Context. A cataclysmic variable contains a white dwarf that accretes material from a secondary star via the Roche lobe mechanism. Systems with high line-of-sight inclination angles offer the possibility to pinpoint the location of the X-ray emitting region by characterizing the observed eclipse by the secondary star. Aims: We present an XMM-Newton observation of the dwarf nova Z Chamaleontis that we analyzed to determine the properties of the X-ray and optical light curves, as well as the high-energy spectrum. Methods: We performed a spectral analysis of the data taken by the EPIC camera, and a timing analysis of the observed X-ray and optical OM light curves. Results: We find that a multi-temperature plasma component absorbed by ionized material is required to describe the data. In particular, we estimate that the total absorbed flux in the 0.2-9.0 keV band is FAbs0.2-9.0 = (4.1±0.1) × 10-12 erg s-1 cm-2, which, when accounted for absorption and bolometric correction, corresponds to a bolometric luminosity of LBolX = (6.9±0.1) × 1030 erg s-1 at a distance of 97 pc. The mass accretion rate onto the white dwarf turns out to be about 1.1 × 10-11Msun yr-1. Our analysis of the optical and X-ray eclipse light curves and the mid-eclipse times of Z-Chamaleontis, in addition to the eclipse (during which the observed EPIC count rate is 0.033 ± 0.003 count s-1), implies that the X-ray light curve contains dips (at the orbital phases 0.30 ± 0.02 and 0.73 ± 0.02) that can be naturally explained as absorption effects by intervening stable gas clouds close to the accretor.
The XMM-Newton view of the eclipse and dips of the dwarf nova Z Chamaleontis.
NUCITA, Achille;MAIOLO, BERLINDA MARIA TERESA;DE PAOLIS, Francesco;INGROSSO, Gabriele;VETRUGNO, DANIELE
2011-01-01
Abstract
Context. A cataclysmic variable contains a white dwarf that accretes material from a secondary star via the Roche lobe mechanism. Systems with high line-of-sight inclination angles offer the possibility to pinpoint the location of the X-ray emitting region by characterizing the observed eclipse by the secondary star. Aims: We present an XMM-Newton observation of the dwarf nova Z Chamaleontis that we analyzed to determine the properties of the X-ray and optical light curves, as well as the high-energy spectrum. Methods: We performed a spectral analysis of the data taken by the EPIC camera, and a timing analysis of the observed X-ray and optical OM light curves. Results: We find that a multi-temperature plasma component absorbed by ionized material is required to describe the data. In particular, we estimate that the total absorbed flux in the 0.2-9.0 keV band is FAbs0.2-9.0 = (4.1±0.1) × 10-12 erg s-1 cm-2, which, when accounted for absorption and bolometric correction, corresponds to a bolometric luminosity of LBolX = (6.9±0.1) × 1030 erg s-1 at a distance of 97 pc. The mass accretion rate onto the white dwarf turns out to be about 1.1 × 10-11Msun yr-1. Our analysis of the optical and X-ray eclipse light curves and the mid-eclipse times of Z-Chamaleontis, in addition to the eclipse (during which the observed EPIC count rate is 0.033 ± 0.003 count s-1), implies that the X-ray light curve contains dips (at the orbital phases 0.30 ± 0.02 and 0.73 ± 0.02) that can be naturally explained as absorption effects by intervening stable gas clouds close to the accretor.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
