The UvA-LINKER will give you a range of other options to find the full text of a publication (including a direct link to the full-text if it is located on another database on the internet).
De UvA-LINKER biedt mogelijkheden om een publicatie elders te vinden (inclusief een directe link naar de publicatie online als deze beschikbaar is in een database op het internet).

Search results

Query: journal id: "astrophysicalxjournal"

AuthorsS.M. Caballero-Nieves, D.R. Gies, C.T. Bolton, P. Hadrava, A. Herrero, T.C. Hillwig, S.B. Howell, W. Huang, L. Kaper, P. Koubský, M.V. McSwain
TitleThe ultraviolet spectrum and physical properties of the mass donor star in HD 226868 = Cygnus X-1
JournalAstrophysical Journal
Volume701
Year2009
Issue2
Pages1895-1905
ISSN0004637X
FacultyFaculty of Science
Institute/dept.FNWI: Astronomical Institute Anton Pannekoek (IAP)
AbstractWe present an examination of high-resolution, ultraviolet (UV) spectroscopy from Hubble Space Telescope of the photospheric spectrum of the O-supergiant in the massive X-ray binary HD 226868 = Cyg X-1. We analyzed this and ground-based optical spectra to determine the effective temperature and gravity of the O9.7 Iab supergiant. Using non-LTE, line-blanketed, plane-parallel models from the TLUSTY grid, we obtain T-eff = 28.0 +/- 2.5 kK and log g greater than or similar to 3.00 +/- 0.25, both lower than in previous studies. The optical spectrum is best fit with models that have enriched He and N abundances. We fit the model spectral energy distribution for this temperature and gravity to the UV, optical, and infrared (IR) fluxes to determine the angular size and extinction toward the binary. The angular size then yields relations for the stellar radius and luminosity as a function of distance. By assuming that the supergiant rotates synchronously with the orbit, we can use the radius-distance relation to find mass estimates for both the supergiant and black hole (BH) as a function of the distance and the ratio of stellar to Roche radius. Fits of the orbital light curve yield an additional constraint that limits the solutions in the mass plane. Our results indicate masses of 23(-6)(+ 8) M-circle dot for the supergiant and 11(-3)(+5) M-circle dot for the BH.
Document typeArticle
Document finderUvA-Linker