1998A&A...338..465S


Query : 1998A&A...338..465S

1998A&A...338..465S - Astronomy and Astrophysics, volume 338, 465-478 (1998/10-2)

The new long-period AM Herculis system RX J0203.8+2959.

SCHWARZ R., SCHWOPE A.D., BEUERMANN K., BURWITZ V., FISCHER J.-U., FRIED R., LEHMANN I., MANTEL K.-H., MENGEL S., METZNER A., MISSELT K., NOTNI P., REINSCH K., SHAFTER A. and THOMAS H.-C.

Abstract (from CDS):

We present the first detailed multi-wavelength study of the ROSAT-discovered AM Herculis binary RX J0203.8+2959 comprising extended CCD and photoelectric photometry, phase-resolved spectroscopy with high and low spectral resolution and pointed ROSAT observations with the PSPC and the HRI. Between 1992 and 1997 the system displayed states of high and low accretion with mean brightness levels of V=15.5m and 18m, respectively. A timing analysis revealed that the binary is rotating synchronously with a period of 4.6hr and is thus one of the longest-period polars known. The emission lines are structured showing narrow and broad components. We could distinguish between line emission arising from the heated side of the secondary star and the accretion stream. Velocity information derived for a narrow emission line with suspected origin on the heated side of the companion star allowed us to constrain its orbital velocity and to phase its inferior conjunction. In addition the photospheric spectrum of the secondary star could be detected in the near-infrared. The strength of the TiO-bands was used to determine its spectral type as dM 2.5, which is consistent with a Roche lobe filling main sequence star, and to estimate the distance of the system to be ∼600pc. Definite confirmation of its magnetic nature is given by the detection of cyclotron harmonics implying a field strength of B=38±2MG. The accretion geometry could not be fixed unequivocally. The morphology of the optical light curves is suggestive of one active accretion region which undergoes no selfeclipse. A corresponding simple light curve pattern is not seen at X-ray wavelengths, it's time signature is dominated by instationary accretion of discrete blobs. We report on the occasional occurence of phase- and colour-dependent quasi-periodic oscillations at periods of ∼7 and ∼14min.

Abstract Copyright:

Journal keyword(s): accretion, accretion disks - binaries: close - stars: individual: RX J0203.8+2959 - stars: magnetic fields - novae, cataclysmic variables

Simbad objects: 13

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Number of rows : 13
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 V* EF Eri CV* 03 14 13.2526234800 -22 35 42.900077688   15.4 14.53 13.5   ~ 419 0
3 V* V1309 Ori CV* 05 15 41.4123253872 +01 04 40.481073984           M0.5 101 0
4 V* Z Cha CV* 08 07 27.7517751528 -76 32 00.665029356           M5.5 599 1
5 V* VV Pup CV* 08 15 06.8009599464 -19 03 17.765706024     13.90     M7V 388 0
6 BD+01 2447 PM* 10 28 55.5512830314 +00 50 27.598904576 12.389 11.151 9.650 8.617 7.389 dM2 281 0
7 V* V834 Cen CV* 14 09 07.2863511816 -45 17 16.023776676   16.0   15.301   M6.5 305 0
8 V* V895 Cen CV* 14 29 27.1971552960 -38 04 09.579261720           ~ 37 0
9 PG 1550+191 CV* 15 52 47.1968971224 +18 56 28.844471472   16.4 15.46 17.0   M6.5Ve 180 0
10 V* AM Her CV* 18 16 13.2546725112 +49 52 04.759613544   15.124 14.808 13.525   M4.5 931 0
11 V* V393 Pav CV* 19 57 11.5514523936 -57 38 22.427884104           ~ 26 0
12 V* QQ Vul CV* 20 05 41.9090048400 +22 39 58.839854760   14.688 14.656 14.584   M2 192 0
13 V* HU Aqr CV* 21 07 58.1944529400 -05 17 40.557671916   16.198 15.814 14.891   D+M4V 261 1

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2022.05.21-02:55:20

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