The Spin Periods of Magnetic Cataclysmic Variables

Norton, A. J.; Somerscales, R. V.; Wynn, G. A.

doi:10.1017/s0252921100002128

Cited by 9 publications

(11 citation statements)

References 42 publications

(41 reference statements)

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“…The asynchronocity (1 − Pω/PΩ) of Paloma was found to be ∼ 16.6 % from the X-ray and optical data, which is slightly away from the line of synchronization. Furthermore, the values of P (ω , ω ′ ) /PΩ (∼ 0.8) obtained from X-ray and optical analyses of Paloma satisfy the synchronization condition derived by Norton et al (2004) i.e., Pω/PΩ > 0.6. The observed asynchronocity in Paloma suggests that it might be representative of a transition object currently in the process of attaining synchronism and evolving into polars.…”

Section: Discussionsupporting

confidence: 62%

“…MCVs occupy a wide range of parameter space in the Pω − PΩ plane in which the evolution of these systems can be drawn from the degree of synchronization with the orbital period. Paloma is one of the few MCVs with an orbital period lying in the period gap (∼ 2 − 3 hr) and discovered as one of the nearly synchronous IPs (see Norton et al 2004). The asynchronocity (1 − Pω/PΩ) of Paloma was found to be ∼ 16.6 % from the X-ray and optical data, which is slightly away from the line of synchronization.…”

Section: Discussionmentioning

confidence: 99%

“…The orbital period distribution of MCVs shows that the P Ω of polars are in the range of 1.0 − 10.0 hr, while a majority of the IPs have orbital periods longer than the period gap of 2 − 3 hrs (Scaringi et al 2010). The period gap is no longer seen to exist for polars (Norton et al 2004;Scaringi et al 2010).…”

Section: Introductionmentioning

confidence: 97%

“…However, there are some MCVs (e.g., V1432 Aql, BY Cam, CD Ind, and V1500 Cyg) for which the spin period (P ω ) and the orbital period (P Ω ) differ by about 2 % or less. These systems are thought to be polars and asynchronism is thought to arise due to a recent nova explosion (Norton et al 2004). The IPs possess a magnetic field of less than 10 MG and the WD rotation is not synchronized with the orbital motion (see Hellier 2002).…”

Section: Introductionmentioning

confidence: 99%

“…There are two other systems namely RX J0524+42 (Paloma) and V697 Sco, which are described as nearly synchronous IPs, with P ω = (0.7 − 0.9) P Ω . Paloma also lies in the period gap and is thought to be currently in the process of attaining synchronism and evolving into a polar (Norton et al 2004;Schwarz et al 2007). The orbital period distribution of MCVs shows that the P Ω of polars are in the range of 1.0 − 10.0 hr, while a majority of the IPs have orbital periods longer than the period gap of 2 − 3 hrs (Scaringi et al 2010).…”

Section: Introductionmentioning

confidence: 99%

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Paloma: A Magnetic Cv Between Polars and Intermediate Polars

Joshi

Pandey

Singh

et al. 2016

ApJ

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We present analyses of archival X-ray data obtained from the XMM-Newton satellite and optical photometric data obtained from 1 m class telescopes of ARIES, Nainital of a magnetic cataclysmic variable (MCV) Paloma. Two persistent periods at 156 ± 1 minutes and 130 ± 1 minutes are present in the X-ray data, which we interpret as the orbital and spin periods, respectively. These periods are similar to those obtained from the previous as well as new optical photometric observations. The soft-X-ray excess seen in the X-ray spectrum of Paloma and the averaged X-ray spectra are well fitted by two-temperature plasma models with temperatures of 0.10 +0.02 −0.01 and 13.0 +0.5 −0.5 keV with an Fe Kα line and an absorbing column density of 4.6 × 10 22 cm -2 . This material partially covers 60 ± 2 % of the X-ray source. We also present the orbital and spin-phase-resolved spectroscopy of Paloma in the 0.3 − 10.0 keV energy band and find that the X-ray spectral parameters show orbital and spin-phase dependencies. New results obtained from optical and X-ray studies of Paloma indicate that it belongs to a class of a few magnetic CVs that seem to have the characteristics of both the polars and the intermediate polars.

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Section: Discussionsupporting

confidence: 62%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Paloma: A Magnetic Cv Between Polars and Intermediate Polars

Joshi

Pandey

Singh

et al. 2016

ApJ

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Accretion Flows in Magnetic Cataclysmic Variables

Norton¹,

Somerscales

Parker³

et al. 2004

International Astronomical Union Colloquium

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ESUMENPreseiitainos los rosnltados d(' sirnulacionos quo exploran la variedad de flujos de acrecion posibles en variables cal-aclisiiiicas iiiay,iieliras (mCVs). Niiestras simulaciories evoliicionan hasta alcanzar periodos de equilibrio qne abarcaii 0.01 < /3;pir,/Porb < 0.6, y los flujos resultantes varian desde sistemas alimentados por disco en Pspin/Porb ~ 0.01 -0.1 a sistciiias alinuaitados por corrientes en Pspin/Porb ~ 0.1 -0.5 y sistemas alimentados d('sd(' un anillo ('ii el borde <'xl,ei ioi-del lobnlo de Roche de la enana blanca, en Pspin/Porb ~ 0.6. ABSTRACT '•V(' present l lu' results of simulations that explore the variety of accretion flows possible in magnetic cataclysmic variabk's (mCVs). Our simulations evolv(' to equilibrium periods spanning 0.01 < Pspin/Porb < 0.6 and the resulting flows vary from disc-fed systems at, Pspin/Porb ~ 0.01 -0.1, to stream fed systems at Pgpin/Porb 0 .1 -0.5 and systenns led from a ring at tlu' outer edge of the white dwarf's Roche lobe at Pspin/Porb ~ 0.6.

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ChandraObservation of V426 Ophiuchi: Weighing the Evidence for a Magnetic White Dwarf

Homer

Szkody

Raymond

et al. 2004

ApJ

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We report the results of a 45 ks Chandra observation of the cataclysmic variable V426 Ophiuchus. The high resolution spectrum from the high-energy transmission grating spectrometer is most consistent with a cooling flow model, placing V426 Oph among the group of CVs including U Gem and EX Hya. An uninterrupted lightcurve was also constructed, in which we detect a significant 4.2 hr modulation together with its first harmonic at 2.1 hrs. Reanalysis of archival Ginga and ROSAT X-ray lightcurves also reveals modulations at periods consistent with 4.2 and/or 2.1 hrs. Furthermore, optical photometry in V, simultaneous with the Chandra observation, indicates a modulation anti-correlated with the X-ray, and later more extensive R band photometry finds a signal at ∼2.1 hrs. The earlier reported X-ray periods at ∼0.5 and 1 hrs appear to be only transient and quasi-periodic in nature. In contrast, the 4.2 hr period or its harmonic are stable and persistent in X-ray/optical data from 1988 to 2003. This periodicity is clearly distinct from the 6.85 hr orbit, and could be due to the spin of the white dwarf. If this is the case, V426 Oph would be the first long period intermediate polar with a ratio P spin /P orb of 0.6. However, this interpretation requires unreasonable values of magnetic field strength and mass accretion rate.

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The Spin Periods of Magnetic Cataclysmic Variables

Cited by 9 publications

References 42 publications

Paloma: A Magnetic Cv Between Polars and Intermediate Polars

Paloma: A Magnetic Cv Between Polars and Intermediate Polars

Accretion Flows in Magnetic Cataclysmic Variables

ChandraObservation of V426 Ophiuchi: Weighing the Evidence for a Magnetic White Dwarf

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