6533b86ffe1ef96bd12cd4e5
RESEARCH PRODUCT
Chandra Observation of the Persistent Emission from the Dipping Source XB 1916-053
T. Di SalvoG. LavagettoN. R. RobbaR. IariaLuciano Burderisubject
Physicsline : formationAbsorption spectroscopySpectrometerAstrophysics::High Energy Astrophysical PhenomenaAstrophysics (astro-ph)FOS: Physical sciencesAstronomy and AstrophysicsAstrophysicsAstrophysicsOrbital periodstars : neutronSpectral linestars : individual (XB 1916-053)Neutron starline : identificationSpace and Planetary Scienceformation; line : identification; stars : individual (XB 1916-053); stars : neutron; X-rays : binaries; X-rays : general [line]Absorption (electromagnetic radiation)X-rays : binarieDiffraction gratingLine (formation)X-rays : generaldescription
We present the results of a 50 ks long Chandra observation of the dipping source XB 1916-053. During the observation two X-ray bursts occurred and the dips were not present at each orbital period. From the zero-order image we estimate the precise X-ray coordinates of the source with a 90% uncertainty of 0.6''. In this work we focus on the spectral study of discrete absorption features, during the persistent emission, using the High Energy Transmission Grating Spectrometer on board the Chandra satellite. We detect, for the first time in the 1st-order spectra of XB 1916-053, absorption lines associated to Ne X, Mg XII, Si XIV, and S XVI, and confirm the presence of the Fe XXV and Fe XXVI absorption lines with a larger accuracy with respect to the previous XMM EPIC pn observation. Assuming that the line widths are due to a bulk motion or a turbulence associated to the coronal activity, we estimate that the lines are produced in a photoionized absorber distant from the neutron star 4 x 10^{10} cm, near the disk edge.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2006-05-02 |