First perihelion of EUI on the Solar Orbiter mission

Berghmans, D.; Antolin, P.; F., Auchere,; Cuadrado, R. Aznar; Barczynski, K.; Chitta, L. P.; S., Gissot,; Harra, L.; Huang, Z.; Janvier, M.; Kraaikamp, E.; Long, D. M; Mandal, S.; Mierla, M.; Parenti, S.; Peter, H.; Rodriguez, L.; Schuhle, U.; Smith, P.J.

doi:10.1051/0004-6361/202245586

Cited by 18 publications

(3 citation statements)

References 64 publications

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“…On 7 March 2022, Solar Orbiter was located half way to the Sun (0.5 AU), and the angular separation between the spacecraft and the Earth was 3.01 • . Solar Orbiter was carrying out its first full science perihelion (Berghmans et al 2023). A20, page 2 of 10…”

Section: Discussionmentioning

confidence: 99%

The source of unusual coronal upflows with photospheric abundance in a solar active region

Harra¹,

Mandrini²,

Brooks³

et al. 2023

A&A

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Context. Upflows in the corona are of importance, as they may contribute to the solar wind. There has been considerable interest in upflows from active regions (ARs). The coronal upflows that are seen at the edges of active regions have coronal elemental composition and can contribute to the slow solar wind. The sources of the upflows have been challenging to determine because they may be multiple, and the spatial resolution of previous observations is not yet high enough. Aims. In this article, we analyse coronal upflows in AR 12960 that are unusually close to the sunspot umbra. We analyse their properties, and we attempt to determine if it is possible that they feed into the slow solar wind. Methods. We analysed the activity in the upflow region in detail using a combination of Solar Orbiter EUV images at high spatial and temporal resolution, Hinode/EUV Imaging Spectrometer data, and observations from instruments on board the Solar Dynamics Observatory. This combined dataset was acquired during the first Solar Orbiter perihelion of the science phase, which provided a spatial resolution of 356 km for two pixels. Doppler velocity, density, and plasma composition determinations, as well as coronal magnetic field modelling, were carried out to understand the source of the upflows. Results. We observed small magnetic fragments, called moving magnetic features (MMFs), moving away from the sunspot in the active region. Specifically, they moved towards the sunspot from the edge of the penumbra where a small positive polarity connects to the umbra via small-scale and very dynamic coronal loops. At this location, small dark grains are evident and flow along penumbral filaments in continuum images. The magnetic field modelling showed small low-lying loops anchored close to the umbral magnetic field. The high-resolution data of the Solar Orbiter EUV Imagers showed the dynamics of these small loops, which last on time scales of only minutes. The edges of these small loops are the location of the coronal upflow that has photospheric abundance.

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Section: Discussionmentioning

confidence: 99%

The source of unusual coronal upflows with photospheric abundance in a solar active region

Harra¹,

Mandrini²,

Brooks³

et al. 2023

A&A

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“…During the Solar Orbiter perihelion at around 0.29 AU, this instrument records the dynamics of the solar atmosphere at a maximum of 3 s cadence with a spatial resolution of about 200 km. This waveband has already shown great capability of resolving prominence fine structure [92]. This can be used to study the dynamic nature of threads and inferring, using seismology diagnostics, magnetic field strength at such small scales [93].…”

Section: Prospects For Future Researchmentioning

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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“…In particular, we used data of the High Resolution Imager at 174 Å (HRI EUV ), which samples plasma with a temperature T of ∼1 MK. The EUI data 1 were obtained on 2022 March 4 between 10:48-11:48 UT when Solar Orbiter was located 0.54 AU away from the Sun and was about 7 • east in solar longitude from the Sun-Earth line, with a pixel size of 0.492 and a time cadence of 5 s (Berghmans et al 2023). At the time of these observations, one pixel size corresponds to approximately 190 km on the Sun.…”

Section: Datamentioning

confidence: 99%

Evidence of external reconnection between an erupting mini-filament and ambient loops observed by Solar Orbiter/EUI

Cheng

Ding

et al. 2023

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Mini-filament eruptions are one of the most common small-scale transients in the solar atmosphere. However, their eruption mechanisms are still not understood thoroughly. Here, with a combination of 174 Å images of high spatio-temporal resolution taken by the Extreme Ultraviolet Imager on board Solar Orbiter and images of the Atmospheric Imaging Assembly on board Solar Dynamics Observatory, we investigate in detail an erupting mini-filament over a weak magnetic field region on 2022 March 4. Two bright ribbons clearly appeared underneath the erupting mini-filament as it quickly ascended, and subsequently, some dark materials blew out when the erupting mini-filament interacted with the outer ambient loops, thus forming a blowout jet characterized by a widening spire. At the same time, multiple small bright blobs of 1−2 Mm appeared at the interaction region and propagated along the post-eruption loops toward the footpoints of the erupting fluxes at a speed of ∼100 km s−1. They also caused a semi-circular brightening structure. Based on these features, we suggest that the mini-filament eruption first experiences internal and then external reconnection, the latter of which mainly transfers mass and magnetic flux of the erupting mini-filament to the ambient corona.

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First perihelion of EUI on the Solar Orbiter mission

Cited by 18 publications

References 64 publications

The source of unusual coronal upflows with photospheric abundance in a solar active region

The source of unusual coronal upflows with photospheric abundance in a solar active region

Future prospects for partially ionized solar plasmas: the prominence case

Evidence of external reconnection between an erupting mini-filament and ambient loops observed by Solar Orbiter/EUI

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