Spectroscopic and imaging observations of transient hot and cool loops by IRIS and SDO

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dc.contributor.author Gupta, Girjesh R.
dc.contributor.author Nayak, Sushree S.
dc.date.accessioned 2012-09-20T03:32:51Z
dc.date.available 2012-09-20T03:32:51Z
dc.date.issued 2022-03
dc.identifier.citation Gupta, Girjesh R. and Nayak, Sushree S., "Spectroscopic and imaging observations of transient hot and cool loops by IRIS and SDO", arXiv, Cornell University Library, DOI: arXiv:2203.03529, Mar. 2022. en_US
dc.identifier.issn
dc.identifier.uri http://arxiv.org/abs/2203.03529
dc.identifier.uri https://repository.iitgn.ac.in/handle/123456789/7590
dc.description.abstract Coronal loops are basic building blocks of solar atmosphere and are observed on various length scales. However, their formation mechanism is still unclear. In this paper, we present the spectroscopic and imaging observations of small-scale transients and subsequent formation of transient loops. For the purpose, we have utilized the multi-wavelength observations recorded by AIA and IRIS-SJI, along with spectroscopic measurements provided by IRIS. For the photospheric magnetic field data, we obtained line-of-sight magnetogram data provided by HMI. Small-scale transients are simultaneously observed with several EUV and UV passbands of AIA and IRIS-SJI. HMI magnetogram provides evidence of negative flux cancellations beneath these transients. Differential Emission Measure (DEM) analysis shows that one of the transient attains temperature up to 8 MK whereas another one reaches only up to 0.4 MK. These transients further lead to the formation of small-scale loops with similar temperature distributions, and thus termed as hot and cool loops respectively. During the course of events, IRIS slit was rastering the region and thus provided spectroscopic measurements at both transients and associated loops. This enabled us to perform in-depth investigations of hot and cool loops. Using density sensitive O IV line pair, we obtained average electron densities along the hot and cool loop to be 1011.2 and 1010.8 cm-3 respectively. Energy estimates suggest that flux cancellation can easily power the hot transient whereas is insufficient for cool transient. Life time estimates and magnetic field extrapolation suggest presence of small-scale and fine structures within these loops. Results provide crucial ingredients on the physics of loop formation and involved thermodynamics.
dc.description.statementofresponsibility by Girjesh R. Gupta and Sushree S. Nayak
dc.language.iso en_US en_US
dc.publisher Cornell University Library en_US
dc.subject Coronal loops en_US
dc.subject Solar atmosphere en_US
dc.subject Spectroscopic en_US
dc.subject Differential Emission Measure en_US
dc.subject Photospheric magnetic field en_US
dc.subject IRIS slit en_US
dc.title Spectroscopic and imaging observations of transient hot and cool loops by IRIS and SDO en_US
dc.type Pre-Print en_US
dc.relation.journal arXiv


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