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		<issn>0273-1177</issn>
		<label>9618</label>
		<citationkey>DAmicoHeRoPeGrPeTo:2001:DeHaXr</citationkey>
		<title>HEXTE studies of SCO X-1 spectra: detections of hard X-ray tails beyond 200 Kev</title>
		<year>2001</year>
		<secondarytype>PRE PI</secondarytype>
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		<author>D'Amico, Flávio,</author>
		<author>Heindl, W. A.,</author>
		<author>Rothschild, R. E.,</author>
		<author>Peterson, L. E.,</author>
		<author>Gruber, D. E.,</author>
		<author>Pelling, M.,</author>
		<author>Tomsick, J. A.,</author>
		<group>DAS-INPE-MCT-BR</group>
		<journal>Advances in Space Research</journal>
		<volume>28</volume>
		<number>2-3</number>
		<pages>389-394</pages>
		<transferableflag>1</transferableflag>
		<contenttype>External Contribution</contenttype>
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		<keywords>ASTROFÍSICA, espectro raio X, estrela de neutron, binarias raio X, buracos negros, X ray spectra, neutron stars, X ray binaries, black holes.</keywords>
		<abstract>Using the HEXTE experiment on-board the RXTE satellite, we performed a search for hard X-ray tails in Sco X-1 spectra. We found strong evidence for the presence of such a non-thermal component on several occasions. Using the PCAIRXTE we were able to track the position of the source along the Z diagram, and we observed that the presence of the hard X-ray tail is not confined to a particular region. However, we found a correlation between the power law index of the non-thermal component and the position of the source in the Z diagram, suggesting that the hard X-ray spectrum (i.e., E > 50 keV)becomes flatter as the mass accretion rate increases. We were also able to study the temporal variation of the appearance/absence of the hard X-ray component. With our derived luminosities, we were also able to test the idea that X-ray luminosities can be used to distinguish between X-ray binary systems containing neutron stars and black holes.</abstract>
		<area>CEA</area>
		<language>en</language>
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