Relevant bibliographies by topics / Accretion discs

Academic literature on the topic 'Accretion discs'

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Published: 4 June 2021
Last updated: 7 September 2023

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Journal articles on the topic "Accretion discs"

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Joshi, Gandhali D., Annalisa Pillepich, Dylan Nelson, Federico Marinacci, Volker Springel, Vicente Rodriguez-Gomez, Mark Vogelsberger, and Lars Hernquist. "The fate of disc galaxies in IllustrisTNG clusters." Monthly Notices of the Royal Astronomical Society 496, no. 3 (June 12, 2020): 2673–703. http://dx.doi.org/10.1093/mnras/staa1668.

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ABSTRACT We study the stellar morphological evolution of disc galaxies within clusters in the TNG50 and TNG100 runs from the IllustrisTNG simulation suite. We select satellites of masses 109.7 ≤ M*, z = 0/M⊙ ≤ 1011.6 residing in clusters of masses 1014 ≲ M200c, z = 0/M⊙ ≤ 1014.6 at z = 0 and that were discs at accretion according to a kinematic morphology indicator (the circularity fraction). These are traced from the time of accretion to z = 0 and compared to a control sample of central galaxies mass-matched at accretion. Most cluster discs become non-discy by z = 0, in stark contrast with the control discs, of which a significant fraction remains discy over the same timescales. Cluster discs become non-discy accompanied by gas removal and star formation quenching, loss of dark matter, and little growth or a loss of stellar mass. In contrast, control discs transform while also losing gas mass and quenching, but growing significantly in dark matter and stellar mass. Most cluster satellites change morphologies on similar timescales regardless of stellar mass, in ∼0.5–4 Gyr after accretion. Cluster discs that experienced more numerous and closer pericentric passages show the largest change in morphology. Morphological change in all cases requires the presence of a gravitational perturbation to drive stellar orbits to non-discy configurations, along with gas removal/heating to prevent replenishment of the disc through continued star formation. For cluster discs, the perturbation is impulsive tidal shocking at pericentres and not tidal stripping of outer disc stellar material, whereas for control discs, a combination of mergers and feedback from active galactic nuclei appears to be the key driving force behind morphological transformations.
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Abramowicz, Marek, and Odele Straub. "Accretion discs." Scholarpedia 9, no. 8 (2014): 2408. http://dx.doi.org/10.4249/scholarpedia.2408.

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Hameury, J. M., and J. P. Lasota. "Models of ultraluminous X-ray transient sources." Astronomy & Astrophysics 643 (November 2020): A171. http://dx.doi.org/10.1051/0004-6361/202038857.

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Context. It is now widely accepted that most ultraluminous X-ray sources (ULXs) are binary systems whose large (above 1039 erg s−1) apparent luminosities are explained by super-Eddington accretion onto a stellar-mass compact object. Many of the ULXs, especially those containing magnetized neutron stars, are highly variable; some exhibit transient behaviour. Large luminosities might imply large accretion discs that could be therefore prone to the thermal–viscous instability known to drive outbursts of dwarf novae and low-mass X-ray binary transient sources. Aims. The aim of this paper is to extend and generalize the X-ray transient disc-instability model to the case of large (outer radius larger than 1012 cm) accretion discs and apply it to the description of systems with super-Eddington accretion rates at outburst and, in some cases, super-Eddington mass transfer rates. Methods. We have used our disc-instability-model code to calculate the time evolution of the accretion disc and the outburst properties. Results. We show that, provided that self-irradiation of the accretion disc is efficient even when the accretion rate exceeds the Eddington value, possibly due to scattering back of the X-ray flux emitted by the central parts of the disc on the outer portions of the disc, heating fronts can reach the disc’s outer edge generating high accretion rates. We also provide analytical approximations for the observable properties of the outbursts. We have successfully reproduced the observed properties of galactic transients with large discs, such as V404 Cyg, as well as some ULXs such as M51 XT-1. Our model can reproduce the peak luminosity and decay time of ESO 243-39 HLX-1 outbursts if the accretor is a neutron star. Conclusions. Observational tests of our predicted relations between the outburst duration and decay time with peak luminosity would be most welcome.
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Vogel, M. "Photoionization models with accretion discs." International Astronomical Union Colloquium 103 (1988): 119–21. http://dx.doi.org/10.1017/s0252921100103252.

