The Intermediate Polars

Hellier, C.

doi:10.1007/978-94-009-0325-8_44

Cited by 33 publications

(15 citation statements)

References 51 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Unlike in other members of the AM Her class, in intermediate polars the rotation of the primary white dwarf is not synchronized with the orbital motion of the binary system. The spin periods found in intermediate polars are usually much shorter than their orbital periods ( Patterson 1994;Hellier 1996).…”

Section: An Intermediate Polar Modelmentioning

confidence: 95%

Nova V4743 Sagittarii 2002: An Intermediate Polar Candidate

Kang

Retter

Liu³

et al. 2006

View full text Add to dashboard Cite

We present the results of 11 nights of CCD unfiltered photometry of V4743 Sgr (Nova Sgr 2002 No. 3) from 2003 and 2005. We find two periods of 0.2799 days (%6.7 hr) and 0.01642 days (%24 minutes) in the 2005 data. The long period is also present in the 2003 data, but only weak evidence of the shorter period is found in this year. The 24 minute period is somewhat longer than the 22 minute period that was detected from X-ray observations. We suggest that the 6.7 hr periodicity represents the orbital period of the underlying binary system and that the 24 minute period is the beat periodicity between the orbital period and the X-ray period, which is presumably the spin period of the white dwarf. Thus, V4743 Sgr should be classified as an intermediate polar (DQ Her star). About 6 months after the nova outburst, the optical light curve of V4743 Sgr seemed to show quasi-periodic oscillations, which are typical of the transient phase in classical novae. Therefore, our results support the previous suggestion that the transition phase in novae may be related to intermediate polars.

show abstract

Section: An Intermediate Polar Modelmentioning

confidence: 95%

Nova V4743 Sagittarii 2002: An Intermediate Polar Candidate

Kang

Retter

Liu³

et al. 2006

View full text Add to dashboard Cite

show abstract

“…The five known asynchronous polars (APs) are V1432 Aql (RXJ 1940-10), BY Cam, V1500 Cyg, CD Ind (RXJ 2115-58), and Paloma (RX J0524+42) (Campbell & Schwope 1999;Schwarz et al 2004). EX Hya is an Intermediate Polar (IP), with a magnetic field of ∼1 MG and an accretion disc that has been observed to have dwarf nova outbursts, which also has a very high asynchronicity (Hellier 1996), and was included in this study as well.…”

Section: Introductionmentioning

confidence: 99%

Non-detection of nova shells around asynchronous polars

Pagnotta¹,

Zurek²

2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

Asynchronous polars (APs) are accreting white dwarfs (WDs) that have different WD and orbital angular velocities, unlike the rest of the known polars, which rotate synchronously (i.e., their WD and orbital angular velocities are the same). Past nova eruptions are the predicted cause of the asynchronicity, in part due to the fact that one of the APs, V1500 Cyg, was observed to undergo a nova eruption in 1975. We used the Southern African Large Telescope 10m class telescope and the MDM 2.4m Hiltner telescope to search for nova shells around three of the remaining four APs (V1432 Aql, BY Cam, and CD Ind) as well as one Intermediate Polar with a high asynchronicity (EX Hya). We found no evidence of nova shells in any of our images. We therefore cannot say that any of the systems besides V1500 Cyg had nova eruptions, but because not all post-nova systems have detectable shells, we also cannot exclude the possibility of a nova eruption occurring in any of these systems and knocking the rotation out of sync.

show abstract

“…The presence of unusual CVs with DN-like outbursts, which significantly deviate from the canonical picture of DNe, has recently been receiving special attention (Ishioka et al 2002;Szkody et al 2002). Some of these objects have been proven to intermediate polars (IPs) (for recent reviews of IPs, see Patterson 1994;Hellier 1996), which contain weakly magnetized white dwarfs. Theoretical attempts have been also made to explain these unusual outburst characters in the presence of a global magnetic field (e.g.…”

Section: Introductionmentioning

confidence: 99%

Two X-ray bright cataclysmic variables with unusual activities: GZ Cnc and NSV 10934

Katô

Dubovský²,

Stubbings³

et al. 2002

A&A

View full text Add to dashboard Cite

Abstract. We report on a discovery of unexpected activities in two X-ray bright dwarf novae. GZ Cnc showed an anomalous clustering of outbursts in 2002, in contrast to a low outburst frequency in the past record. The activity resembles an increased activity seen in some intermediate polars or candidates. We identified NSV 10934, X-ray selected high-amplitude variable star, as a dwarf nova with unusually rapid decline. The outburst characteristics make NSV 10934 a twin of recently discovered intermediate polar (HT Cam) with dwarf nova-type outbursts. We propose that these activities in X-ray strong dwarf novae may be a previously overlooked manifestation of outburst activities in magnetic cataclysmic variables.

show abstract

The Intermediate Polars

Cited by 33 publications

References 51 publications

Nova V4743 Sagittarii 2002: An Intermediate Polar Candidate

Nova V4743 Sagittarii 2002: An Intermediate Polar Candidate

Non-detection of nova shells around asynchronous polars

Two X-ray bright cataclysmic variables with unusual activities: GZ Cnc and NSV 10934

Contact Info

Product

Resources

About