RX J1712.6-2414: a polarized intermediate polar from the ROSAT Galactic Plane Survey

Buckley, D.; Sekiguchi, K.; Motch, C.; O’Donoghue, D.; Chen, An-Le; Schwarzenberg-Czerny, A.; Pietsch, W.; Harrop-Allin, M. K.

doi:10.1093/mnras/275.4.1028

Cited by 58 publications

(66 citation statements)

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“…The balance of the two factors would determine whether the blobs accumulate sufficiently to form a disc, and it appears that V2400 Oph is close to this borderline, with sufficient orbiting blobs to carry much of the accretion flow (thus diluting the stream-fed pulsations), yet with the blobs not 'organised' enough to form a disc or to produce an X-ray spin pulse. V2400 Oph has a field strength (estimated as 9-27 MG; Buckley et al 1995;Väth 1997) that is as high or higher than in any other IP, and this may explain why the orbiting blobs cannot quite form a disc in this star, whereas they do in most IPs.…”

Section: Disc Formation: the Case Of V2400 Ophmentioning

confidence: 95%

Disc–magnetosphere interactions in cataclysmic variable stars

Hellier¹

2007

Proc. IAU

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Abstract. I review, from an observational perspective, the interactions of accretion discs with magnetic fields in cataclysmic variable stars. I start with systems where the accretion flows via a stream, and discuss the circumstances in which the stream forms into an accretion disc, pointing to stars which are close to this transition. I then turn to disc-fed systems and discuss what we know about how material threads on to field lines, as deduced from the pattern of accretion footprints on the white dwarf. I discuss whether distortions of the field lines are related to accretion torques and the changing spin periods of the white dwarfs. I also review the effect on the disc-magnetosphere interaction of disc-instability outbursts. Lastly, I discuss the temporary, dynamo-driven magnetospheres thought to occur in dwarf-nova outbursts, and whether slow-moving waves are excited at the inner edges of the disc.

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Section: Disc Formation: the Case Of V2400 Ophmentioning

confidence: 95%

Disc–magnetosphere interactions in cataclysmic variable stars

Hellier¹

2007

Proc. IAU

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“…The absence of an orbital variability typically expected in a disc-less configuration indicates that RX J1712 is a low inclination system. Indeed, a 10 o inclination is reported by Buckley et al (1995) and hence the secondary pole is never observed and the primary pole is mostly visible throughout the spin cycle. Our data do not support an additional emitting region in both soft and hard X-rays.…”

Section: Who Insteadmentioning

confidence: 98%

“…This system was discovered as a hard X-ray IP (Haberl & Motch 1995) pulsating at a period of 1003 s, but with a 927 s period in its optical polarised light (Buckley et al 1995(Buckley et al , 1997.…”

Section: The Beat Pulsation Of Rx J1712mentioning

confidence: 99%

BeppoSAX observations of soft X-ray intermediate polars

Martino

Matt

Belloni

et al. 2004

A&A

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Abstract. We present broad-band (0.1-90 keV) spectral and temporal properties of the three Intermediate Polars, RE 0751+144 (PQ Gem), RX J0558.0+5353 (V405 Aur) and RX J1712.6−2414 (V2400 Oph) based on simultaneous soft and hard X-ray observations with the BeppoSAX satellite. The analysis of their spectra over the wide energy range of BeppoSAX instruments allows us to identify the soft and hard X-ray components and to determine simultaneously their temperatures. The black-body temperatures of the irradiated poles of the white dwarf atmosphere are found to be 60-100 eV, much higher than those found in their synchronous analogues, the Polars. The temperature of the optically thin post-shock plasma is well constrained in RX J1712.6−2414 and in RE 0751+144 (13 and 17 keV) and less precisely determined in RX J0558.0+5353. In the first two systems evidence of subsolar abundances is found, similarly to that estimated in other magnetic Cataclysmic Variables. A Compton reflection component is present in RX J0558.0+5353 and in RE 0751+144 and it is favoured in RX J1712.6−2414. Its origin is likely at the irradiated white dwarf surface. Although these systems share common properties (a soft X-ray component and optical polarized radiation), their X-ray power spectra and light curves at different energies suggest accretion geometries that cannot be reconciled with a single and simple configuration.

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“…The first discless IP (Buckley et al 1995(Buckley et al , 1997, has a spin period of 927 s and an orbital period of 3.42 h, although no ephemeris has been published for V2400 Oph. It is believed to be at a low inclination of 10…”

Section: V2400 Ophmentioning

confidence: 99%

X-ray orbital modulations in intermediate polars

Parker

Norton

Mukai³

2005

A&A

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Abstract.We present an analysis of 30 archival ASCA and RXTE X-ray observations of 16 intermediate polars to investigate the nature of their orbital modulation. We show that X-ray orbital modulation is widespread amongst these systems, but not ubiquitous as indicated by previous studies that included fewer objects. Only seven of the sixteen systems show a clearly statistically significant modulation depth whose amplitude decreases with increasing X-ray energy. Interpreting this as due to photoelectric absorption in material at the edge of an accretion disc would imply that such modulations are visible for all system inclination angles in excess of 60 degrees. However, it is also apparent that the presence of an X-ray orbital modulation can appear and disappear on a timescale of ∼years or months in an individual system. This may be evidence for the presence of a precessing, tilted accretion disc, as inferred in some low mass X-ray binaries.

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RX J1712.6-2414: a polarized intermediate polar from the ROSAT Galactic Plane Survey

Cited by 58 publications

References 0 publications

Disc–magnetosphere interactions in cataclysmic variable stars

Disc–magnetosphere interactions in cataclysmic variable stars

BeppoSAX observations of soft X-ray intermediate polars

X-ray orbital modulations in intermediate polars

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