Query : 2014A&A...562A..42T

2014A&A...562A..42T - Astronomy and Astrophysics, volume 562A, 42-42 (2014/2-1)

Phase-resolved X-ray spectroscopy and spectral energy distribution of the X-ray soft polar RS Caeli.


Abstract (from CDS):

RS Cae is the third target in our series of XMM-Newton observations of soft X-ray-dominated polars. Our observational campaign aims to better understand and describe the multiwavelength data, the physical properties of the system components, and the short- and long-term behavior of the component fluxes in RS Cae. We employ stellar atmosphere, stratified accretion-column, and widely used X-ray spectral models. We fit the XMM-Newton spectra, model the multiband light curves, and opt for a mostly consistent description of the spectral energy distribution. Our XMM-Newton data of RS Cae are clearly dominated by soft X-ray emission. The X-ray light curves are shaped by emission from the main accretion region, which is visible over the whole orbital cycle, interrupted only by a stream eclipse. The optical light curves are formed by cyclotron and stream emission. The XMM-Newton X-ray spectra comprise a black-body-like and a plasma component at mean temperatures of 36eV and 7keV. The spectral fits give evidence of a partially absorbing and a reflection component. Multitemperature models, covering a broader temperature range in the X-ray emitting accretion regions, reproduce the spectra appropriately well. Including archival data, we describe the spectral energy distribution with a combination of models based on a consistent set of parameters and derive a lower limit estimate of the distance d>750pc. The high bolometric soft-to-hard flux ratios and short-term variability of the (X-ray) light curves are characteristic of inhomogeneous accretion. RS Cae clearly belongs in the group of polars that show a very strong soft X-ray flux compared to their hard X-ray flux. The different black-body fluxes and similar hard X-ray and optical fluxes during the XMM-Newton and ROSAT observations show that soft and hard X-ray emission are not directly correlated.

Abstract Copyright:

Journal keyword(s): novae, cataclysmic variables - stars: fundamental parameters - stars: individual: RS Caeli - X-rays: binaries - accretion, disks accretion

Simbad objects: 8

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Number of rows : 8
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
1 V* AI Tri CV* 02 03 48.6151979976 +29 59 25.897508700           M2.5 39 1
2 V* RS Cae CV* 04 53 25.46 -42 13 39.6           Am 36 0
3 V* BY Cam CV* 05 42 48.8013535344 +60 51 31.376128608   16.60       ~ 243 0
4 V* EK UMa CV* 10 51 35.1578195280 +54 04 36.112715220   18       ~ 79 0
5 V* AR UMa CV* 11 15 44.5891034908 +42 58 22.431026739     16.4     D+M 134 0
6 V* AM Her CV* 18 16 13.2546725112 +49 52 04.759613544   15.124 14.808 13.525   M4.5-5Ve 936 0
7 V* QS Tel CV* 19 38 35.8144163880 -46 12 57.106344420           ~ 111 0
8 V* HU Aqr CV* 21 07 58.1944529400 -05 17 40.557671916   16.198 15.814 14.891   D+M4V 264 1

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