The evolution of viscous discs - I. Mass transfer variations

Bath, G. T.; Pringle, J. E.

doi:10.1093/mnras/194.4.967

Cited by 140 publications

(85 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The model by Bath & Pringle (1981) shows that both the disk luminosity and structure settle down in a time considerably shorter than the observed main outburst. The observed very slow decay can be explained if the mass inflow rate from the donor to the disk,ṁ tr , becomes a significant fraction of the mass accretion rate from the disk onto the NS,ṁ acc during the outburst (Eq.…”

Section: Discussionmentioning

confidence: 92%

Echo outbursts in KS 1731–260

Šimon

2010

A&A

View full text Add to dashboard Cite

Context. The thermal-viscous instability of the accretion disk is thought to play an important role in the activity of low-mass X-ray binaries (LMXBs). It should also appear when a (quasi)persistent LMXB goes into its low state. Aims. We analyze the long-term X-ray activity of the neutron star LMXB KS 1731-260 during a part of its long main outburst and a complicated transition back to the low state (quiescence). We pay special attention to the variations during the state transition. Methods. We make use of the ASM/RXTE observations for a timeseries analysis of the longterm variations and investigation of the X-ray color changes in the 1.5-12 keV passband. Results. In our interpretation, the mass transfer rateṁ tr between the donor and neutron star significantly increased during the main outburst of KS 1731-260, which prolonged this event by keeping the disk ionized to its outer rim. Later on, a considerable fraction of the outer part of the disk was rapidly brought out of steady-state whenṁ tr decreased again. Only a slow decrease ofṁ tr continued even after the end of the main outburst. This lead to the formation of the central disk region, which was kept thermally stable, ionized by irradiation, and was surrounded by the outer, thermally unstable disk region. This configuration triggered the series of the echo outbursts. These outbursts are outside-in, caused by the still continuingṁ tr via the mass stream impinging the outer rim of the disk without overflow. We argue that introducing any strong bursts of matter from the donor to the disk as the cause of the echo outbursts is superfluous. The spectral evolution suggests that the disk returns to steady-state during the maxima of the echo outbursts. The X-ray emission between the echo outbursts is much higher than in the true quiescence and can be due to the ongoingṁ tr . We place the peculiar long-term activity of KS 1731-260 in the context of the systems with the echo outbursts, both soft X-ray transients and dwarf novae.

show abstract

Section: Discussionmentioning

confidence: 92%

Echo outbursts in KS 1731–260

Šimon

2010

A&A

View full text Add to dashboard Cite

show abstract

“…For this computation we have taken Rmin = 5AU and Rmax = 1056AU. We use a radial grid of 400 points equally spaced in √ R (Bath & Pringle 1981). At time t = 0, mass is injected steadily and the number density starts growing, creating a spike around 85AU.…”

Section: Evolution To the Steady State Of An α Disc With Fixed Tempermentioning

confidence: 99%

A self-consistent model for the evolution of the gas produced in the debris disc of β Pictoris

Kral¹,

Wyatt²,

Carswell³

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

View full text Add to dashboard Cite

This paper presents a self-consistent model for the evolution of gas produced in the debris disc of β Pictoris. Our model proposes that atomic carbon and oxygen are created from the photodissociation of CO, which is itself released from volatile-rich bodies in the debris disc due to grain-grain collisions or photodesorption. While the CO lasts less than one orbit, the atomic gas evolves by viscous spreading resulting in an accretion disc inside the parent belt and a decretion disc outside. The temperature, ionisation fraction and population levels of carbon and oxygen are followed with the photodissociation region model Cloudy, which is coupled to a dynamical viscous α model. We present new gas observations of β Pic, of C I observed with APEX and O I observed with Herschel, and show that these along with published C II and CO observations can all be explained with this new model. Our model requires a viscosity α > 0.1, similar to that found in sufficiently ionised discs of other astronomical objects; we propose that the magnetorotational instability is at play in this highly ionised and dilute medium. This new model can be tested from its predictions for high resolution ALMA observations of C I. We also constrain the water content of the planetesimals in β Pic. The scenario proposed here might be at play in all debris discs and this model could be used more generally on all discs with C, O or CO detections.

show abstract

“…To calculateK we replaced in relation (5) R g by R disk and T eff, g by T edge, disk , using relations (A.2) and (A.3). The characteristic disk temperature and the temperature distribution from the stellar surface to the edge of the disk were calculated from the model of Bath & Pringle (1981). Horne (1985) developed a method of eclipse mapping of accretion disks with this model, and Rutten et al (1992) applied the latter method to construct models of accretion disks for six cataclysmic variables.…”

Section: A2 Three Gainers With An Accretion Diskmentioning

confidence: 99%

Mass loss out of close binaries

Rensbergen

Greve

Mennekens

et al. 2011

A&A

View full text Add to dashboard Cite

Context. Several authors have previously introduced liberal evolution of interacting binaries, with the purpose of meeting various observed binary characteristics better than with conservative evolution. Since Algols are eclipsing binaries, the distribution of their orbital periods is known precisely. The distribution of their mass ratios contains, however, more uncertainties. We try to reproduce these two distributions theoretically using a liberal scenario in which the gainer star can lose mass into interstellar space as a consequence of its rapid rotation and the energy of a hot spot. Aims. In a recent paper we calculated the liberal evolution of binaries with a B-type primary at birth where mass transfer starts during core hydrogen burning of the donor. In this paper we include the cases where mass transfer starts during shell hydrogen burning, and it is our aim to reproduce the observed distributions of the system parameters of Algol-type semidetached systems. Methods. Our calculations reveal the amount of time that an Algol binary lives with a well-defined value of mass ratio and orbital period. We used these data to simulate the distribution of mass ratios and orbital periods of Algols. Results. Binaries with a late B-type initial primary hardly lose any mass, whereas those with an early B primary evolve in a nonconservative way. Conservative binary evolution predicts only ∼12% of Algols with a mass ratio q above 0.4. This value is raised up to ∼17% using our scenario of liberal evolution, which is still far below the ∼45% that is observed. Conclusions. Observed orbital periods of Algol binaries longer than one day are faithfully reproduced by our liberal scenario. Mass ratios are reproduced better than with conservative evolution, but the resemblance is still poor.

show abstract

The evolution of viscous discs - I. Mass transfer variations

Cited by 140 publications

References 0 publications

Echo outbursts in KS 1731–260

Echo outbursts in KS 1731–260

A self-consistent model for the evolution of the gas produced in the debris disc of β Pictoris

Mass loss out of close binaries

Contact Info

Product

Resources

About