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AbstractThe diagnositic possibilities for identifying the ionizing source in symbiotic systems are explored. As possible sources we consider hot blackbodies and accretion discs. It turns out that main sequence accretors and hot blackbodies may have the same appearance in both, emission line and continuum flux distribution. However, UV continuum indices of models containing an accretion disc around a white dwarf are confined to a very small region, separated from main sequence accretors and blackbodies. Furthermore, if symbiotic systems containing a white dwarf accretor exist, they might be recognizable by strong emission in Fe X λ6374.
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Fraternali, Filippo, and Gabriele Pezzulli. "Angular Momentum Accretion onto Disc Galaxies." Proceedings of the International Astronomical Union 14, A30 (August 2018): 228–32. http://dx.doi.org/10.1017/s1743921319004125.

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AbstractThroughout the Hubble time, gas makes its way from the intergalactic medium into galaxies fuelling their star formation and promoting their growth. One of the key properties of the accreting gas is its angular momentum, which has profound implications for the evolution of, in particular, disc galaxies. Here, we discuss how to infer the angular momentum of the accreting gas using observations of present-day galaxy discs. We first summarize evidence for ongoing inside-out growth of star forming discs. We then focus on the chemistry of the discs and show how the observed metallicity gradients can be explained if gas accretes onto a disc rotating with a velocity 20 – 30% lower than the local circular speed. We also show that these gradients are incompatible with accretion occurring at the edge of the discs and flowing radially inward. Finally, we investigate gas accretion from a hot corona with a cosmological angular momentum distribution and describe how simple models of rotating coronae guarantee the inside-out growth of disc galaxies.
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Hure, J. M., and D. Richard. "Accretion Discs in AGN, Viscosity and Structure of Accretion Disks." EAS Publications Series 1 (2001): 53–61. http://dx.doi.org/10.1051/eas:2001008.

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Ginzburg, Sivan, and Eugene Chiang. "The endgame of gas giant formation: accretion luminosity and contraction post-runaway." Monthly Notices of the Royal Astronomical Society 490, no. 3 (October 16, 2019): 4334–43. http://dx.doi.org/10.1093/mnras/stz2901.

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ABSTRACT Giant planets are thought to form by runaway gas accretion on to solid cores. Growth must eventually stop running away, ostensibly because planets open gaps (annular cavities) in their surrounding discs. Typical models stop runaway by artificially capping the accretion rate and lowering it to zero over an arbitrarily short time-scale. In reality, post-runaway accretion persists as long as the disc remains. During this final and possibly longest phase of formation, when the planet is still emerging from the disc, its mass can more than double, and its radius contracts by orders of magnitude. By drawing from the theory of how gaps clear, we find that post-runaway accretion luminosities diverge depending on disc viscosity: luminosities fall in low-viscosity discs but continue to rise past runaway in high-viscosity discs. This divergence amounts to a factor of 102 by the time the disc disperses. Irrespective of the specifics of how planets interact with discs, the observed luminosity and age of an accreting planet can be used to calculate its instantaneous mass, radius, and accretion rate. We perform this exercise for the planet candidates embedded within the discs orbiting PDS 70, HD 163296, and MWC 758, inferring masses of 1–10 MJ, accretion rates of 0.1–10 MJ Myr−1, and radii of 1–10 RJ. Our radii are computed self-consistently from the planet’s concurrent contraction and accretion and do not necessarily equal the value of 2RJ commonly assumed; in particular, the radius depends on the envelope opacity as R ∝ κ0.5.
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Lyubarskij, Yu E., K. A. Postnov, and M. E. Prokhorov. "Eccentric accretion discs." Monthly Notices of the Royal Astronomical Society 266, no. 3 (February 1994): 583–96. http://dx.doi.org/10.1093/mnras/266.3.583.

