Stereoscopic disambiguation of vector magnetograms: First applications to SO/PHI-HRT data

Valori, G.; Calchetti, D.; Moreno Vacas, A.; Pariat, É.; Solanki, S. K.; Löschl, P.; Hirzberger, J.; Parenti, S.; Albert, K.; Albelo Jorge, N.; Álvarez-Herrero, A.; Appourchaux, T.; Bellot Rubio, L. R.; Blanco Rodríguez, J.; Campos-Jara, A.; Feller, A.; Gandorfer, A.; García Parejo, P.; Germerott, D.; Gizon, L.; Gómez Cama, J. M.; Guerrero, L.; Gutierrez-Marques, P.; Kahil, F.; Kolleck, M.; Korpi-Lagg, A.; Orozco Suárez, D.; Pérez-Grande, I.; Sanchis Kilders, E.; Schou, J.; Schühle, U.; Sinjan, J.; Staub, J.; Strecker, H.; del Toro Iniesta, J. C.; Volkmer, R.; Woch, J.

doi:10.1051/0004-6361/202345859

Cited by 4 publications

(1 citation statement)

References 34 publications

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“…Measurements of the magnetic field in prominences are quite limited and have important uncertainties. For instance, the line of sight, the different height in the atmosphere where the spectral lines are formed and the 180 • ambiguity, can all affect the polarimetric diagnostics [76]. Another limitation up to now is given by the sensitivity of polarimetric instruments, which should be high enough to be able to measure the weak magnetic field in prominences (one to a few tens of Gauss for quiescent prominences, [31,67]) with a relatively high cadence, as done for measuring the temporal variation of the plasma parameters.…”

Section: Observational Evidence Of Pip In Prominences: Current Insightsmentioning

confidence: 99%

Future prospects for partially ionized solar plasmas: the prominence case

Parenti,

Luna,

Ballester

2024

Phil. Trans. R. Soc. A.

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Partially ionized plasmas (PIP) constitute an essential ingredient of our plasma universe. Historically, the physical effects associated with partial ionization were considered in astrophysical topics such as the interstellar medium, molecular clouds, accretion disks and, later on, in solar physics. PIP can be found in layers of the Sun’s atmosphere as well as in solar structures embedded within it. As a consequence, the dynamical behaviour of these layers and structures is influenced by the different physical effects introduced by partial ionization. Here, rather than considering an exhaustive discussion of partially ionized effects in the different layers and structures of the solar atmosphere, we focus on solar prominences. The reason is that they represent a paradigmatic case of a partially ionized solar plasma, confined and insulated by the magnetic field, constituting an ideal environment to study the effects induced by partial ionization. We present the current knowledge about the effects of partial ionization in the global stability, mass cycle and dynamics of solar prominences. We revise the identified observational signatures of partial ionization in prominences. We conclude with prospects for PIP research in prominences, proposing the path for advancing in the prominence modelling and theory and using new and upcoming instrumentation. This article is part of the theme issue ‘Partially ionized plasma of the solar atmosphere: recent advances and future pathways’.

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Section: Observational Evidence Of Pip In Prominences: Current Insightsmentioning

confidence: 99%

Future prospects for partially ionized solar plasmas: the prominence case

Parenti,

Luna,

Ballester

2024

Phil. Trans. R. Soc. A.

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A multiple spacecraft detection of the 2 April 2022 M-class flare and filament eruption during the first close Solar Orbiter perihelion

