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  • 1. van der Voort, L. Rouppe
    et al.
    De Pontieu, B.
    Scharmer, Göran B.
    Stockholm University, Faculty of Science, Department of Astronomy. The Royal Swedish Academy of Sciences, Sweden.
    de la Cruz Rodríguez, Jaime
    Stockholm University, Faculty of Science, Department of Astronomy.
    Martínez-Sykora, J.
    Nóbrega-Siverio, D.
    Guo, L. J.
    Jafarzadeh, S.
    Pereira, T. M. D.
    Hansteen, V. H.
    Carlsson, M.
    Vissers, Gregal
    Stockholm University, Faculty of Science, Department of Astronomy.
    Intermittent Reconnection and Plasmoids in UV Bursts in the Low Solar Atmosphere2017In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 851, no 1, article id L6Article in journal (Refereed)
    Abstract [en]

    Magnetic reconnection is thought to drive a wide variety of dynamic phenomena in the solar atmosphere. Yet, the detailed physical mechanisms driving reconnection are difficult to discern in the remote sensing observations that are used to study the solar atmosphere. In this Letter, we exploit the high-resolution instruments Interface Region Imaging Spectrograph and the new CHROMIS Fabry Perot instrument at the Swedish 1-m Solar Telescope (SST) to identify the intermittency of magnetic reconnection and its association with the formation of plasmoids in socalled UV bursts in the low solar atmosphere. The Si IV 1403 angstrom UV burst spectra from the transition region show evidence of highly broadened line profiles with often non-Gaussian and triangular shapes, in addition to signatures of bidirectional flows. Such profiles had previously been linked, in idealized numerical simulations, to magnetic reconnection driven by the plasmoid instability. Simultaneous CHROMIS images in the chromospheric Ca 11 K 3934 angstrom line now provide compelling evidence for the presence of plasmoids by revealing highly dynamic and rapidly moving brightenings that are smaller than 0.12 and that evolve on timescales of the order of seconds. Our interpretation of the observations is supported by detailed comparisons with synthetic observables from advanced numerical simulations of magnetic reconnection and associated plasmoids in the chromosphere. Our results highlight how subarcsecond imaging spectroscopy sensitive to a wide range of temperatures combined with advanced numerical simulations that are realistic enough to compare with observations can directly reveal the small-scale physical processes that drive the wide range of phenomena in the solar atmosphere.

  • 2. Young, Peter R.
    et al.
    Tian, Hui
    Peter, Hardi
    Rutten, Robert J.
    Nelson, Chris J.
    Huang, Zhenghua
    Schmieder, Brigitte
    Vissers, Gregal J. M.
    Stockholm University, Faculty of Science, Department of Astronomy.
    Toriumi, Shin
    van der Voort, Luc H. M. Rouppe
    Madjarska, Maria S.
    Danilovic, Sanja
    Stockholm University, Faculty of Science, Department of Astronomy.
    Berlicki, Arkadiusz
    Chitta, L. P.
    Cheung, Mark C. M.
    Madsen, Chad
    Reardon, Kevin P.
    Katsukawa, Yukio
    Heinzel, Petr
    Solar Ultraviolet Bursts2018In: Space Science Reviews, ISSN 0038-6308, E-ISSN 1572-9672, Vol. 214, no 8, article id 120Article, review/survey (Refereed)
    Abstract [en]

    The term ultraviolet (UV) burst is introduced to describe small, intense, transient brightenings in ultraviolet images of solar active regions. We inventorize their properties and provide a definition based on image sequences in transition-region lines. Coronal signatures are rare, and most bursts are associated with small-scale, canceling opposite-polarity fields in the photosphere that occur in emerging flux regions, moving magnetic features in sunspot moats, and sunspot light bridges. We also compare UV bursts with similar transition-region phenomena found previously in solar ultraviolet spectrometry and with similar phenomena at optical wavelengths, in particular Ellerman bombs. Akin to the latter, UV bursts are probably small-scale magnetic reconnection events occurring in the low atmosphere, at photospheric and/or chromospheric heights. Their intense emission in lines with optically thin formation gives unique diagnostic opportunities for studying the physics of magnetic reconnection in the low solar atmosphere. This paper is a review report from an International Space Science Institute team that met in 2016-2017.

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