File Download
  Links for fulltext
     (May Require Subscription)
Supplementary

Article: Orbital and Spin Parameter Variations of Partial Eclipsing Low Mass X-ray Binary X 1822-371

TitleOrbital and Spin Parameter Variations of Partial Eclipsing Low Mass X-ray Binary X 1822-371
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. 831 n. 1, p. 29:1-10 How to Cite?
AbstractWe report our measurements for orbital and spin parameters of X 1822-371 using its X-ray partial eclipsing profile and pulsar timing from data collected by the Rossi X-ray Timing Explorer (RXTE). Four more X-ray eclipse times obtained by the RXTE 2011 observations were combined with historical records to trace evolution of orbital period. We found that a cubic ephemeris likely better describes evolution of the X-ray eclipse times during a time span of about 34 years with a marginal second order derivative of $ddot{P}_{orb}=(-1.05 pm 0.59) imes 10^{-19}$ s$^{-1}$. Using the pulse arrival time delay technique, the orbital and spin parameters were obtained from RXTE observations from 1998 to 2011. The detected pulse periods show that the neutron star in X 1822-371 is continuously spun-up with a rate of $dot{P}_{s}=(-2.6288 pm 0.0095) imes 10^{-12}$ s s$^{-1}$. Evolution of the epoch of the mean longitude $l=pi /2$ (i.e. $T_{pi / 2}$) gives an orbital period derivative value consistent with that obtained from the quadratic ephemeris evaluated by the X-ray eclipse but the detected $T_{pi / 2}$ values are significantly and systematically earlier than the corresponding expected X-ray eclipse times by $90 pm 11$ s. This deviation is probably caused by asymmetric X-ray emissions. We also attempted to constrain the mass and radius of the neutron star using the spin period change rate and concluded that the intrinsic luminosity of X 1822-371 is likely more than $10^{38}$ ergs s$^{-1}$.
Persistent Identifierhttp://hdl.handle.net/10722/238707
ISSN
2017 Impact Factor: 5.551
2015 SCImago Journal Rankings: 3.266
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorChou, Y-
dc.contributor.authorHsieh, HE-
dc.contributor.authorHu, CP-
dc.contributor.authorYang, TC-
dc.contributor.authorSu, YH-
dc.date.accessioned2017-02-20T01:25:00Z-
dc.date.available2017-02-20T01:25:00Z-
dc.date.issued2016-
dc.identifier.citationThe Astrophysical Journal, 2016, v. 831 n. 1, p. 29:1-10-
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/10722/238707-
dc.description.abstractWe report our measurements for orbital and spin parameters of X 1822-371 using its X-ray partial eclipsing profile and pulsar timing from data collected by the Rossi X-ray Timing Explorer (RXTE). Four more X-ray eclipse times obtained by the RXTE 2011 observations were combined with historical records to trace evolution of orbital period. We found that a cubic ephemeris likely better describes evolution of the X-ray eclipse times during a time span of about 34 years with a marginal second order derivative of $ddot{P}_{orb}=(-1.05 pm 0.59) imes 10^{-19}$ s$^{-1}$. Using the pulse arrival time delay technique, the orbital and spin parameters were obtained from RXTE observations from 1998 to 2011. The detected pulse periods show that the neutron star in X 1822-371 is continuously spun-up with a rate of $dot{P}_{s}=(-2.6288 pm 0.0095) imes 10^{-12}$ s s$^{-1}$. Evolution of the epoch of the mean longitude $l=pi /2$ (i.e. $T_{pi / 2}$) gives an orbital period derivative value consistent with that obtained from the quadratic ephemeris evaluated by the X-ray eclipse but the detected $T_{pi / 2}$ values are significantly and systematically earlier than the corresponding expected X-ray eclipse times by $90 pm 11$ s. This deviation is probably caused by asymmetric X-ray emissions. We also attempted to constrain the mass and radius of the neutron star using the spin period change rate and concluded that the intrinsic luminosity of X 1822-371 is likely more than $10^{38}$ ergs s$^{-1}$.-
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.titleOrbital and Spin Parameter Variations of Partial Eclipsing Low Mass X-ray Binary X 1822-371-
dc.typeArticle-
dc.identifier.emailHu, CP: cphu@hku.hk-
dc.description.naturepostprint-
dc.identifier.doi10.3847/0004-637X/831/1/29-
dc.identifier.hkuros271328-
dc.identifier.volume831-
dc.identifier.issue1-
dc.identifier.spage29:1-
dc.identifier.epage10-
dc.identifier.isiWOS:000387141200003-
dc.publisher.placeUnited States-

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats