Ellerman bombs and UV bursts: reconnection at different atmospheric layers

• Published in: Astronomy and astrophysics (Berlin) 2020, Vol.633, p.A58
• Main Authors: Ortiz, Ada, Hansteen, Viggo H., Nóbrega-Siverio, Daniel, van der Voort, Luc Rouppe
• Format: Article
• Language: English
• Subjects: Bombs; Bursts; Chromosphere; Current sheets; Line spectra; Magnesium; Magnetic flux; Mathematical analysis; Photosphere; Silicon; Solar atmosphere
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361/201936574

The emergence of magnetic flux through the photosphere and into the outer solar atmosphere produces, amongst other dynamical phenomena, Ellerman bombs (EBs), which are observed in the wings of H α and are due to magnetic reconnection in the photosphere below the chromospheric canopy. Signs of magnetic reconnection are also observed in other spectral lines, typical of the chromosphere or the transition region. An example are the ultraviolet (UV) bursts observed in the transition region lines of Si  IV and the upper chromospheric lines of Mg  II . In this work we analyze high-cadence, high-resolution coordinated observations between the Swedish 1m Solar Telescope (SST) and the Interface Region Imaging Spectrograph (IRIS) spacecraft. H α images from the SST provide us with the positions, timings, and trajectories of EBs in an emerging flux region. Simultaneous, co-aligned IRIS slit-jaw images at 133 (C  II , transition region), 140 (Si  IV , transition region), and 279.6 (Mg  II k, core, upper chromosphere) nm as well as spectroscopy in the far- and near-ultraviolet from the fast spectrograph raster allow us to study the possible chromospheric and transition region counterparts of those EBs. Our main goal is to study the possible temporal and spatial relationship between several reconnection events at different layers in the atmosphere (namely EBs and UV bursts), the timing history between them, and the connection of these dynamical phenomena to the ejection of surges in the chromosphere. We also investigate the properties of an extended UV burst and their variations across the burst domain. Our results suggest a scenario where simultaneous and co-spatial EBs and UV bursts are part of the same reconnection system occurring sequentially along a vertical or nearly vertical current sheet. Heating and bidirectional jets trace the location where reconnection takes place. These results support and expand those obtained from recent numerical simulations of magnetic flux emergence.