Disc–magnetosphere interactions in cataclysmic variable stars

Hellier, C.

doi:10.1017/s1743921307009684

Cited by 37 publications

(44 citation statements)

References 73 publications

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“…In these progenitor systems an accreting CO WD reaches the Chandrasekhar limit and explodes. Observationally, these systems manifest themselves as cataclysmic variables (Hellier 2001), symbiotic systems (Kenyon 1986), and supersoft X-ray sources (van den Heuvel et al 1992;Kahabka & van den Heuvel 1997), depending on the companion star mass, its evolutionary status, and the masstransfer rate. It should be noted that the classification scheme overlaps somewhat on certain aspects.…”

Section: Accretion Onto a White Dwarfmentioning

confidence: 99%

Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

Tauris

Sanyal

Yoon

et al. 2013

A&A

142

181

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Context. Millisecond pulsars (MSPs) are generally believed to be old neutron stars (NSs), formed via type Ib/c core-collapse supernovae (SNe), which have been spun up to high rotation rates via accretion from a companion star in a low-mass X-ray binary (LMXB). In an alternative formation channel, NSs are produced via the accretion-induced collapse (AIC) of a massive white dwarf (WD) in a close binary. Aims. Here we investigate binary evolution leading to AIC and examine if NSs formed in this way can subsequently be recycled to form MSPs and, if so, how they can observationally be distinguished from pulsars formed via the standard core-collapse SN channel in terms of their masses, spins, orbital periods and space velocities. Methods. Numerical calculations with a detailed stellar evolution code were used for the first time to study the combined pre-and post-AIC evolution of close binaries. We investigated the mass transfer onto a massive WD (treated as a point mass) in 240 systems with three different types of non-degenerate donor stars: main-sequence stars, red giants, and helium stars. When the WD is able to accrete sufficient mass (depending on the mass-transfer rate and the duration of the accretion phase) we assumed it collapses to form a NS and we studied the dynamical effects of this implosion on the binary orbit. Subsequently, we followed the mass-transfer epoch which resumes once the donor star refills its Roche lobe and calculated the continued LMXB evolution until the end. Results. We show that recycled pulsars may form via AIC from all three types of progenitor systems investigated and find that the final properties of the resulting MSPs are, in general, remarkably similar to those of MSPs formed via the standard core-collapse SN channel. However, as a consequence of the fine-tuned mass-transfer rate necessary to make the WD grow in mass, the resultant MSPs created via the AIC channel preferentially form in certain orbital period intervals. In addition, their predicted small space velocities can also be used to identify them observationally. The production time of NSs formed via AIC can exceed 10 Gyr which can therefore explain the existence of relatively young NSs in globular clusters. Our calculations are also applicable to progenitor binaries of SNe Ia under certain conditions.

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Section: Accretion Onto a White Dwarfmentioning

confidence: 99%

Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

Tauris

Sanyal

Yoon

et al. 2013

A&A

142

181

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“…Among them are Livio & Shaviv (1984), Hack & La Dous (1990, 1993, Warner (1995), Hellier (2001). Several older reviews also provide an in-depth discussion of CVs, including La Dous (1994) and Patterson (1994).…”

Section: Introductionmentioning

confidence: 99%

An intrinsic source of reddening in the cataclysmic variable SS Cygni

Gaudenzi

Giovannelli

Mandalari

et al. 2010

A&A

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By using the INES archive of the IUE satellite, we analyzed the spectra of SS Cygni in quiescence in order to determine the value of the reddening of the binary system. The reddening of the system is reported in the literature with values that vary significantly from one another. The results demonstrate that the reddening is comprised by two components: the first, interstellar in origin, with a value E(B − V) = 0.04 ± 0.02 mag, and the second, intrinsic to the binary system, with values up to E(B − V) = 0.16 ± 0.02 mag. The intrinsic value of the reddening is variable along the quiescent phase and with orbital phase.

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“…These systems are composed of a white dwarf orbited every ∼80 min by a brown dwarf, the mass of the latter being of the order of a mere ∼0.06 M (Hellier 2001), which is below the limit for stable hydrogen burning in the core. The mass transfer rate in this kind of system is extremely low, ∼10 −12 M /yr, and unable to sustain the presence of the nebula.…”

Section: Discussionmentioning

confidence: 99%

“…This kind of classification is sound, given the presence of early superhumps, the large amplitude of the recorded outburst, and its rarity (no previous outbursts recorded). WZ Sge stars are an extreme case of SU UMatype CVs, with intervals between superoutbursts lasting decades, while normal outbursts are few and far in between (Hellier 2001). WZ Sge itself undergoes a superoutburst every ∼30 yr (events recorded in 1913, 1946, 1978and 2001Kuulker et al 2011) and has never been seen to undergo a normal outburst in between.…”

Section: Introductionmentioning

confidence: 99%

“…WZ Sge stars are an extreme case of SU UMatype CVs, with intervals between superoutbursts lasting decades, while normal outbursts are few and far in between (Hellier 2001). WZ Sge itself undergoes a superoutburst every ∼30 yr (events recorded in 1913, 1946, 1978and 2001Kuulker et al 2011) and has never been seen to undergo a normal outburst in between. At the opposite end of SU UMa-type of CVs are the ER UMa stars, which spend typically a third to half of their time in superoutbursts, going into one every one to two months.…”

Section: Introductionmentioning

confidence: 99%

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Outburst evolution, historic light curve and a flash-ionized nebula around the WZ Sge-type object PNV J03093063+2638031

Munari

Jurdana-Šepić

Ochner

et al. 2015

A&A

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We have monitored the 2014 superoutburst of the WZ Sge-type transient PNV J03093063+2638031 for more than four months, from V = 11.0 maximum brightness down to V = 18.4 mag, close to quiescence value, by obtaining BVR C I C photometry and low resolution fluxed spectroscopy. The evolution was normal and no late-time "echo" outbursts were observed. The absolute integrated flux of emission lines kept declining along the superoutburst, and their increasing contrast with the underlying continuum was simply the result of the faster decline of the continuum compared to the emission lines. Inspection of historical Harvard plates covering the 1899-1981 period did not reveal previous outbursts, neither "normal" nor "super". We discovered an extended emission nebula (radius ∼1 arcmin) around PNV J03093063+2638031, that became visible for a few months as the result of photo-ionization from the superoutburst of the central star. The nebula is not present on Palomar I and II sky survey images and it quickly disappeared when the outburst was over. From the rate at wich the ionization front swept through the nebula, we derive a distance of ∼120 pc to the system. The nebula is density bounded with an outer radius of 0.03 pc, and the absolute magnitude of the central star in quiescence is M V ∼ 14.2 mag. The electron density in the nebula is estimated to be 10 5 cm −3 from the observed recombination time scale. Given the considerable substructures seen across the nebula, a low filling factor is inferred. Similar nebulae have not been reported for other WZ Sge objects and the challenges posed to models are considered.

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Disc–magnetosphere interactions in cataclysmic variable stars

Cited by 37 publications

References 73 publications

Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

An intrinsic source of reddening in the cataclysmic variable SS Cygni

Outburst evolution, historic light curve and a flash-ionized nebula around the WZ Sge-type object PNV J03093063+2638031

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