File Download

There are no files associated with this item.

  Links for fulltext
     (May Require Subscription)
Supplementary

Article: Swift observations of the Be/X-ray transient system 1A 1118-615

TitleSwift observations of the Be/X-ray transient system 1A 1118-615
Authors
KeywordsAccretion, accretion discs
Binaries: general
Pulsars: individual: 1A 1118-615
Stars: emission-line, Be
Stars: neutron
X-rays: binaries
Issue Date2010
PublisherBlackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNR
Citation
Monthly Notices Of The Royal Astronomical Society, 2010, v. 409 n. 3, p. 1127-1135 How to Cite?
AbstractWe report results of Swift observations for the high-mass Be/X-ray binary system 1A 1118-615, during an outburst stage in 2009 January and at a flaring stage in 2009 March. Using the epoch-folding method, we successfully detected a pulsed period of 407.69(2) s in the outburst of January and of 407.26(1) s after the flare detection in March. We find that the spectral detection for the source during outburst can be described by a blackbody model with a high temperature () and a small radius ( km), indicating that the emission results from the polar cap of the neutron star. On the other hand, the spectra obtained after the outburst can further be described by adding an additional component with a lower temperature () and a larger emission radius ( km), which indicates the emission from around the inner region of an accretion disc. We find that the thermal emission from the hotspot of the accreting neutron star dominates the radiation in outburst; the existence of both this X-ray contribution and the additional soft component suggests that the polar cap and the accretion disc emission might co-exist after the outburst. Because the two-blackbody signature at the flaring stage is a unique feature of 1A 1118-615, our spectral results may provide a new insight to interpret the X-ray emission for the accreting neutron star. The time separation between the three main outbursts of this system is ~17 yr and it might be related to the orbital period. We derive and discuss the associated physical properties by assuming the elongated orbit for this specific Be/X-ray transient. © 2010 The Authors. Journal compilation © 2010 RAS.
Persistent Identifierhttp://hdl.handle.net/10722/135360
ISSN
2015 Impact Factor: 4.952
2015 SCImago Journal Rankings: 2.806
ISI Accession Number ID
Funding AgencyGrant Number
National Science CouncilNSC 98-2811-M-008-044
NSC 96-2112-M-008-017-MY3
NSC 95-2923-M-008-001-MY3
NSC 96-2112-M-007-037-MY3
Funding Information:

The authors appreciate an anonymous referee for his/her fruitful comments. We thank Prof. Kwong-Sang Cheng for the fruitful discussion to this manuscript. This research has made use of the data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center. This work also made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This work was partially supported by the National Science Council through grant NSC 98-2811-M-008-044. C-YH acknowledges support from the National Science Council through grants NSC 96-2112-M-008-017-MY3 and NSC 95-2923-M-008-001-MY3. AKHK acknowledges support from the National Science Council through grant NSC 96-2112-M-007-037-MY3.

References

 

DC FieldValueLanguage
dc.contributor.authorLin, LCCen_HK
dc.contributor.authorTakata, Jen_HK
dc.contributor.authorKong, AKHen_HK
dc.contributor.authorHwang, CYen_HK
dc.date.accessioned2011-07-27T01:34:10Z-
dc.date.available2011-07-27T01:34:10Z-
dc.date.issued2010en_HK
dc.identifier.citationMonthly Notices Of The Royal Astronomical Society, 2010, v. 409 n. 3, p. 1127-1135en_HK
dc.identifier.issn0035-8711en_HK
dc.identifier.urihttp://hdl.handle.net/10722/135360-
dc.description.abstractWe report results of Swift observations for the high-mass Be/X-ray binary system 1A 1118-615, during an outburst stage in 2009 January and at a flaring stage in 2009 March. Using the epoch-folding method, we successfully detected a pulsed period of 407.69(2) s in the outburst of January and of 407.26(1) s after the flare detection in March. We find that the spectral detection for the source during outburst can be described by a blackbody model with a high temperature () and a small radius ( km), indicating that the emission results from the polar cap of the neutron star. On the other hand, the spectra obtained after the outburst can further be described by adding an additional component with a lower temperature () and a larger emission radius ( km), which indicates the emission from around the inner region of an accretion disc. We find that the thermal emission from the hotspot of the accreting neutron star dominates the radiation in outburst; the existence of both this X-ray contribution and the additional soft component suggests that the polar cap and the accretion disc emission might co-exist after the outburst. Because the two-blackbody signature at the flaring stage is a unique feature of 1A 1118-615, our spectral results may provide a new insight to interpret the X-ray emission for the accreting neutron star. The time separation between the three main outbursts of this system is ~17 yr and it might be related to the orbital period. We derive and discuss the associated physical properties by assuming the elongated orbit for this specific Be/X-ray transient. © 2010 The Authors. Journal compilation © 2010 RAS.en_HK
dc.languageengen_US
dc.publisherBlackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNRen_HK
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_HK
dc.rightsThe definitive version is available at www.blackwell-synergy.com-
dc.subjectAccretion, accretion discsen_HK
dc.subjectBinaries: generalen_HK
dc.subjectPulsars: individual: 1A 1118-615en_HK
dc.subjectStars: emission-line, Been_HK
dc.subjectStars: neutronen_HK
dc.subjectX-rays: binariesen_HK
dc.titleSwift observations of the Be/X-ray transient system 1A 1118-615en_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0035-8711&volume=409&issue=3&spage=1127&epage=1135&date=2010&atitle=Swift+observations+of+the+Be/X-ray+transient+system+1A+1118‑615-
dc.identifier.emailTakata, J: takata@hku.hken_HK
dc.identifier.authorityTakata, J=rp00786en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1111/j.1365-2966.2010.17368.xen_HK
dc.identifier.scopuseid_2-s2.0-78649730416en_HK
dc.identifier.hkuros186455en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-78649730416&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume409en_HK
dc.identifier.issue3en_HK
dc.identifier.spage1127en_HK
dc.identifier.epage1135en_HK
dc.identifier.isiWOS:000284854300021-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridLin, LCC=24366370500en_HK
dc.identifier.scopusauthoridTakata, J=22735157300en_HK
dc.identifier.scopusauthoridKong, AKH=35185316600en_HK
dc.identifier.scopusauthoridHwang, CY=7403387605en_HK

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats