Stability of helium accretion discs in ultracompact binaries

Lasota, Jean–Pierre; Dubus, G.; Kruk, K.

doi:10.1051/0004-6361:200809658

Cited by 100 publications

(170 citation statements)

References 45 publications

Supporting

Mentioning

160

Contrasting

Unclassified

Order By: Relevance

“…Using the ultracompact X-ray binary evolution track of Deloye & Bildsten (2003), we can thus predict an orbital period of 50 minutes for this system. If the NS experiences enhanced neutrino cooling, then the mass transfer rate would be higher, and the orbital period could be lower, down to 21 minutes (the minimum for transient helium-accreting ultracompact X-ray binaries; Lasota, Dubus & Kruk 2008).…”

Section: Discussionmentioning

confidence: 99%

Improved mass and radius constraints for quiescent neutron stars in ω Cen and NGC 6397

Heinke¹,

Cohn²,

Lugger³

et al. 2014

Monthly Notices of the Royal Astronomical Society

113

155

View full text Add to dashboard Cite

We use Chandra and XMM-Newton observations of the globular clusters ω Cen and NGC 6397 to measure the spectrum of their quiescent neutron stars (NSs), and thus to constrain the allowed ranges of mass and radius for each. We also use Hubble Space Telescope photometry of NGC 6397 to identify a potential optical companion to the quiescent NS, and find evidence that the companion lacks hydrogen. We carefully consider a number of systematic problems, and show that the choices of atmospheric composition, interstellar medium abundances, and cluster distances can have important effects on the inferred NS mass and radius. We find that for typical NS masses, the radii of both NSs are consistent with the 10 − 13 km range favored by recent nuclear physics experiments. This removes the evidence suggested by Guillot and collaborators for an unusually small NS radius, which relied upon the small inferred radius of the NGC 6397 NS.

show abstract

Section: Discussionmentioning

confidence: 99%

Improved mass and radius constraints for quiescent neutron stars in ω Cen and NGC 6397

Heinke¹,

Cohn²,

Lugger³

et al. 2014

Monthly Notices of the Royal Astronomical Society

113

155

View full text Add to dashboard Cite

show abstract

“…The threshold luminosities in these refined expressions are up to 2 orders of magnitude higher for P orb < 1 h. The luminosity derived from the burst energetics of (3.1±2.3)×10 35 erg s −1 is consistent with a persistently accreting helium disk only if P orb is smaller than 6 min (1σ confidence), or 7 min (2σ confidence). For a carbon-oxygen-rich disk, this limit would be even more extreme because of higher ionization potentials of these atoms (Lasota et al 2008;Menou et al 2002). For a hydrogen disk P orb would be smaller than 35 min, which is impossible because a hydrogen dwarf would not fit within such an orbit (e.g., Nelson et al 1986;Nelemans 2008).…”

Section: Discussionmentioning

confidence: 99%

Monitoring campaign of 1RXS J171824.2–402934, the low-mass X-ray binary with the lowest mass accretion rate

Zand¹,

Jonker

Bassa

et al. 2009

A&A

View full text Add to dashboard Cite

An X-ray monitoring campaign with Chandra and Swift confirms that 1RXS J171824.2-402934 is accreting at the lowest rate among the known persistently accreting low-mass X-ray binaries. A thermonuclear X-ray burst was detected with the all-sky monitor on RXTE. This is only the second such burst seen in 1RXS J171824.2-402934 in more than 20 Ms of observations done over 19 years. The low burst recurrence rate is in line with the low accretion rate. The persistent nature and low accretion rate can be reconciled within accretion disk theory if the binary system is ultracompact. An unprecedentedly short orbital period of less than ≈7 min would be implied. An ultracompact nature, together with the properties of the type I X-ray burst, suggests, in turn, that helium-rich material is accreted. Optical follow-up of the Chandra error region does not reveal an unambiguous counterpart.

show abstract

“…An additional critical rate is associated with the stability of the accretion disk since we assume that the pulsar can turn on during the quiescent state of the system when it exhibits X-ray transient phenomena (see below). The latter critical accretion rate depends upon the composition of the disk and on the degree of irradiation (Lasota, Dubus & Kruk 2008). For a helium (He) star or He WD we use the He disk models, whereas H disk models are used for MS or giant star companions.…”

Section: Distinguishing Between Accretion Ablation and Propellermentioning

confidence: 99%

“…For a helium (He) star or He WD we use the He disk models, whereas H disk models are used for MS or giant star companions. For simplicity we only consider the irradiated disk models (Lasota, Dubus & Kruk 2008) and assume that the outer edge of the disk extends to 0.8 times the NS Roche radius, however, we included the non-irradiated case as an option within BSE. The pure hydrogen equation is (Lasota, Dubus & Kruk 2008; Appendix A), M irr = 1.5 × 10 −11 R 2.39 10 M −0.64…”

Section: Distinguishing Between Accretion Ablation and Propellermentioning

confidence: 99%

See 1 more Smart Citation

Accretion, ablation and propeller evolution in close millisecond pulsar binary systems

Kiel¹,

Taam²

2013

Astrophys Space Sci

View full text Add to dashboard Cite

A model for the formation and evolution of binary millisecond radio pulsars in systems with low mass companions (< 0.1 M ⊙ ) is investigated using a binary population synthesis technique. Taking into account the non conservative evolution of the system due to mass loss from an accretion disk as a result of propeller action and from the companion via ablation by the pulsar, the transition from the accretion powered to rotation powered phase is investigated. It is shown that the operation of the propeller and ablation mechanisms can be responsible for the formation and evolution of black widow millisecond pulsar systems from the low mass X-ray binary phase at an orbital period of ∼ 0.1 day. For a range of population synthesis input parameters, the results reveal that a population of black widow millisecond pulsars characterized by orbital periods as long as ∼ 0.4 days and companion masses as low as ∼ 0.005 M ⊙ can be produced. The orbital periods and minimum companion mass of this radio millisecond pulsar population critically depend on the thermal bloating of the semi-degenerate hydrogen mass losing component, with longer orbital periods for a greater degree of bloating. Provided that the radius of the companion is increased by about a factor of 2 relative to a fully degenerate, zero temperature configuration, an approximate agreement between observed long orbital periods and theoretical modeling of hydrogen rich donors can be achieved. We find no discrepancy between the estimated birth rates for LMXBs and black

show abstract

Stability of helium accretion discs in ultracompact binaries

Cited by 100 publications

References 45 publications

Improved mass and radius constraints for quiescent neutron stars in ω Cen and NGC 6397

Improved mass and radius constraints for quiescent neutron stars in ω Cen and NGC 6397

Monitoring campaign of 1RXS J171824.2–402934, the low-mass X-ray binary with the lowest mass accretion rate

Accretion, ablation and propeller evolution in close millisecond pulsar binary systems

Contact Info

Product

Resources

About