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Chakrabarty, D., J. Murray, G. A. Wynn, and A. R. King. "Warped Accretion Discs." Symposium - International Astronomical Union 208 (2003): 385–86. http://dx.doi.org/10.1017/s0074180900207389.

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In this article we report the results of our numerical investigation of warped accretion discs in binary stellar systems. We perform complete 3-D hydrodynamic simulations of binary discs. The disc is rendered unstable to the warp mode under the action of the magnetic field of the companion star in the binary. The disc thus warped is noted to undergo retrograde precession with a precession period just slightly less than the binary period. This small difference in periods can explain the phenomenon of negative superhumps observed in a number of binaries. Besides the modal analysis based on Fourier transforms, warps were also studied by a simple and robust technique that we developed; this is based on an analysis of the azimuthal distributions of particles that lie above and below the mid-plane of the disc.
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BOGOVALOV, S. V., and S. R. KELNER. "ACCRETION AND PLASMA OUTFLOW FROM DISSIPATIONLESS DISCS." International Journal of Modern Physics D 19, no. 03 (March 2010): 339–65. http://dx.doi.org/10.1142/s0218271810016373.

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We consider the specific case of disc accretion for negligibly low viscosity and infinitely high electric conductivity. The key component in this model is the outflowing magnetized wind from the accretion disc, since this wind effectively carries away angular momentum of the accreting matter. Assuming magnetic field has variable polarity in the disc (to avoid magnetic flux and energy accumulation at the gravitational center), this leads to radiatively inefficient accretion of the disc matter onto the gravitational center. In such a case, the wind forms an outflow, which carries away all the energy and angular momentum of the accreted matter. Interestingly, in this framework, the basic properties of the outflow (as well as angular momentum and energy flux per particle in the outflow) do not depend on the structure of accretion disc. The self-similar solutions obtained prove the existence of such an accreting regime. In the self-similar case, the disc accretion rate (Ṁ) depends on the distance to the gravitational center, r, as [Formula: see text], where λ is the dimensionless Alfvenic radius. Thus, the outflow predominantly occurs from the very central part of the disc provided that λ ≫ 1 (it follows from the conservation of matter). The accretion/outflow mechanism provides transformation of the gravitational energy from the accreted matter into the energy of the outflowing wind with efficiency close to 100%. The flow velocity can essentially exceed the Kepler velocity at the site of the wind launch.
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Dissertations / Theses on the topic "Accretion discs"

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Kumar, S. "Twisted accretion discs." Thesis, University of Cambridge, 1985. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.372882.

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Ogilvie, Gordon Ian. "Magnetic fields in accretion discs." Thesis, University of Cambridge, 1998. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.624666.

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Matthews, Owen Martin. "Accretion discs around magnetic stars." Thesis, University of Leicester, 2004. http://hdl.handle.net/2381/30678.

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Accretion discs are commonplace around magnetic stars. They can be found in newly formed stars and in interacting binaries. The effects of the stellar magnetic field on these discs are manifold. For example it may act as a 'seed field' for the initiation of the magneto-rotational instability and thus drive viscosity. However this thesis explores the more direct effect of the stellar magnetic field on the global structure of circumstellar accretion discs, and how this structure may in turn influence the time dependent behaviour of the disc. This work is done through a combination of analytic and numerical techniques, by modelling a torque which represents the effect of the magnetic field.;Some young stellar objects exhibit disc outbursts, known as FU Orionis events, which are separated by recurrence times much longer than would be expected from the standard disc instability model. However, it is shown here that a moderate stellar magnetic field may truncate the accretion disc, and so stabilise the inner accretion disc against outbursts. This forces outbursts to begin in the outer disc where higher trigger densities must be reached, and so extends the recurrence time. This result is of great interest since planet formation may be strongly influenced by the structure of the protoplanetary disc.;The dwarf nova WZ Sagittae is unusual in that it also has very long recurrence times. In addition, a series of short echos have been observed to follow the main outburst. It has therefore been suggested that this object is surrounded by an accretion disc which is magnetically truncated in a similar manner to those around the FU Orionis stars. It is shown that such a truncated disc may, when placed within the binary Roche potential, exhibit echo outbursts.
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Ballantyne, D. R. "Ionized accretion discs around black holes." Thesis, University of Cambridge, 2002. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.596325.

