000315521 001__ 315521
000315521 005__ 20211110140137.0
000315521 020__ $$a978-3-935702-59-1
000315521 0247_ $$2datacite_doi$$a10.3204/DESY-PROC-2014-03/chowdhury_partha
000315521 0247_ $$2ISSN$$a1435-8077
000315521 037__ $$aPUBDB-2016-05928
000315521 1001_ $$0P:(DE-HGF)0$$aChowdhury, Partha $$b0$$eCorresponding author
000315521 1112_ $$0C14-06-29.1$$2inspire$$a10th Patras Workshop on Axions, WIMPs and WISPs$$cGeneva$$d2014-06-29 - 2014-07-04$$gAXION-WIMP 2014$$wSwitzerland
000315521 245__ $$aPeriodicities in the soft X-ray emission from the solar corona during descending phase of cycle 23
000315521 260__ $$aHamburg$$bVerlag Deutsches Elektronen-Synchrotron$$c2014
000315521 29510 $$aChowdhury, Partha "Periodicities in the soft X-ray emission from the solar corona during descending phase of cycle 23" in Proceedings, 10th Patras Workshop on Axions, WIMPs and WISPs (AXION-WIMP 2014)  / Tsesmelis, Emmanuel, Maroudas, Marios (eds.), Verlag Deutsches Elektronen-Synchrotron : 2014 ; AXION-WIMP 2014 : 10th Patras Workshop on Axions, WIMPs and WISPs, 2014-06-29 - 2014-07-04, Geneva
000315521 300__ $$a141-146
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000315521 4900_ $$0PERI:(DE-600)2450075-6$$aDESY-PROC
000315521 520__ $$aWe have studied the time series of full disk integrated soft X-ray emission from the solar corona during January 2004 to December 2008, covering the entire descending phase of solar cycle 23 from a global point of view. We employ the daily X-ray index (DXI) derived from 1s cadence X-ray observations from the Si detector of ``Solar X-ray Spectrometer (SOXS)'' mission in four different energy bands ranging between $6 - 25~KeV$. The daily time series is subjected to power spectrum analysis after appropriate correction for noise. Lomb-Scargle periodogram technique has shown prominent periods of $ \sim13.5$ days, $ \sim 27$ days, and near Rieger period of $ \sim 181$ days and $ \sim 1.24$ years in all energy bands. Further to this, other periods like $ \sim 31$, $\sim 48$, $\sim 57$, $\sim 76$, $\sim 96$, $\sim 130$, $\sim 227$ and $\sim 303$ days are also detected in different energy bands. We discuss our results in the light of previous observations and existing numerical models.
000315521 7870_ $$0PUBDB-2016-05897$$aTsesmelis, Emmanuel et. al.$$dVerlag Deutsches Elektronen-Synchrotron$$iisPartOf$$rDESY-PROC-2014-03$$tProceedings, 10th Patras Workshop on Axions, WIMPs and WISPs (AXION-WIMP 2014) : Geneva, Switzerland, June 29-July 4, 2014
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000315521 9101_ $$0I:(DE-HGF)0$$6P:(DE-HGF)0$$aUniversity College of Science \ and  Technology - Calcutta University - Kolkata 700009 - West Bengal - India $$b0
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