The PDFI_SS Electric Field Inversion Software

Fisher, G. H.; Kazachenko, Maria D.; Welsch, B. T.; Sun, Xudong; Lumme, E.; Bercik, D. J.; DeRosa, Marc L.; Cheung, Mark C. M.

doi:10.3847/1538-4365/ab8303

Cited by 31 publications

(33 citation statements)

References 59 publications

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“…Photospheric Doppler velocity field data are also adopted to help investigate magnetic cancellation at a cPIL. The corrected velocity field data are available in the data series cgem.doppcal 720s, which are corrected for the differential rotation and the Solar Dynamics Observatory spacecraft velocity (see Section 4 of Fisher et al 2020). The convective blueshift is further subtracted from the corrected data, which is saved in the DOPPBIAS keyword of the header file (for a detailed discussion, see Welsch et al 2013).…”

Section: Discussion and Summarymentioning

confidence: 99%

Buildup of the Magnetic Flux Ropes in Homologous Solar Eruptions

Wang,

Liu,

Yang

et al. 2022

Preprint

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Homologous coronal mass ejections (CMEs) are an interesting phenomenon, and it is possible to investigate the formation of CMEs by comparing multi-CMEs under a homologous physical condition. AR 11283 had been present on the solar surface for several days when a bipole emerged on 2011 September 4. Its positive polarity collided with the pre-existing negative polarity belonging to a different bipole, producing recurrent solar activities along the polarity inversion line (PIL) between the colliding polarities, namely the so-called collisional PIL (cPIL). Our results show that a large amount of energy and helicity were built up in the form of magnetic flux ropes (MFRs), with recurrent release and accumulation processes. These MFRs were built up along the cPIL. A flux deficit method is adopted and shows that magnetic cancellation happens along the cPIL due to the collisional shearing scenario proposed by Chintzoglou et al.The total amount of canceled flux was ∼0.7×10 21 Mx with an uncertainty of ∼13.2% within the confidence region of the 30 • sun-center distance. The canceled flux amounts to 24% of the total unsigned flux of the bipolar magnetic region. The results show that the magnetic fields beside the cPIL are very sheared, and the average shear angle is above 70 • after the collision. The fast expansion of the twist kernels of the MFRs and the continuous eruptive activities are both driven by the collisional shearing process. These results are important for better understanding the buildup process of the MFRs associated with homologous solar eruptions.

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Section: Discussion and Summarymentioning

confidence: 99%

Buildup of the Magnetic Flux Ropes in Homologous Solar Eruptions

Wang,

Liu,

Yang

et al. 2022

Preprint

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“…Future studies could use this overlap period to develop line-of-sight proxies for the vector magnetic field maps or summary parameters and extend these proxies backward in time. Future studies could also supplement the SMARP and SHARP data with other curated data sets that characterize, for example, subsurface properties of emerging active regions (Schunker et al 2016), the surface electric field (Kazachenko et al 2014;Fisher et al 2020), and atmospheric phenomena (Galvez et al 2019).…”

Section: Discussionmentioning

confidence: 99%

SMARPs and SHARPs: Two Solar Cycles of Active Region Data

Bobra,

Wright,

Sun

et al. 2021

Preprint

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We present a new data product, called Space-Weather MDI Active Region Patches (SMARPs), derived from maps of the solar surface magnetic field taken by the Michelson Doppler Imager (MDI) aboard the Solar and Heliospheric Observatory (SoHO). Together with the Space-Weather HMI Active Region Patches (SHARPs), derived from similar maps taken by the Helioseismic and Magnetic Imager (HMI) aboard the Solar Dynamics Observatory, these data provide a continuous and seamless set of maps and keywords that describe every active region observed over the last two solar cycles, from 1996 to the present day. In this paper, we describe the SMARP data and compare it to the SHARP data.

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“…In this study, we performed a test to validate the PDFI SS electric field inversion method (Fisher et al 2020), using the photospheric data extracted from an interior-to-corona MHD simulation of the emergence of a twisted flux tube. Unlike the previous validation tests for the PDFI SS method that used just one snapshot of a rising flux tube in the solar interior (see, e.g.…”

Section: Discussionmentioning

confidence: 99%

“…Here we introduce the threshold to reduce the computational time and also for consistency with the previous studies. Moreover, magnetic field masks are used by the PDFI SS software when computing the Doppler contribution to the electric field (Fisher et al 2020). We performed several FLCT reconstructions with other threshold values (even one order of magnitude larger) and have not found a significant effect on the results.…”

Section: Flct Inversions Of Horizontal Flowsmentioning

confidence: 99%

“…Kazachenko et al (2014) found the best values for free parameters in the PDFI method and applied it to real solar data to study the evolution of the energy and magnetic helicity fluxes in a solar active region (Kazachenko et al 2015). Fisher et al (2020) further improved the PDFI method by including spherical geometry as well as switching to a more conservative staggered-grid description of variables, hence the new method name became PDFI SS .…”

Section: Introductionmentioning

confidence: 99%

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Validation of the PDFI_SS method for electric field inversions using a magnetic flux emergence simulation

Afanasyev,

Kazachenko,

Fan

et al. 2021

Preprint

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Knowledge of electric fields in the photosphere is required to calculate the electromagnetic energy flux through the photosphere and set up boundary conditions for data-driven magnetohydrodynamic (MHD) simulations of solar eruptions. Recently, the PDFI SS method for inversions of electric fields from a sequence of vector magnetograms and Doppler velocity measurements was improved to incorporate spherical geometry and a staggered-grid description of variables. The method was previously validated using synthetic data from anelastic MHD (ANMHD) simulations. In this paper, we further validate the PDFI SS method, using approximately one-hour long MHD simulation data of magnetic flux emergence from the upper convection zone into the solar atmosphere. We reconstruct photospheric electric fields and calculate the Poynting flux, and compare those to the actual values from the simulations. We find that the accuracy of the PDFI SS reconstruction is quite good during the emergence phase of the simulated ephemeral active region evolution and decreases during the shearing phase. Analysing our results, we conclude that the more complex nature of the evolution (compared to the previously studied ANMHD case) that includes the shearing evolution phase is responsible for the obtained accuracy decrease.

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The PDFI_SS Electric Field Inversion Software

Cited by 31 publications

References 59 publications

Buildup of the Magnetic Flux Ropes in Homologous Solar Eruptions

Buildup of the Magnetic Flux Ropes in Homologous Solar Eruptions

SMARPs and SHARPs: Two Solar Cycles of Active Region Data

Validation of the PDFI_SS method for electric field inversions using a magnetic flux emergence simulation

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