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Many galaxies in the Universe show evidence of a supermassive black hole at their dynamical centre. About 10-20% of these galaxies also contain an extremely bright, point-like continuum source in their nuclear region. These luminous objects are called active galactic nuclei (AGN), and are thought to be powered by material accreting onto the central black hole. The infalling gas loses its energy and angular momentum by passing through an accretion disc. The disc then radiates away this energy, and it is this radiation that is observed as an AGN. When observed in the X-ray waveband AGN are found to be very bright and rapidly variable (on timescales as small as 1000 s), implying that the emission must originate from the innermost regions of the central engine. X-ray spectra of AGN often exhibit distinct features that are attributed to radiation reflecting off of the accretion disc. Therefore, it is possible to use sensitive X-ray spectroscopic observations of AGN to directly probe the physics of accretion flows only a short distance away from the black hole. Comparing the results from AGN with different properties, such as luminosity or radio power, may allow general conclusions on the AGN phenomenon to be drawn. This thesis applies computations of X-ray reflection spectra to observations of different AGN in order to determine various properties of their accretion flows. The calculations take into account the ionization effects of the incident radiation and consider different density structures for the surface of the accretion disc. It was found that the model spectra were a good description of the observed X-ray data for many AGN between 1 and 10 keV. In particular, five narrow-line Seyfert 1 galaxies were well fit with reflection spectra from a highly ionized accretion disc, consistent with the idea that they contain rapidly accreting black holes. A similar result was found when fitting the data of 3C 120, a broad-line radio galaxy, which argues against the claim that radio-loud AGN have truncated accretion discs. On the other hand, a weakly ionized reflector proved to be a better fit to the Seyfert 1 galaxy MCG-6-30-15.
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Young, Matthew Daniel. "Fragmentation of self-gravitating accretion discs." Thesis, University of Cambridge, 2015. https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.708572.

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Heron, Daniel Anthony Westwood. "The internal structure of alpha-accretion discs." Thesis, University of Leicester, 1997. http://hdl.handle.net/2381/30581.

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In this thesis we develop a mathematical model to describe the internal structure of an -accretion disc. The method is to consider the standard thin disc as a zero order approximation to a disc with vertical structure. The order of the approximation is controlled by the parameter 1/M2, where M is the Mach number of the azimuthal flow is a fiducial point. The theory is developed analytically as far as possible, using numerical solutions for the final system of ordinary differential equations only. The model expands upon the work of other authors by assuming a disc surface defined by the condition of pressure balance between the disc and its environment. Vertically transported angular momentum is extracted by coupling to these surroundings. In the absence of an external couple, the vertical transport of angular momentum is ignored, as in the standard thin disc. The internal structure and stability of the disc is investigated in both the gas and radiation pressure dominated regions, and the effects of including advection and the vertical transport of angular momentum is discussed. An application of the disc model is presented whereby external heating from X-rays associated with a radio jet are shown to induce mass loss from the disc surface. Such a configuration may undergo symmetry breaking to an asymmetric state in which one jet dominates. This is therefore a possible model for intrinsically one-sided radio sources.
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Billington, Ian Michael. "Images of accretion discs in cataclysmic variables." Thesis, University of Oxford, 1995. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.308377.

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Honey, William Bruce. "Observations of accretion discs in interacting binaries." Thesis, University of Oxford, 1989. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.277028.

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Dunhill, Alexander Charles. "Adventures with planets and binaries in accretion discs." Thesis, University of Leicester, 2013. http://hdl.handle.net/2381/28373.

