The disc instability model of dwarf novae and low-mass X-ray binary transients

By Jan Lasota. 2001

644 citations recorded by the source corpus.

Abstract The disc instability model which is supposed to describe outbursts of dwarf nova and low-mass X-ray binary transient systems is presented and reviewed in detail. Various deficiencies of the model are pointed out and various remedies and generalizations are presented and discussed.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/bc4827bfb52cd5fa144002ebd5a0eb3cfc277e17

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In Astronomy and Astrophysics

Citations in the corpus

CONSTRAINTS ON BLACK HOLE GROWTH, QUASAR LIFETIMES, AND EDDINGTON RATIO DISTRIBUTIONS FROM THE SDSS BROAD-LINE QUASAR BLACK HOLE MASS FUNCTION (2010, background): “The ionization instability has been invoked to explain the outbursts seen in dwarf novae and soft X-ray transients (for a review see Lasota 2001), and the radiationpressure instability has been invoked to explain the outbursts seen in the microquasar GRS 1915+105 (e.g., Nayakshin et al. 2000;…”
Constraining the mass and radius of neutron stars in globular clusters (2017, background): “…of LMXBs, the material falling from the companion star piles up in an accretion disk around the NS, where it builds up for months to years until the disk becomes dense and hot enough to become partly ionized, leading to increased viscosity and flow of matter down onto the NS (e.g. Lasota 2001).”
Global simulations of axisymmetric radiative black hole accretion discs in general relativity with a mean-field magnetic dynamo (2014, background): “This fact inevitably leads either to a local runaway collapse or expansion of the disk, and may trigger a large scale evolution of the disc structure (limit cycle) similar to the one seen in dwarf nova outbursts (see Lasota 2001, for a review).”
No observational proof of the black-hole event-horizon (2002, background): “The accreting matter forms a disc whose instabilities trigger outbursts (see Lasota 2001 for a review of the instability model).”
Testing Accretion Disk Theory in Black Hole X-Ray Binaries (2006, result): “At first sight, this appears inconsistent with the α ≥ 0.1 values inferred for the outburst phases of dwarf novae (Lasota 2001) and soft X-ray transients (e.g. Dubus et al. 2001).”
THE EVOLUTION OF CATACLYSMIC VARIABLES AS REVEALED BY THEIR DONOR STARS (2011, methodology): “According to the disk instability model (DIM) for DN eruptions (e.g., Osaki 1996; Lasota 2001), these CV sub-classes are differentiated primarily by the rate at which mass is supplied to the accretion disk.”
X-Ray Emissions from Accreting White Dwarfs: A Review (2017, background): “Byckling et al. (2010) used a sample with parallax based distances10, and derived a luminosity in the 1030–1032 ergs s−1 range, which requires an accretion rate that is many times higher than can be achieved through a cold disk (Lasota 2001).”
WATCHDOG: A COMPREHENSIVE ALL-SKY DATABASE OF GALACTIC BLACK HOLE X-RAY BINARIES (2015, methodology): “…to outburst occurs as a consequence of instabilities, both thermal and viscous in nature, developing in the accretion disk that cause more rapid mass transfer onto the BH and lead to bright X-ray emission (Meyer & Meyer-Hofmeister 1981; Cannizzo et al. 1995; King & Ritter 1998; Lasota 2001).”
Explaining changing-look AGN with state transition triggered by rapid mass accretion rate drop (2018, background): “This results in a heating front propagating inwards, traveling at a speed which is shorter than the MNRAS 000, 1–10 (2015) viscous timescale by a factor (H/R) (Hameury et al. 1998; Dubus et al. 2001; Lasota 2001; Hameury et al. 2009).”
X-Ray Properties of Black-Hole Binaries (2006, methodology): “This model was developed initially for dwarf novae (e.g., Smak 1971; Lasota 2001) and extended to X-ray novae (e.g., Dubus et al. 2001).”
Accretion disc viscosity: how big is alpha? (2007, methodology): “There is now general agreement that these outbursts result from the presence of ionization zones within the disc, allowing this to switch between a cool, low-ionization, low-viscosity state, and a hot, highly ionized, highviscosity state (see Lasota 2001, for a recent review).”