| Author(s) * |
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A.K. Srivastava1, Yamini K. Rao1, P. Konkol2, K. Murawski2, P. Kayshap3, M. Mathioudakis4, E. Scullion5, S.K. Tiwari6, J.G. Doyle7, B.N. Dwivedi1 |
| Abstract * |
: |
1. Department of Physics, Indian Institute of Technology (BHU), Varanasi-211005, India.
2. Group of Astrophysics, Institute of Physics, University of M. Curie-Skłodowska, ul. Radziszewskiego 10, 20-031 Lublin, Poland.
3. Faculty of Science, University of South Bohemia, Ceské Budejovice, Czech Republic.
4. Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, BT7 1NN, UK
5. Department of Mathematics & Information Sciences, Northumbria University, Newcastle Upon Tyne, NE1 8ST, UK
6. Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover Street, Bldg. 252, Palo Alto, CA 94304, USA
7. Armagh Observatory and Planetarium, College Hill, Armagh, BT61 9DG, N. Ireland
ABSTRACT:
The fine-structured flowing cool loops are firstly observed using Slit-Jaw Imager of the Interface Region Imaging Spectrometer (IRIS). Huang et al. (2018) have observed unusually broadened Si IV 1403 A line profiles at the footpoints of such loops as a signature of the explosive events (EEs). We have chosen such uni and bi-directional flowing cool loop systems as observed by IRIS whose footpoints were associated with a largely broadened Si line profile indicating the occurrence of EEs and exhibiting an association of a considerable velocity perturbations of large amplitude. The model solar atmosphere was mimicking low lying bi-polar magnetic field system, which was perturbed in the chromosphere by the velocity pulses. The bi-directional as well as uni-directional plasma motions evolve in a similar manner as observed by IRIS in form of the flowing fine-structured plasma in the cool loop system. We compare the spatio-temporal evolution of the flowing cool loop system in our model with the observed such cases by IRIS, and conjecture that their formation is mostly associated with the transient energy release at their footpoints in the chromosphere/TR. We also compare our model results with other possibilities of the generation of localized plasma flows in the solar chromosphere. |