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The primary idea behind the work in this thesis is that accretion discs interacting with astrophysical bodies, from planets to supermassive black holes (SMBHs), can strongly affect the dynamical behaviour of those bodies. While this idea is by no means new, observational and theoretical developments in recent years provide fresh motivation to consider this effect across a number of astrophysical contexts. Of particular relevance to the work here are three observational measurements which I attempt to reconcile with theory by invoking interactions with accretion discs. Firstly, observations of giant exoplanets show that they prefer to inhabit eccentric orbits, which is unexpected given the predictions of planet formation theory. Conversely, Kepler’s discovery of planets with low eccentricities around moderately eccentric binaries goes against theoretical expectation that their orbits should be eccentric. In galactic centres, binary supermassive black holes are not observed despite theoretical expectations that their evolution should drive them to ~ parsec separations and leave them there. In this thesis I use high-resolution smoothed particle hydrodynamics simulations to investigate each of these problems involving planet- and binary-disc interactions. I show that these interactions are unable to solve the problem of eccentric giant exoplanets, but that they can cause damping of circumbinary planetary eccentricity and so are able to explain Kepler’s circumbinary planets. I use this latter to place a limit on the surface density in which Kepler-16b in particular can have formed. I also show that a disc formed from a gas cloud moving prograde with respect to a SMBH binary will fragment to form stars sooner than a similar retrograde disc. Consequently, a retrograde disc is able to drive stronger binary evolution than is the prograde disc. Allowing that a large number of such encounters would be expected in the aftermath of the galaxy merger that formed the binary, this process may be able to solve the ‘last parsec problem.’
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Eckersall, Alexander James. "The accretion discs of transient X-ray binaries." Thesis, University of Leicester, 2018. http://hdl.handle.net/2381/42522.

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One of the larger questions within the study of X-ray Binaries currently concerns the geometry of the accretion disc during the so called ’hard state’. A model involving a truncated disc is often used to explain the properties of the hard state, but there is still disagreement on the extent to which it is necessary. Presented in this thesis are three studies related to this issue. The first looks into the changes in the accretion geometry using an argument based around radiative efficiency. Periods of exponential decay before and after the soft- to hard-state transition are found. The e-folding times of these decays are measured and it is found that this value changes from ~12 days in the soft state to ~7 days in the hard state. This factor ~2 change would be expected if there is a change from a radiatively efficient regime to a radiatively inefficient regimee. The second concerns the treatment of absorption from the Interstellar Medium in studies of X-ray Binaries. Column densities for the most abundant elements are found and compared with previous results for a number of sources. Simulated data is also used to test the impact of using incorrect column densities and older X-ray absorption models on spectral analysis. It is found that the use of incorrect absorption parameters can have a large effect on the results of spectral fitting. The third directly tests for the presence of a truncated disc by fitting a model to energy spectra from the XMM-Newton/EPIC-pn instrument. The model assumes the accretion disc extends down to rISCO at all times, and is fit to a large range of observations in both the hard and soft states. In the majority of cases there is no explicit need for a truncated disc in either the soft or hard state.
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Books on the topic "Accretion discs"

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Beskin, Vassily, Gilles Henri, François Menard, Guy Pelletier, and Jean Dalibard, eds. Accretion discs, jets and high energy phenomena in astrophysics. Berlin, Heidelberg: Springer Berlin Heidelberg, 2003. http://dx.doi.org/10.1007/b80353.

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S, Beskin V., North Atlantic Treaty Organization. Scientific Affairs Division., and Nato Advanced Study Institute (2002 : Les Houches, Haute-Savoie, France)., eds. Accretion discs, jets, and high energy phenomena in astrophysics =: Disques d'accrétion, jets et phénomènes de haute énergie en astrophysique : Ecole d'été de physique des Houches, Session LXXVIII, 29 July-23 August 2002 : Nato Advanced Study Institute, Euro Summer School, Ecole thématique du CNRS. Les Ulis: EDP Sciences, 2003.

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Meyer, Friedrich, Wolfgang J. Duschl, Juhan Frank, and Emmi Meyer-Hofmeister, eds. Theory of Accretion Disks. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-1037-9.

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Meyer-Hofmeister, Emmi, and Henk Spruit, eds. Accretion Disks — New Aspects. Berlin, Heidelberg: Springer Berlin Heidelberg, 1997. http://dx.doi.org/10.1007/bfb0105816.

