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Zoekopdracht: journal id: "astrophysicalxjournal"

AuteursM.V. McSwain, D.R. Gies, W. Huang, P.J. Wiita, D.W. Wingert, L. Kaper
TitelThe N Enrichment and Supernova Ejection of the Runaway Microquasar LS 5039
TijdschriftAstrophysical Journal
Jaargang600
Jaar2004
Pagina's927-938
ISSN0004637X
FaculteitFaculteit der Natuurwetenschappen, Wiskunde en Informatica
Instituut/afd.FNWI: Astronomical Institute Anton Pannekoek (IAP)
Trefwoorden-
SamenvattingWe present an investigation of new optical and ultraviolet spectra of the mass donor star in the massive X-ray binary LS 5039. The optical band spectral line strengths indicate that the atmosphere is N-rich and C-poor, and we classify the stellar spectrum as type ON6.5 V((f)). The N-strong and C-weak pattern is also found in the stellar wind P Cygni lines of N V lambda1240 and C IV lambda1550 (narrow absorption components in the former indicate that the wind terminal velocity is V<SUB>∞</SUB>=2440+/-190 km s<SUP>-1</SUP>). We suggest that the N enrichment may result from internal mixing if the O star was born as a rapid rotator or the O star may have accreted N-rich gas prior to a common envelope interaction with the progenitor of the supernova. We reevaluated the orbital elements to find an orbital period of P=4.4267+/-0.0005 days. We compared the spectral line profiles with new non-LTE line-blanketed model spectra from Lanz and Hubeny, from which we derive an effective temperature T<SUB>eff</SUB>=37.5+/-1.7 kK, gravity logg=4.0+/-0.1, and projected rotational velocity Vsini=140+/-8 km s<SUP>-1</SUP>. We fitted the UV, optical, and IR flux distribution by using a model spectrum and extinction law with parameters E(B-V)=1.28+/-0.02 and R=3.18+/-0.07. We confirm the covariability of the observed X-ray flux and stellar wind mass-loss rate derived from the Halpha profile, which supports the wind accretion scenario for the X-ray production in LS 5039. Wind accretion models indicate that the compact companion has mass M<SUB>X</SUB>/M<SUB>solar</SUB>=1.4+/-0.4, consistent with its identification as a neutron star. We argue that the O star has mass in the range 20-35 M<SUB>solar</SUB> (based on a lower limit for the distance and the lack of eclipses). The observed eccentricity and runaway velocity of the binary can be reconciled only if the neutron star received a modest kick velocity due to a slight asymmetry in the supernova explosion (during which more than 5 M<SUB>solar</SUB> was ejected).
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