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Article: Chandra and Swift X-ray Observations of the X-ray Pulsar SMC X-2 During the Outburst of 2015

TitleChandra and Swift X-ray Observations of the X-ray Pulsar SMC X-2 During the Outburst of 2015
Authors
Issue Date2016
PublisherAmerican Astronomical Society, co-published with Institute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/
Citation
The Astrophysical Journal, 2016, v. 828 n. 2, p. 74:1-7 How to Cite?
AbstractWe report the Chandra/HRC-S and Swift/XRT observations for the 2015 outburst of the high-mass X-ray binary pulsar in the Small Magellanic Cloud, SMC X-2. While previous studies suggested that either an O star or a Be star in the field is the high-mass companion of SMC X-2, our Chandra/HRC-S image unambiguously confirms the O-type star as the true optical counterpart. Using the Swift/XRT observations, we extracted accurate orbital parameters of the pulsar binary through a time of arrivals analysis. In addition, there were two X-ray dips near the inferior conjunction, which are possibly caused by eclipses or an ionized high-density shadow wind near the companion’s surface. Finally, we propose that an outflow driven by the radiation pressure from day ∼10 played an important role in the X-ray/optical evolution of the outburst.
Persistent Identifierhttp://hdl.handle.net/10722/238706
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266

 

DC FieldValueLanguage
dc.contributor.authorLi, KL-
dc.contributor.authorHu, CP-
dc.contributor.authorLin, LCC-
dc.contributor.authorKong, AKH-
dc.date.accessioned2017-02-20T01:24:59Z-
dc.date.available2017-02-20T01:24:59Z-
dc.date.issued2016-
dc.identifier.citationThe Astrophysical Journal, 2016, v. 828 n. 2, p. 74:1-7-
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/10722/238706-
dc.description.abstractWe report the Chandra/HRC-S and Swift/XRT observations for the 2015 outburst of the high-mass X-ray binary pulsar in the Small Magellanic Cloud, SMC X-2. While previous studies suggested that either an O star or a Be star in the field is the high-mass companion of SMC X-2, our Chandra/HRC-S image unambiguously confirms the O-type star as the true optical counterpart. Using the Swift/XRT observations, we extracted accurate orbital parameters of the pulsar binary through a time of arrivals analysis. In addition, there were two X-ray dips near the inferior conjunction, which are possibly caused by eclipses or an ionized high-density shadow wind near the companion’s surface. Finally, we propose that an outflow driven by the radiation pressure from day ∼10 played an important role in the X-ray/optical evolution of the outburst.-
dc.languageeng-
dc.publisherAmerican Astronomical Society, co-published with Institute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/-
dc.relation.ispartofThe Astrophysical Journal-
dc.rightsThe Astrophysical Journal. Copyright © American Astronomical Society, co-published with Institute of Physics Publishing, Inc.-
dc.rightsThis work is licensed under a Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.-
dc.titleChandra and Swift X-ray Observations of the X-ray Pulsar SMC X-2 During the Outburst of 2015-
dc.typeArticle-
dc.identifier.emailHu, CP: cphu@hku.hk-
dc.description.naturepostprint-
dc.identifier.doi10.3847/0004-637X/828/2/74-
dc.identifier.hkuros271327-
dc.identifier.volume828-
dc.identifier.issue2-
dc.identifier.spage74:1-
dc.identifier.epage7-
dc.publisher.placeUnited States-

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