Magnetic helicity and eruptivity in active region 12673
K Moraitis, X Sun, É Pariat, L Linan - Astronomy & Astrophysics, 2019 - aanda.org
Context. In September 2017, the largest X-class flare of solar cycle 24 occurred from the most
active region (AR) of this cycle, AR 12673. This AR attracted much interest because of its …
active region (AR) of this cycle, AR 12673. This AR attracted much interest because of its …
Using relative field line helicity as an indicator for solar eruptivity
… values of E div /E have on our results. The original sample of 22 flares for which E div /E
< 0.05 is denoted as S2 in this Appendix. When we increase the threshold to E div /E < 0.085, …
< 0.05 is denoted as S2 in this Appendix. When we increase the threshold to E div /E < 0.085, …
Relative magnetic field line helicity
… As an application to solar situations, we compared the morphology of field line helicity on
the photosphere with that of the connectivity-based helicity flux density in two reconstructions of …
the photosphere with that of the connectivity-based helicity flux density in two reconstructions of …
Computation of relative magnetic helicity in spherical coordinates
K Moraitis, É Pariat, A Savcheva, G Valori - Solar Physics, 2018 - Springer
… used to estimate non-solenoidality (Pariat et al., 2015; Valori et al., 2016; Pariat et al., 2017;
Polito et al., 2017). Table 1 shows that the low values of \(E_{\mathrm{div}}/E\) are again an …
Polito et al., 2017). Table 1 shows that the low values of \(E_{\mathrm{div}}/E\) are again an …
Relative field line helicity of a large eruptive solar active region
… which is a measure of how much a numerical model of a magnetic field deviates from
solenoidality; lower values of E div , and consequently of the energy ratio E div /E, indicate a less …
solenoidality; lower values of E div , and consequently of the energy ratio E div /E, indicate a less …
Validation and benchmarking of a practical free magnetic energy and relative magnetic helicity budget calculation in solar magnetic structures
… It then follows from Equation (5) that the difference between E c and \(E'_{\… Pariat (2012):
we first choose the gauge \(\hat{z}\cdot\mathbf{A}=0\) throughout \(\mathcal{V}\), so that the x …
we first choose the gauge \(\hat{z}\cdot\mathbf{A}=0\) throughout \(\mathcal{V}\), so that the x …
Energy and helicity evolution in a flux emergence simulation
K Moraitis, V Archontis, G Chouliaras - arXiv preprint arXiv:2409.02445, 2024 - aanda.org
Aims. The main aim of this work is to study the evolution of the recently introduced relative
helicity of the magnetic polarity inversion line (PIL) in a magnetohydrodynamics simulation. …
helicity of the magnetic polarity inversion line (PIL) in a magnetohydrodynamics simulation. …
An observationally-driven kinetic approach to coronal heating
Aims. Coronal heating through the explosive release of magnetic energy remains an open
problem in solar physics. Recent hydrodynamical models attempt an investigation by placing …
problem in solar physics. Recent hydrodynamical models attempt an investigation by placing …
Magnetic helicity estimations in models and observations of the solar magnetic field. IV. Application to solar observations
…, F Chen, Y Guo, K Moraitis… - The Astrophysical …, 2021 - iopscience.iop.org
… The FI methods used in this study include that of Pariat et al. (… (E F ) at those times composes
about 14%, 6%, and 2% of E p , respectively. Correspondingly, we find a higher value of E F …
about 14%, 6%, and 2% of E p , respectively. Correspondingly, we find a higher value of E F …
Energy and helicity fluxes in line-tied eruptive simulations
L Linan, É Pariat, G Aulanier, K Moraitis… - Astronomy & …, 2020 - aanda.org
… Unlike E v , E p is a conserved quantity in … to E v , H j to E j , H pj to E p . This is particularly
visible for the current-carrying helicity and the free energy: when H j increases (decreases), E j …
visible for the current-carrying helicity and the free energy: when H j increases (decreases), E j …