![]() 2012) and result in ubiquitous small-scale solar eruptions (i.e. Moreover, it has been suggested that swirling motions could also lead to mass flows (e.g. These waves may channel significant energy flux into the upper solar atmosphere. 2013 Shukla 2013 Mumford & Erdélyi 2015 Leonard et al. sausage and kink, and especially Alfvén waves) could be excited by photospheric swirls (e.g. Analytical analysis and numerical simulations have suggested that upwardly propagating magnetohydrodynamic (MHD) waves (including magneto-acoustic, e.g. Considering their ubiquity in the solar atmosphere, a number of attempts have been made to explore their potential as an energy supplier to the upper solar atmosphere. 2009 Wedemeyer-Böhm & Rouppe van der Voort 2009 Wedemeyer-Böhm et al. Swirling motions have been widely observed at different heights in the solar atmosphere, from the photosphere up to the corona (e.g. Key words: magnetohydrodynamics (MHD) / Sun: atmosphere / Sun: magnetic fields The co-temporal and co-spatial rotation in the photospheric velocity and magnetic fields provide evidence that the conjectured condition for the excitation of Alfvén pulses by photospheric swirls is fulfilled. On average, ∼71% of the detected velocity swirls have been found to co-exist with photospheric magnetic swirls with the same rotating direction.Ĭonclusions. More than 80% of the detected velocity swirls are found to be accompanied by local magnetic concentrations in intergranular lanes. On average, there are ∼63 short-lived photospheric velocity swirls (with lifetimes mostly less than 20 s, and average radius of ∼37 km and rotating speeds of ∼2.5 km s −1) detected in a field of view (FOV) of 6 × 6 Mm −2, implying a total population of velocity swirls of ∼1.06 × 10 7 in the solar photosphere. The spatial relationship between the detected velocity and magnetic swirls is further investigated via a well-defined correlation index (CI) study. The automated swirl detection algorithm (ASDA) is applied to the photospheric horizontal velocity and vertical magnetic fields obtained from a series of realistic numerical simulations using the radiative magnetohydrodynamics (RMHD) code Bifrost. We aim to understand whether photospheric velocity swirls exist co-spatially and co-temporally with photospheric magnetic swirls, in order to demonstrate the link between swirls and pulses. However, the conjectured necessary physical conditions for their excitation, that the magnetic field rotates co-spatially and co-temporally with the velocity field, has not been verified.Īims. It has been suggested that these events could contribute to the heating of the upper solar atmosphere, via exciting Alfvén pulses, which could carry significant amounts of energy. Velocity or intensity swirls have now been shown to be widely present throughout the photosphere and chromosphere. sétány 1/A, 1117 Budapest, HungaryĬAS Key Laboratory of Geospace Environment, Department of Geophysics and Planetary Sciences, University of Science and Technology of China, Hefei, Anhui 230026, PR ChinaĬontext. Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029, Blindern 0315, Oslo, NorwayĪstrophysics Research Centre (ARC), School of Mathematics and Physics, Queen’s University, Belfast BT7 1NN, UKĭepartment of Astronomy, Eötvös Loránd University, Pázmány P. Solar Physics and Space Plasma Research Centre (SP2RC), School of Mathematics and Statistics, The University of Sheffield, Sheffield S3 7RH, UKĮ-mail: Centre for Solar Physics, University of Oslo, PO Box 1029, Blindern 0315, Oslo, Norway Jiajia Liu (刘佳佳) 1, Mats Carlsson 2 ,3, Chris J. Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences ![]() Punctuation and style concerns regarding equations, figures, tables, and footnotes
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