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1928-, Meyer Friedrich, and NATO Advanced Research Workshop on Theory of Accretion Disks (1st : 1989 : Garching bei München (Germany)), eds. Theory of accretion disks. Dordrecht: Kluwer Academic Publishers, 1989.

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Katō, Shōji. Black-hole accretion disks. Kyoto, Japan: Kyoto University Press, 1998.

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Guessoum, Nidhal. Neutron viscosity in accretion disks. Greenbelt, MD: Laboratory for High Energy Astrophysics, NASA/Goddard Space Flight Center, 1990.

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Duschl, Wolfgang J., Juhan Frank, Friedrich Meyer, Emmi Meyer-Hofmeister, and Werner M. Tscharnuter, eds. Theory of Accretion Disks — 2. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0858-4.

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1958-, Duschl W. J., North Atlantic Treaty Organization. Scientific Affairs Division., and NATO Advanced Research Workshop on Theory of Accretion Disks (2nd : 1993 : Garching, Germany), eds. Theory of accretion disks--2. Dordrecht: Kluwer Academic, 1994.

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Craig, Wheeler J., ed. Accretion disks in compact stellar systems. Singapore: World Scientific, 1993.

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Book chapters on the topic "Accretion discs"

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Katz, J. I. "Accretion Discs." In Cataclysmic Variables and Low-Mass X-Ray Binaries, 359–77. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5319-2_44.

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Pringle, J. E. "Accretion Discs." In Formation and Evolution of Low Mass Stars, 153–62. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-3037-7_9.

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Pringle, James E. "Protostellar Discs." In Theory of Accretion Disks, 105–11. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-1037-9_11.

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Lasota, J. P. "Slim Accretion Discs." In Accretion Disks and Magnetic Fields in Astrophysics, 273–78. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2401-7_29.

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Lasota, J. P. "Slim Accretion Discs." In Theory of Accretion Disks — 2, 341–49. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0858-4_34.

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King, A. R., and G. A. Wynn. "Magnetic Discs." In Theory of Accretion Disks — 2, 375–87. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0858-4_38.

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Lasota, Jean-Pierre. "Black Hole Accretion Discs." In Astrophysics of Black Holes, 1–60. Berlin, Heidelberg: Springer Berlin Heidelberg, 2016. http://dx.doi.org/10.1007/978-3-662-52859-4_1.

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Kuznetsov, O. A. "Hydrodynamical Turbulence in Accretion Discs." In Astrophysical disks, 241–58. Dordrecht: Springer Netherlands, 2006. http://dx.doi.org/10.1007/1-4020-4348-1_14.

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Shaviv, Giora, and Rainer Wehrse. "Continuum Spectra of Accretion Discs." In Theory of Accretion Disks, 419–44. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-1037-9_40.

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Kumar, Sanjiv. "The Dynamics of Twisted Accretion Discs." In Theory of Accretion Disks, 297–306. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-1037-9_29.

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Conference papers on the topic "Accretion discs"

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Schild, R. "Resolving accretion discs with microlensing." In Testing the AGN paradigm diagnostics. AIP, 1992. http://dx.doi.org/10.1063/1.42180.

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Quinton, Michael, Iain McGregor, and David Benyon. "Sonification of Exosolar System Accretion Discs." In ICAD 2021: The 26th International Conference on Auditory Display. icad.org: International Community for Auditory Display, 2021. http://dx.doi.org/10.21785/icad2021.021.

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This study investigated the design and evaluation of a sonification, created for an astronomer who studies exosolar accretion discs. User design methods were applied to sonify data that could allow the classification of accretion discs. The sonification was developed over three stages: a requirements gathering exercise that inquired about the astronomer’s work and the data, design and development, as well as an evaluation. Twenty datasets were sonified and analysed. The sonification effectively represented the accretion discs allowing the astronomer to commence a preliminary, comparative classification. Multiple parameter mappings provide rich auditory stimuli. Spatial mapping and movement allow for easier identification of fast changes and peaks in the data which improved the understanding of the extent of these changes.
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Mayer, M., and J. E. Pringle. "Flickering in Black Hole Accretion discs." In THE MULTICOLORED LANDSCAPE OF COMPACT OBJECTS AND THEIR EXPLOSIVE ORIGINS. American Institute of Physics, 2007. http://dx.doi.org/10.1063/1.2774939.

