C.D.S. - SIMBAD4 rel 1.7 - 2020.08.04CEST22:33:01

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 - 2020
1 V* AI Tri AM* 02 03 48.6152251668 +29 59 25.898735063           M2.5 39 1
2 V* RS Cae AM* 04 53 25.46 -42 13 39.6           Am 36 0
3 V* BY Cam AM* 05 42 48.8013255299 +60 51 31.375887904   16.60       ~ 234 0
4 V* EK UMa AM* 10 51 35.1581989706 +54 04 36.103337325   18       CVam 77 0
5 V* AR UMa AM* 11 15 44.5894046553 +42 58 22.427873664     16.4     D+M 126 0
6 V* AM Her AM* 18 16 13.2546541781 +49 52 04.759861155     12.30     M4.5 911 0
7 V* QS Tel AM* 19 38 35.8145594082 -46 12 57.107614734           ~ 110 0
8 V* HU Aqr AM* 21 07 58.1945403160 -05 17 40.557984218   15.1   15.4   D+M4V 256 1

    Equat.    Gal    SGal    Ecl

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