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Forward modeling of standing slow modes in flaring coronal loops

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dc.contributor.author Yuan, D
dc.contributor.author Van Doorsselaere, T
dc.contributor.author Banerjee, D
dc.contributor.author Antolin, P
dc.date.accessioned 2020-11-14T07:07:08Z
dc.date.available 2020-11-14T07:07:08Z
dc.date.issued 2015-07-01
dc.identifier.citation The Astrophysical Journal, Vol. 807, No. 1, 98 en_US
dc.identifier.issn 0004-637X
dc.identifier.uri http://prints.iiap.res.in/handle/2248/7000
dc.description Restricted Access © IOP Publishing http://dx.doi.org/10.1088/0004-637X/807/1/98 en_US
dc.description.abstract Standing slow-mode waves in hot flaring loops are exclusively observed in spectrometers and are used to diagnose the magnetic field strength and temperature of the loop structure. Owing to the lack of spatial information, the longitudinal mode cannot be effectively identified. In this study, we simulate standing slow-mode waves in flaring loops and compare the synthesized line emission properties with Solar Ultraviolet Measurements of Emitted Radiation spectrographic and Solar Dynamics Observatory/Atmospheric Imaging Assembly imaging observations. We find that the emission intensity and line width oscillations are a quarter period out of phase with Doppler shift velocity in both time and spatial domain, which can be used to identify a standing slow-mode wave from spectroscopic observations. However, the longitudinal overtones could only be measured with the assistance of imagers. We find emission intensity asymmetry in the positive and negative modulations; this is because the contribution function pertaining to the atomic emission process responds differently to positive and negative temperature variations. One may detect half periodicity close to the loop apex, where emission intensity modulation is relatively small. The line-of-sight projection affects the observation of Doppler shift significantly. A more accurate estimate of the amplitude of velocity perturbation is obtained by de-projecting the Doppler shift by a factor of 1–2θ/π rather than the traditionally used cos q. If a loop is heated to the hotter wing, the intensity modulation could be overwhelmed by background emission, while the Doppler shift velocity could still be detected to a certain extent. en_US
dc.language.iso en en_US
dc.publisher IOP Publishing en_US
dc.subject Magnetohydrodynamics (MHD) en_US
dc.subject Sun: atmosphere en_US
dc.subject Sun: corona en_US
dc.subject Sun: oscillations en_US
dc.subject Waves en_US
dc.title Forward modeling of standing slow modes in flaring coronal loops en_US
dc.type Article en_US

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