2010A&A...516A..76T


Query : 2010A&A...516A..76T

2010A&A...516A..76T - Astronomy and Astrophysics, volume 516, A76-76 (2010/6-2)

X-ray spectroscopy and photometry of the long-period polar AI Trianguli with XMM-Newton.

TRAULSEN I., REINSCH K., SCHWARZ R., DREIZLER S., BEUERMANN K., SCHWOPE A.D. and BURWITZ V.

Abstract (from CDS):

The energy balance of cataclysmic variables with strong magnetic fields is a central subject in understanding accretion processes on magnetic white dwarfs. With XMM-Newton, we perform a spectroscopic and photometric study of soft X-ray selected polars during their high states of accretion. On the basis of X-ray and optical observations of the magnetic cataclysmic variable AI Tri, we derive the properties of the spectral components, their flux contributions, and the physical structure of the accretion region in soft polars. We use multi-temperature approaches in our xspec modeling of the X-ray spectra to describe the physical conditions and the structures of the post-shock accretion flow and the accretion spot on the white-dwarf surface. In addition, we investigate the accretion geometry of the system by completing a timing analysis of the photometric data. Flaring soft X-ray emission from the heated surface of the white dwarf dominates the X-ray flux during roughly 70% of the binary cycle. This component deviates from a single black body and can be described by a superimposition of mildly absorbed black bodies with a Gaussian temperature distribution between kTbb,low:=2eV and kTbb,high=43.9+3.3–3.2eV, and NH,ISM=1.5+0.8–0.7x1020cm–2. In addition, weaker hard X-ray emission is visible nearly all the time. The spectrum from the cooling post-shock accretion flow is most closely fitted by a combination of thermal plasma mekal models with temperature profiles adapted from prior stationary two-fluid hydrodynamic calculations. The resulting plasma temperatures lie between kTMEKAL,low=0.8+0.4–0.2keV and kTMEKAL,high=20.0+9.9–6.1keV; additional intrinsic, partial-covering absorption is on the order of NH,int=3.3+2.5–1.2x1023cm–2. The soft X-ray light curves show a dip during the bright phase, which can be interpreted as self-absorption in the accretion stream. Phase-resolved spectral modeling supports the picture of one-pole accretion and self-eclipse. One of the optical light curves corresponds to an irregular mode of accretion. During a short XMM-Newton observation at the same epoch, the X-ray emission of the system is clearly dominated by the soft component.

Abstract Copyright:

Journal keyword(s): novae, cataclysmic variables - stars: individual: AI Tri - X-rays: binaries - accretion, accretion disks

Simbad objects: 18

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Number of rows : 18
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 V* AI Tri CV* 02 03 48.6151979976 +29 59 25.897508700           M2.5 39 1
2 USNO-B1.0 1199-00026672 * 02 03 54.4613846712 +29 57 55.046283948   14.8 14.62 13.5   ~ 1 0
3 USNO-B1.0 1199-00026710 * 02 03 59.0967520608 +29 58 28.979069016   13.8 13.29 12.9   ~ 1 0
4 V* EF Eri CV* 03 14 13.2526234800 -22 35 42.900077688   15.4 14.53 13.5   ~ 422 0
5 V* V1309 Ori CV* 05 15 41.4123253872 +01 04 40.481073984           M0.5 101 0
6 V* BY Cam CV* 05 42 48.8013535344 +60 51 31.376128608   16.60       ~ 243 0
7 V* VV Pup CV* 08 15 06.8009599464 -19 03 17.765706024     13.90     M7V 390 0
8 V* AR UMa CV* 11 15 44.5891034908 +42 58 22.431026739     16.4     D+M 134 0
9 V* EU UMa CV* 11 49 55.7017863576 +28 45 07.294697604           DB+K 69 0
10 V* EV UMa CV* 13 07 53.8579537224 +53 51 30.500194464           ~ 60 0
11 2XMM J131223.4+173659 CV* 13 12 23.4769193064 +17 36 59.185421388           ~ 10 0
12 V* V2301 Oph CV* 18 00 35.5317201576 +08 10 13.920836628           ~ 93 0
13 V* AM Her CV* 18 16 13.2546725112 +49 52 04.759613544   15.124 14.808 13.525   M4.5-5Ve 936 0
14 V* MT Dra CV* 18 46 58.7968849152 +55 38 28.771274508   20.4   19.4   ~ 19 0
15 RX J1856.6-3754 Psr 18 56 35.11 -37 54 30.5     25.7     ~ 413 0
16 V* V1432 Aql CV* 19 40 11.4199326288 -10 25 25.771706256     14.40 15.437   ~ 155 0
17 V* QQ Vul CV* 20 05 41.9090048400 +22 39 58.839854760   14.688 14.656 14.584   M2 193 0
18 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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2022.08.10-06:16:24

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