DW Cancri: a magnetic VY Scl star with an orbital period of 86 min

Rodríguez‐Gil, P.; Gänsicke, B. T.; Araujo-Betancor, S.; Casares, J.

doi:10.1111/j.1365-2966.2004.07512.x

Cited by 31 publications

(41 citation statements)

References 19 publications

(20 reference statements)

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“…The continuum is flatter and about 3 times less intense in the blue than the spectrum from Augusteijn et al (2010). The spectrum is quite similar to that of short-period IPs like SDSS J2333 (Southworth et al 2007;Szkody et al 2005), HT Cam (Kemp et al 2002) and DW Cnc (Patterson et al 2004;Rodríguez-Gil et al 2004), among others. These objects present spectra that are indistinguishable from quiescent dwarf novae spectra and, therefore, show that a single optical spectrum is not enough to confirm the IP nature of a source.…”

Section: Ctcv2056-30 (Ctcv J2056-3014 = 1rxs J2056521-301433)mentioning

confidence: 63%

Exploratory Spectroscopy of Magnetic Cataclysmic Variables Candidates and Other Variable Objects

Oliveira¹,

Rodrigues²,

Cieslinski³

et al. 2017

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The increasing number of synoptic surveys made by small robotic telescopes, such as the photometric Catalina Real-Time Transient Survey (CRTS), represents a unique opportunity for the discovery of variable sources and improves the statistical samples of such classes of objects. Our goal is the discovery of magnetic Cataclysmic Variables (mCVs). These are rare objects, which probe interesting accretion scenarios controlled by the white dwarf magnetic field. In particular, improved statistics of mCVs would help to address open questions on their formation and evolution. We performed an optical spectroscopy survey to search for signatures of magnetic accretion in 45 variable objects selected mostly from the CRTS. In this sample we found 32 CVs, 22 being mCV candidates from which 13 are previously unreported as such. If the proposed classifications are confirmed, it would represent an increase of 4% in the number of known polars and 12% in the number of known IPs. A fraction of our initial sample was classified as extragalactic sources or other types of variable stars by the inspection of the identification spectra. Despite the inherent complexity in identifying a source as a mCV, variability-based selection followed by spectroscopic snapshot observations has proved to be an efficient strategy for their discoveries, being a relatively inexpensive approach in terms of telescope time.

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Section: Ctcv2056-30 (Ctcv J2056-3014 = 1rxs J2056521-301433)mentioning

confidence: 63%

Exploratory Spectroscopy of Magnetic Cataclysmic Variables Candidates and Other Variable Objects

Oliveira¹,

Rodrigues²,

Cieslinski³

et al. 2017

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“…Therefore, a much longer spectroscopic coverage is needed in order to confirm whether this radial velocity variation is produced by a stable clock in the system. In such a case, the 19.9‐min period should be related to the spin period of a magnetic white dwarf as it happens in intermediate polars like V1025 Cen (Buckley et al 1998), DW Cnc (Rodríguez‐Gil et al 2004a) and HS 0943+1404 (Rodríguez‐Gil et al 2005).…”

Section: Results On the Individual Objectsmentioning

confidence: 99%

Spectroscopic search for new SW Sextantis stars in the 3-4 h orbital period range - I

Rodríguez‐Gil

Schmidtobreick

Gänsicke

2007

Monthly Notices of the Royal Astronomical Society

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We report on time‐resolved optical spectroscopy of 10 non‐eclipsing nova‐like cataclysmic variables in the orbital period range between 3 and 4 h. The main objective of this long‐term programme is to search for the characteristic SW Sextantis behaviour and to eventually quantify the impact of the SW Sex phenomenon on nova‐likes at the upper boundary of the orbital period gap. Of the 10 systems observed so far, HL Aqr, BO Cet, AH Men, V380 Oph, AH Pic and LN UMa are identified as new members of the SW Sex class. We present improved orbital period measurements for HL Aqr (Porb= 3.254 ± 0.001 h) and V380 Oph (Porb= 3.69857 ± 0.00002 h). BO Cet and V380 Oph exhibit emission‐line flaring with periodicities of 20 and 47 min, respectively. The Hα line of HL Aqr shows significant blueshifted absorption modulated at the orbital period. Similarly to the emission S‐wave of the high‐inclination SW Sex stars, this absorptionS‐wave has its maximum blue velocity at orbital phase ∼0.5. We estimate an orbital inclination for HL Aqr in the range 19° < i < 27°, which is much lower than that of the emission‐dominated, non‐eclipsing SW Sex stars (i∼ 60°–70°). This gives rise to the interesting possibility of many low‐inclination nova‐likes actually being SW Sex stars, but with a very different spectroscopic appearance as they show significant absorption. The increasing blueshifted absorption with decreasing inclination points to the existence of a mass outflow with significant vertical motion. These six new additions to the SW Sex class increase the presence of non‐eclipsing systems to about one‐third of the whole SW Sex population, which therefore makes the requirement of eclipses as a defining criterion for SW Sex membership no longer valid. The statistics of the cataclysmic variable population in the vicinity of the upper period gap are also discussed.

