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<ri:Resource created="2021-12-07T08:46:14Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>GRB spectral properties from Fermi and Swift</title><shortName>J/ApJ/898/14</shortName><identifier>ivo://CDS.VizieR/J/ApJ/898/14</identifier><altIdentifier>doi:10.26093/cds/vizier.18980014</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Mao J.</name></creator><creator><name>Li L.</name></creator><creator><name>Wang J.</name></creator><date role="Updated">2022-03-21T07:04:24Z</date><date role="Created">2021-12-07T08:46:14Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>gamma-ray-astronomy</subject><subject>gamma-ray-bursts</subject><description>We statistically examine the gamma-ray burst (GRB) photon indices obtained by the Fermi-GBM and Fermi-LAT observations and compare the LAT GRB photon indices to the GBM GRB photon indices. We apply the jitter radiation to explain the GRB spectral diversities in the high-energy bands. In our model, the jitter radiative spectral index is determined by the spectral index of the turbulence. We classify GRBs into three classes depending on the shape of the GRB high-energy spectrum when we compare the GBM and LAT detections: the GRB spectrum is concave (GRBs turn out to be softer and are labeled as S-GRBs), the GRB spectrum is convex (GRBs turn out to be harder and are labeled as H-GRBs), and the GRBs have no strong spectral changes (labeled as N-GRBs). A universal Kolmogorov index 7/3 in the turbulent cascade is consistent with the photon index of the N-GRBs. The S-GRB spectra can be explained by the turbulent cascade due to the kinetic magnetic reconnection with the spectral index range of the turbulence from 8/3 to 3.0. The H-GRB spectra originate from the inverse turbulent cascade with the spectral index range of the turbulence from 2.0 to 3.5 that occurred during the large lengthscale magnetic reconnection. Thus, the GRB radiative spectra are diversified because the turbulent cascade modifies the turbulent energy spectrum. More observational samples are expected in the future to further identify our suggestions.</description><source format="bibcode">2020ApJ...898...14M</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/898/14</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/B/swift">B/swift : Swift Master Catalog (HEASARC, 2004-)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/754/121">J/ApJ/754/121 : GRBs from Fermi/GBM and LAT (The Fermi Team, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/787/90">J/ApJ/787/90 : Gamma-ray bursts minimum timescales (Golkhou+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/781/37">J/ApJ/781/37 : Multi-band photometry of GRB 130427A (Perley+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/211/13">J/ApJS/211/13 : The second Fermi/GBM GRB catalog (4yr) (von Kienlin+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/811/93">J/ApJ/811/93 : Fermi/GBM GRB minimum timescales (Golkhou+, 2015)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/223/28">J/ApJS/223/28 : The third Fermi/GBM GRB catalog (6yr) (Bhat+, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/829/7">J/ApJ/829/7 : 3rd Swift/BAT GRB catalog (past ~11yrs) (BAT3) (Lien+, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/588/A135">J/A+A/588/A135 : Fermi/GBM GRB time-resolved spectral catalog (Yu+, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/893/46">J/ApJ/893/46 : 4rth 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