Circumstellar and circumbinary discs in eccentric stellar binaries

Pichardo, B.; Sparke, Linda S.; Aguilar, L. A.

doi:10.1111/j.1365-2966.2005.08905.x

Cited by 176 publications

(199 citation statements)

References 53 publications

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“…This is because the truncation and stellar radii are very similar, so any disc would have to be very small indeed (Pichardo, Sparke, & Aguilar 2005;Garcia et al 2013). Instead we model the accretion as falling directly from the corotation radius of each star (Da Rio et al 2014).…”

Section: Resultsmentioning

confidence: 99%

“…A disc around the primary would be truncated at R trunc = 4 R , and the secondary disc at R trunc = 3 R (Pichardo et al 2005;Garcia et al 2013). Comparing this with the stellar radii themselves (respectively 3.3 and 2.5 R ; Böhm et al 2004;Fumel & Böhm 2012) clearly shows that any discs will be small indeed.…”

Section: Numerical Limitations and Omissions From The Modelmentioning

confidence: 99%

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Precession and accretion in circumbinary discs: the case of HD 104237

Dunhill

Cuadra

Dougados

2015

Monthly Notices of the Royal Astronomical Society

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We present the results of smoothed particle hydrodynamics (SPH) simulations of the disc around the young, eccentric stellar binary HD 104237. We find that the binary clears out a large cavity in the disc, driving a significant eccentricity at the cavity edge. This then precesses around the binary at a rate of˙ = 0.48 • T −1 b , which for HD 104237 corresponds to a precession period of 40 years. We find that the accretion pattern into the cavity and onto the binary changes with this precession, resulting in a periodic accretion variability driven purely by the physical parameters of the binary and its orbit. For each star we find that this results in order of magnitude changes in the accretion rate. We also find that the accretion variability allows the primary to accrete gas at a higher rate than the secondary for approximately half of each precession period. Using a large number of 3-body integrations of test particles orbiting different binaries, we find good agreement between the precession rate of a test particle and our SPH disc precession. These rates also agree very well with the precession rates predicted by the analytic theory of Leung & Lee (2013), showing that their prescription can be accurately used to predict long-term accretion variability timescales for eccentric binaries accreting from a disc. We discuss the implications of our result, and suggest that this process provides a viable way of preserving unequal mass ratios in accreting eccentric binaries in both the stellar and supermassive black hole regimes.

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Section: Resultsmentioning

confidence: 99%

Section: Numerical Limitations and Omissions From The Modelmentioning

confidence: 99%

Precession and accretion in circumbinary discs: the case of HD 104237

Dunhill

Cuadra

Dougados

2015

Monthly Notices of the Royal Astronomical Society

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“…In viscous evolution, the timescale of dissipation is given by t ∝ R 2 out . The R out of binary systems depends upon the semi-major axis a, being approximated by ∼a/3 (e.g., Artymowicz & Lubow 1994;Pichardo et al 2005). Therefore, the peak in the EF distribution is difficult to reproduce assuming viscous evolution alone, since more time is required to disperse the dust disk as the binary separation (hence the disk size) increases.…”

Section: Mechanism Of Dust Dispersal In Binary Systemsmentioning

confidence: 99%

“…In addition, EF model (a < ∼ 40 AU) ∼ 20-40% is assumed based on the report by Cieza et al (2009). Adopting a truncation radius of R out = 0.337a found in the systems of mass ratio q ≡ M s /M p = 1 with low-eccentricity (Pichardo et al 2005), the EF can be estimated as a function of R out over three separation regions; R out < ∼ 10 AU, R out ∼ 100-150 AU, and R out > ∼ 150 AU. From the above arguments, the EF model (R out )'s in the three separation regions are varied around ∼20, 100, and 70%, respectively.…”

Section: Ef Distribution As a Function Of Disk Outer Radiusmentioning

confidence: 99%

Study of infrared excess from circumstellar disks in binaries with Spitzer/IRAC

Itoh

Fukagawa

Shibai

et al. 2015

Publications of the Astronomical Society of Japan

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The presence of excess emission at 3.6-8.0 µm was investigated in a sample of 27 binary systems located in two nearby star-forming regions, Taurus and Ophiuchus, by using Spitzer/Infrared Array Camera (IRAC) archival data. Angular (Projected) separations for the binaries are greater than 2 ′′ (∼280 AU), which allowed us to perform spatially resolved photometry of individual primary and secondary sources. The measured occurrence of infrared excess suggests that binarity plays a role in the evolution of circumstellar disks, even at such wide binary separations. Most of the binaries have excess emission from both the circumprimary and circumsecondary disks, or show photospheric levels for both components at all four wavelengths of IRAC. On the other hand, four systems (17 +11 −8 %, designated by "mixed" systems) exhibit excess emission from a single binary component. This ratio is significantly smaller than that predicted by the random pairing of single stars, suggesting that circumprimary and circumsecondary disks are synchronously dispersed. In addition, the excess frequencies (EFs) of primary and secondary sources with a projected distance of a p ≃ 280-450 AU are 100 +0 −17 % and 91 +8 −18 %, respectively, and significantly higher than that of single stars (70 ± 5%). We made a simple model describing the EF distribution as a function of the disk outer radius, R out . Comparisons with observations using the Kolmogorov-Smirnov test show that the observational data are consistent with the model when the EF ≃ 1 region is found at R out ∼ 30-100 AU. This disk radius is smaller than that typically estimated for single stars. The high EF of circumstellar disks with these radii may indicate a prolonged lifetime of dust in binary systems possibly because smaller disks counteract mass loss by photoevaporation.

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“…If we assume that the system was about 1.4 times closer before the mass loss of the white dwarf progenitor star (Weidemann 2000), such a close companion yields only a small long time stable region for planets (only 1.7 AU, Holman & Wiegert 1997). The same holds for the size of the protoplanetary disk in which the planet formation process took place (Pichardo et al 2005), posing a problem to the theory of planet formation. Nevertheless, a massive planet (msin(i) =4 M Jup , Queloz et al 2000) had been formed in this environment and finally also survived the post main sequence evolution of the white dwarf progenitor star.…”

Section: Introductionmentioning

confidence: 99%