations have lower resolution and the Poynting flux comes more from the braiding of the QS network field, which is mostly absent in our simulation set. MURaM simulations of coronal loops also show that photospheric energy output is sufficient to maintain a hot corona (Breu et al 2022(Breu et al , 2023.…”

Section: Discussionmentioning

confidence: 95%

“…Significant strides have been made in both magnetic field inversions from observed Stokes profiles (Asensio Ramos & Díaz Baso 2019; de la Cruz Rodríguez 2019), and electric field inversions (e.g., Welsch & Fisher 2016;Fisher et al 2020). However, most of the quantitative studies of Poynting flux have been constrained to either simulated data (Shelyag et al 2012;Kazachenko et al 2014;Afanasyev et al 2021;Breu et al 2022Breu et al , 2023, or active regions and plages (Kazachenko et al 2015;Lumme et al 2019), since in these settings one deals with relatively high polarimetric signal-to-noise ratios (S/Ns). In particular, Breu et al (2022) used high-fidelity simulations of the quiet Sun (QS) photosphere to explain heating in a coronal loop, while Kazachenko et al (2015) computed Poynting flux from Active Region 11158 and found it to be sufficient to explain the heating of the chromosphere and corona, according to theoretical estimates in Withbroe & Noyes (1977).…”

Section: Introductionmentioning

confidence: 99%

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Quantifying Poynting Flux in the Quiet Sun Photosphere

Tilipman,

Kazachenko,

Tremblay

et al. 2023

ApJ

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Poynting flux is the flux of magnetic energy, which is responsible for chromospheric and coronal heating in the solar atmosphere. It is defined as a cross product of the electric and magnetic fields, and in ideal MHD conditions it can be expressed in terms of the magnetic field and plasma velocity. Poynting flux has been computed for active regions and plages, but estimating it in the quiet Sun (QS) remains challenging due to resolution effects and polarimetric noise. However, with the upcoming DKIST capabilities, such estimations will become more feasible than ever before. Here, we study QS Poynting flux in SUNRISE/IMaX observations and MURaM simulations. We explore two methods for inferring transverse velocities from observations—FLCT and a neural network–based method DeepVel—and show DeepVel to be the more suitable method in the context of small-scale QS flows. We investigate the effect of azimuthal ambiguity on Poynting flux estimates, and we describe a new method for azimuth disambiguation. Finally, we use two methods for obtaining the electric field. The first method relies on an idealized Ohm’s law, whereas the second is a state-of-the-art inductive electric field inversion method PDFI_SS. We compare the resulting Poynting flux values with theoretical estimates for chromospheric and coronal energy losses and find that some of the Poynting flux estimates are sufficient to match the losses. Using MURaM simulations, we show that photospheric Poynting fluxes vary significantly with optical depth, and that there is an observational bias that results in underestimated Poynting fluxes due to an unaccounted shear term contribution.

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