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“…Examples of systems discovered or independently identified in our program include the deeply Based in part on observations obtained at the German-Spanish Astronomical Center, Calar Alto, operated by the Max-PlanckInstitut für Astronomie, Heidelberg, jointly with the Spanish National Commission for Astronomy; on observations made with the IAC80 and OGS telescopes, operated on the island of Tenerife by the Instituto de Astrofísica de Canarias (IAC) and the European Space Agency (ESA), respectively, in the Spanish Observatorio del Teide of the IAC; on observations made at the 1.2 m telescope, located at Kryoneri Korinthias, and owned by the National Observatory of Athens, Greece; and on observations made with the William Herschel Telescope, which is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the IAC. eclipsing, long-period dwarf nova GY Cnc (=HS 0907+1902, Gänsicke et al 2000), the rarely outbursting SU UMatype dwarf nova KV Dra (=HS 1449+6415, Nogami et al 2000), the two intemediate polars 1RXS J062518.2+733433 (=HS 0618+7336, Araujo-Betancor et al 2003) and DW Cnc (=HS 0756+1624, Rodríguez-Gil et al 2004a), the SW Sex stars KUV 03580+0614 (=HS 0357+0614, Szkody et al 2001) and HS 0728+6738 (Rodríguez-Gil et al 2004b), and the old pre-CV HS 2237+8154 . Whereas all these systems belong to species that are currently rare in the overall population of known CVs, their intrinsic number may be comparable to, if not larger than, that of the "classic" CVs, which are either frequently in outburst, or X-ray bright, or display obvious photometric variability.…”

Section: Introductionmentioning

confidence: 99%

Detection of the white dwarf and the secondary star in the new SU UMa dwarf nova HS 2219+1824

Rodríguez‐Gil¹,

Gänsicke²,

Hagen

et al. 2005

A&A

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Abstract.We report the discovery of a new, non-eclipsing SU UMa-type dwarf nova, HS 2219+1824. Photometry obtained in quiescence (V ≈ 17.5) reveals a double-humped light curve from which we derive an orbital period of 86.2 min. Additional photometry obtained during a superoutburst reaching V 12.0 clearly shows superhumps with a period of 89.05 min. The optical spectrum contains double-peaked Balmer and He I emission lines from the accretion disc as well as broad absorption troughs of Hβ, Hγ, and Hδ from the white dwarf primary star. Modelling of the optical spectrum implies a white dwarf temperature of 13 000 K < ∼ T eff < ∼ 17 000 K, a distance of 180 pc < ∼ d < ∼ 230 pc, and suggests that the spectral type of the donor star is later than M 5. Phase-resolved spectroscopy obtained during quiescence reveals a narrow Hα emission line component which has a radial velocity amplitude and phase consistent with an origin on the secondary star, possibly on the irradiated hemisphere facing the white dwarf. This constitutes the first detection of line emission from the secondary star in a quiescent SU UMa star.

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DW Cancri: a magnetic VY Scl star with an orbital period of 86 min

Cited by 31 publications

References 19 publications

Exploratory Spectroscopy of Magnetic Cataclysmic Variables Candidates and Other Variable Objects

Exploratory Spectroscopy of Magnetic Cataclysmic Variables Candidates and Other Variable Objects

Spectroscopic search for new SW Sextantis stars in the 3-4 h orbital period range - I

Detection of the white dwarf and the secondary star in the new SU UMa dwarf nova HS 2219+1824

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