Title is correctly edited i.e. Suzaku observation of Be/X-ray binary pulsar EXO 2030+375
Postal Code - 380009
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INTRODUCTIONSection :
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Section 2 gives the details of the Suzakuobservation used in the present work, Section 3 presents the analysis and results obtained from the observation and Section 4 presents discussion and interpretation of the results obtained from our work.
OBSERVATIONSection :
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One-day averaged light curves of EXO 2030+375 in 15-50 keV energy range obtained from theSwift//BAT monitoring data from 2006November 21 to 2008 February 04 (top panel) and 2011 December05 to 2013 March 09 (bottom panel) covering both the Type I outbursts are shown in Figure 1.
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Combining XIS with HXD,Suzakucovers abroad energy band and can be used for the detailed study of X-ray sources. The publicly available archival data (version 2.7.16.33) ofthe 2012 May observation of EXO 2030+375 are used in the present work. As XIS-2 was nonoperationalduring above observation of the pulsar, data from the other three instruments that are part of XIS, as well as PIN and GSO, are used in our analysis.
ANALYSIS AND RESULTS Section :
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Timing Analysis (Subsection 3.1) :
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Spectral Analysis (Subsection 3.2) :
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Pulse-phase-resolved spectroscopy (Subsection 3.2.2) :
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Background spectra and response matrices used in the phase-averaged spectroscopy were also used in the phase-resolved spectral analysis.
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In case of both the models, the value of additional column density(NH2) was found to be high in 0.6-0.9 pulse phase range.
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DISCUSSION :
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The lower value of additional columndensity, absence of absorption dips in the pulse profile of the pulsar and about an order of magnitude lessluminous during 2012 MaySuzakuobservation confirm that mass accretion from the circumstellar disk ofthe Be star to the neutron star was significantly low comparedto that during 2007 May observation.
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Therefore, we suggest that the size of the circumstellar disk of the Be star in EXO 2030+375 binary system was relatively small during the 2012 May outburst compared to that during 2007 May observation.
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Therefore, the change in shape of the pulse profiles with luminosity in Be/X-ray binary pulsars agrees with the theoretical prediction by Romanova et al. (2008) though it was done for objects with a low magnetic field.
ACKNOWLEDGEMENT Section : The text is correctly edited.