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Lovelace, R. V. E., and M. M. Romanova. "Particle rings and astrophysical accretion discs." In THE PHYSICS OF PLASMA-DRIVEN ACCELERATORS AND ACCELERATOR-DRIVEN FUSION: The Proceedings of Norman Rostoker Memorial Symposium. AIP Publishing LLC, 2016. http://dx.doi.org/10.1063/1.4944026.

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Katz, J. I. "Particle acceleration in (by) accretion discs." In Particle acceleration in cosmic plasmas. AIP, 1992. http://dx.doi.org/10.1063/1.42698.

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Poutanen, Juri, and Osmi Vilhu. "Compton scattering polarization in accretion discs." In COMPTON GAMMA-RAY OBSERVATORY. AIP, 1993. http://dx.doi.org/10.1063/1.44317.

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Torkelsson, Ulf. "Magnetohydrodynamic turbulence in warped accretion discs." In RELATIVISTIC ASTROPHYSICS: 20th Texas Symposium. AIP, 2001. http://dx.doi.org/10.1063/1.1419636.

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Lipunova, G., K. Malanchev, A. Avakyan, N. Shakura, S. Tsygankov, A. Tavleev, and D. Kolesnikov. "Modeling outbursts of viscous accretion discs." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.110.

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A brief review is given on the topic of viscously-evolving accretion discs around compact objects that covers the developmentof analytical studies and our numerical model freddi allowing comparison of theory with observations.
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Mineshige, Shin, Ken Ohsuga, and Magnus Axelsson. "Modeling Super-Eddington Accretion Flow." In COOL DISCS, HOT FLOWS: The Varying Faces of Accreting Compact Objects. AIP, 2008. http://dx.doi.org/10.1063/1.3002505.

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Tavleev, A., K. Malanchev, and G. Lipunova. "Vertical structure of accretion discs in LMXB." In The multi-messenger astronomy: gamma-ray bursts, search for electromagnetic counterparts to neutrino events and gravitational waves. Sneg, 2019. http://dx.doi.org/10.26119/sao.2019.1.35553.

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Reports on the topic "Accretion discs"

1

Amin, Mustafa A., and Andrei V. Frolov. Persistent Patterns in Accretion Disks. Office of Scientific and Technical Information (OSTI), April 2006. http://dx.doi.org/10.2172/878720.

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Ortega-Rodriguez, Manuel, Appl Phys Dept /Costa Rica U. /Stanford U., Alexander S. Silbergleit, HEPL /Stanford U., Robert V. Wagoner, and Phys Dept /KIPAC, Menlo Park /Stanford U. Normal Modes of Black Hole Accretion Disks. US: Stanford Linear Accelerator Center (SLAC), November 2006. http://dx.doi.org/10.2172/894930.

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Miller, Jonah, Kelsey Lund, Matthew Mumpower, and Gail McLaughlin. Magnetic Turbulence in Post-Merger Accretion Disks. Office of Scientific and Technical Information (OSTI), May 2022. http://dx.doi.org/10.2172/1870625.

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Liedahl, D., and C. Mauche. Structure and Spectroscopy of Black Hole Accretion Disks. Office of Scientific and Technical Information (OSTI), February 2005. http://dx.doi.org/10.2172/918406.

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Matsumoto, R., and T. Tajima. Magnetic viscosity by localized shear flow instability in magnetized accretion disks. Office of Scientific and Technical Information (OSTI), January 1995. http://dx.doi.org/10.2172/10120439.

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Miller, Jonah. Fusion in Space: Nuclear Astrophysics, Neutron Star Mergers, and Accretion Disks. Office of Scientific and Technical Information (OSTI), November 2021. http://dx.doi.org/10.2172/1829623.

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You might also be interested in the extended bibliographies on the topic 'Accretion discs' for particular source types:
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