RX J1643.7+3402: A new bright cataclysmic variable

Mickaelian, A. M.; Balayan, S. K.; Ilovaisky, S.A.; Chevalier, C.; Véron-Cetty, M. P.; Véron, Philippe

doi:10.1051/0004-6361:20011244

Cited by 15 publications

(13 citation statements)

References 39 publications

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“… References . 1 Rodríguez‐Gil et al (2001); 2 Casares et al (1996); 3 Mickaelian et al (2002); 4 Hoard et al (2000); 5 Rodríguez‐Gil, Schmidtobreick & Gänsicke (2007); 6 Rodríguez‐Gil et al (2004); 7 Szkody et al (2003); 8 Thorstensen et al (1991b); 9 Wolfe et al (2003); 10 Beuermann et al (1992); 11 Moustakas & Schlegel (1999); 12 Schmidtobreick, Tappert & Saviane (2003); 13 Rodríguez‐Gil & Martínez‐Pais (2002); 14 Szkody et al (2001); 15 Thorstensen et al (1991a); 16 Hoard et al (1998); 17 Young, Schneider & Shectman (1981); 18 Garnavich et al (1990); 19 Taylor et al (1999); 20 Thoroughgood et al (2005); 21 Groot, Rutten & van Paradijs (2004); 22 Thoroughgood et al (2004); 23 Smith et al (1998) …”

Section: The Sw Sex Stars In the Context Of Cataclysmic Variable Evmentioning

confidence: 99%

SW Sextantis stars: the dominant population of cataclysmic variables with orbital periods between 3 and 4 h

Rodríguez‐Gil

Gänsicke

Hagen

et al. 2007

Monthly Notices of the Royal Astronomical Society

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We present time‐series optical photometry of five new cataclysmic variables (CVs) identified by the Hamburg Quasar Survey (HQS). The deep eclipses observed in HS 0129+2933 (= TT Tri), HS 0220+0603 and HS 0455+8315 provided very accurate orbital periods of 3.35129827(65), 3.58098501(34) and 3.56937674(26) h, respectively. HS 0805+3822 shows grazing eclipses and has a likely orbital period of 3.2169(2) h. Time‐resolved optical spectroscopy of the new CVs (with the exception of HS 0805+3822) is also presented. Radial velocity studies of the Balmer emission lines provided an orbital period of 3.55 h for HS 1813+6122, which allowed us to identify the observed photometric signal at 3.39 h as a negative superhump wave. The spectroscopic behaviour exhibited by all the systems clearly identifies them as new SW Sextantis (SW Sex) stars. HS 0220+0603 shows unusual N ii and Si ii emission lines suggesting that the donor star may have experienced nuclear evolution via the CNO cycle. These five new additions to the class increase the number of known SW Sex stars to 35. Almost 40 per cent of the total SW Sex population do not show eclipses, invalidating the requirement of eclipses as a defining characteristic of the class and the models based on a high orbital inclination geometry alone. On the other hand, as more SW Sex stars are identified, the predominance of orbital periods in the narrow 3–4.5 h range is becoming more pronounced. In fact, almost half the CVs which populate the 3–4.5 h period interval are definite members of the class. The dominance of SW Sex stars is even stronger in the 2–3 h period gap, where they make up 55 per cent of all known gap CVs. These statistics are confirmed by our results from the HQS CVs. Remarkably, 54 per cent of the Hamburg nova‐like variables have been identified as SW Sex stars with orbital periods in the 3–4.5 h range. The observation of this pile‐up of systems close to the upper boundary of the period gap is difficult to reconcile with the standard theory of CV evolution, as the SW Sex stars are believed to have the highest mass‐transfer rates among CVs. Finally, we review the full range of common properties that the SW Sex stars exhibit. Only a comprehensive study of this rich phenomenology will prompt to a full understanding of the phenomenon and its impact on the evolution of CVs and the accretion processes in compact binaries in general.

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Section: The Sw Sex Stars In the Context Of Cataclysmic Variable Evmentioning

confidence: 99%

SW Sextantis stars: the dominant population of cataclysmic variables with orbital periods between 3 and 4 h

Rodríguez‐Gil

Gänsicke

Hagen

et al. 2007

Monthly Notices of the Royal Astronomical Society

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“…The ROSAT X‐ray source RX J1643.7+3402 (AAVSO 1640+34) was identified as a cataclysmic variable (CV) by Mickaelian et al (2002). Based on spectroscopic and photometric data, they classified this object as a member of the SW Sex family.…”

Section: Introductionmentioning

confidence: 99%

The magnetic SW Sextantis star RX J1643.7+3402

Rodríguez‐Gil

Martínez‐País

Rodríguez

2009

Monthly Notices of the Royal Astronomical Society

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We present time‐resolved spectroscopy and circular spectropolarimetry of the SW Sex star RX J1643.7+3402. We find significant polarization levels exhibiting a variability at a period of 19.38 ± 0.39 min. In addition, emission‐line flaring is found predominantly at twice the polarimetric period. These two findings are strong evidences in favour of the presence of a magnetic white dwarf in the system. We interpret the measured periodicities in the context of our magnetic accretion model for SW Sex stars. In contrast with LS Pegasi – the first SW Sex star discovered to have modulated circular polarization – the polarization in RX J1643.7+3402 is suggested to vary at 2(ω−Ω), while the emission lines flare at (ω−Ω). However, a 2ω/ω interpretation cannot be ruled out. Together with LS Peg and V795 Her, RX J1643.7+3402 is the third SW Sex star known to exhibit modulated circular polarization.

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“…(Mickaelian et al , 2001(Mickaelian et al , 2002. Altogether, spectroscopic observations have been carried out for ∼400 FBS objects; however, only 100 have been published so far.…”

Section: The Fbs Blue Stellar Objectsmentioning

confidence: 99%

DSS1/DSS2 astrometry for 1101 First Byurakan Survey blue stellar objects: Accurate positions and other results

Mickaelian

2004

A&A

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Abstract. Accurate measurements of the positions of 1101 First Byurakan Survey (FBS) blue stellar objects (the Second part of the FBS) have been carried out on the DSS1 and DSS2 (red and blue images). To establish the accuracy of the DSS1 and DSS2, measurements have been made for 153 AGN for which absolute VLBI coordinates have been published. The rms errors are: 0.45 for DSS1, 0.33 for DSS2 red, and 0.59 for DSS2 blue in each coordinate, the corresponding total positional errors being 0.64 , 0.46 , and 0.83 , respectively. The highest accuracy (0.42 ) is obtained by weighted averaging of the DSS1 and DSS2 red positions. It is shown that by using all three DSS images accidental errors can be significantly reduced. The comparison of DSS2 and DSS1 images made it possible to reveal positional differences and proper motions for 78 objects (for 62 of these for the first time), including new high-probability candidate white dwarfs, and to find objects showing strong variability, i.e. high-probability candidate cataclysmic variables.

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RX J1643.7+3402: A new bright cataclysmic variable

Cited by 15 publications

References 39 publications

SW Sextantis stars: the dominant population of cataclysmic variables with orbital periods between 3 and 4 h

SW Sextantis stars: the dominant population of cataclysmic variables with orbital periods between 3 and 4 h

The magnetic SW Sextantis star RX J1643.7+3402

DSS1/DSS2 astrometry for 1101 First Byurakan Survey blue stellar objects: Accurate positions and other results

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