Janvier,

Mzerguat,

Young

et al. 2023

A&A

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Context. The Solar Orbiter mission completed its first remote-sensing observation windows in the spring of 2022. On 2 April 2022, an M-class flare followed by a filament eruption was seen both by the instruments on board the mission and from several observatories in Earth’s orbit, providing an unprecedented view of a flaring region with a large range of observations. Aims. We aim to understand the nature of the flaring and filament eruption events via the analysis of the available dataset. The complexity of the observed features is compared with the predictions given by the standard flare model in 3D. Methods. In this paper, we use the observations from a multi-view dataset, which includes extreme ultraviolet (EUV) imaging to spectroscopy and magnetic field measurements. These data come from the Interface Region Imaging Spectrograph, the Solar Dynamics Observatory, Hinode, as well as several instruments on Solar Orbiter. Results. The large temporal coverage of the region allows us to analyse the whole sequence of the filament eruption starting with its pre-eruptive state. Information given by spectropolarimetry from SDO/HMI and Solar Orbiter PHI/HRT shows that a parasitic polarity emerging underneath the filament is responsible for bringing the flux rope to an unstable state. As the flux rope erupts, Hinode EIS captures blue-shifted emission in the transition region and coronal lines in the northern leg of the flux rope prior to the flare peak. This may be revealing the unwinding of one of the flux rope legs. At the same time, Solar Orbiter SPICE captures the whole region, complementing the Doppler diagnostics of the filament eruption. Analyses of the formation and evolution of a complex set of flare ribbons and loops, of the hard and soft X-ray emissions with STIX, show that the parasitic emerging bipole plays an important role in the evolution of the flaring region. Conclusions. The extensive dataset covering this M-class flare event demonstrates how important multiple viewpoints and varied observations are in order to understand the complexity of flaring regions. While the analysed data are overall consistent with the standard flare model, the present particular magnetic configuration shows that surrounding magnetic activity such as nearby emergence needs to be taken into account to fully understand the processes at work. This filament eruption is the first to be covered from different angles by spectroscopic instruments, and provides an unprecedented diagnostic of the multi-thermal structures present before and during the flare. This complete dataset of an eruptive event showcases the capabilities of coordinated observations with the Solar Orbiter mission.

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Comparison of magnetic data products from Solar Orbiter SO/PHI-FDT and SDO/HMI

Moreno Vacas,

Orozco Suárez,

Strecker

et al. 2024

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The Polarimetric and Helioseismic Imager (SO/PHI), on board the Solar Orbiter mission, is the first photospheric magnetograph and tachograph to observe the Sun from outside the Sun-Earth line. The Full Disc Telescope (FDT) of SO/PHI, images the whole solar disk with a spatial resolution that varies with the distance between the Sun and the spacecraft. To check for consistency between the magnetic field strength ($B$), the field inclination (gamma ), the line-of-sight (LoS) magnetic component ($B_ LoS $) and the field azimuth (phi ), inferred by SO/PHI-FDT and the Helioseismic and Magnetic Imager (HMI), on board Solar Dynamics Observatory (SDO), and obtain linear correlation coefficients among them. We use data from both instruments obtained on 8 March 2022, when the angle between SDO and Solar Orbiter was $3.4^ circ $ and the solar disk showed four developed active regions. Before comparing the magnetic field products of both instruments we perform a precise alignment of the data, including a matching of the plate scale. Further, in order to improve the homogeneity of the compared data products, the SDO/HMI data were convolved with the SO/PHI-FDT point spread function (PSF). The linear correlation coefficients are obtained through a linear regression of SDO/HMI to SO/PHI-FDT. The two instruments yield comparable magnetic field data products. The slope coefficients for a linear fit are 1.37 for $B$, 1.11 for gamma , 1.35 for $B_ LoS $ and 1 for the azimuth. The corresponding fit offsets are $-94$ G, $-9.8^ circ $, $5.2$ G and $0.1^ circ $, respectively. The agreement between both instruments is significantly better when we take into account the different spatial resolution of both instruments. The fitting results vary slightly depending on the analyzed active region except for one of the four active regions, which shows larger differences and has been excluded from the comparison. The comparison of the LoS magnetic field products from SDO/HMI at 45 s and 720 s with SO/PHI-FDT shows a slope value of 1.17, with the offset less than $6$ G, in both cases.

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Stereoscopic disambiguation of vector magnetograms: First applications to SO/PHI-HRT data

Cited by 4 publications

References 34 publications

Future prospects for partially ionized solar plasmas: the prominence case

Future prospects for partially ionized solar plasmas: the prominence case

A multiple spacecraft detection of the 2 April 2022 M-class flare and filament eruption during the first close Solar Orbiter perihelion

Comparison of magnetic data products from Solar Orbiter SO/PHI-FDT and SDO/HMI

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