Relevant bibliographies by topics / Accretion disk

Academic literature on the topic 'Accretion disk'

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Published: 4 June 2021
Last updated: 8 June 2024

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Journal articles on the topic "Accretion disk"

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Ikhsanov, N. R., and N. G. Beskrovnaya. "Deceleration of the disk by the accreting magnetized star in the corotation approximation." Publications of the Pulkovo Observatory 228 (May 2023): 1–3. http://dx.doi.org/10.31725/0367-7966-2023-228-6.

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We analyze the process of interaction of the viscous keplerian accretion disk with the dipole magnetic field of the accretor within the corotation approximation. We estimate the radial dependence of the gaseous pressure in such non-magnetized accretion disk. We calculate the equilibrium radius at which the gaseous pressure in the disk is balanced by the pressure of the dipole magnetic field of the accreting star. We show that this radius depends on the disk viscosity and is significantly smaller than the canonical Alfvén radius realized in the process of spherical accretion.
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Thanathibodee, Thanawuth, Nuria Calvet, Jesús Hernández, Karina Maucó, and César Briceño. "A Census of the Low Accretors. I. The Catalog." Astronomical Journal 163, no. 2 (January 19, 2022): 74. http://dx.doi.org/10.3847/1538-3881/ac3ee6.

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Abstract Observations have shown that the disk frequency and the fraction of accreting pre-main-sequence stars decrease with the age of the population and that some stars appear to have disks while their accretion has stopped. Still, it is unclear how disk-bearing stars stop their accretion. To provide insight into the last stages of accretion in low-mass young stars, we conducted a survey of disk-bearing stars that are thought to be non-accretors to identify stars still accreting at very low rates. Here we present the first catalog of the survey of 170 disk-bearing non-accreting stars in Chamaeleon I, Orion OB1, Upper Scorpius, γ Velorum, and Upper Centaurus–Lupus, using He i λ10830 as a sensitive probe of accretion. We classify the line profiles into six types and argue that those showing redshifted and/or blueshifted absorption are still accreting. Using these classifications, we found that, among disk-bearing stars previously classified as non-accretors, at least 20%–30% are still accreting, with a larger fraction of those at younger population ages. While the difference between the outer disk signature and accretion status is unclear, we found a difference between the inner disk excess and accretion status. There is no preference in the mass of the newly identified accretors, suggesting that the processes inhibiting accretion do not directly depend on mass in the typical mass range of T Tauri stars. Lastly, we found that at a low accretion level, the “Hα width at the 10% height” criterion mischaracterizes a larger fraction of accretors than the line’s equivalent width.
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Bath, G. T. "Accretion Disk Evolution." International Astronomical Union Colloquium 93 (1987): 293–302. http://dx.doi.org/10.1017/s0252921100105007.

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AbstractThree aspects of mass transfer instability models of dwarf novae are examined. The hydrodynamic development of instabilities in the secondary are examined within Roche geometry and shown to extend at least a few degrees away from the line of centres. The form of the outburst light curves observed in SS Cygni are shown to be a natural consequence of mass transfer bursts with a duration either less than, or greater than, the disk viscous timescale. Finally the two-dimensional structure of the disc in the plane of the orbit is studied. As with α-disks the viscous evolution time following a burst of mass transfer determines the size of viscosity within the disk. Significant deviations from axial symmetry are found to be present.
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Kuperus, Max. "Accretion Disk Coronae." Highlights of Astronomy 8 (1989): 535–38. http://dx.doi.org/10.1017/s1539299600008248.

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SummaryAccretion disk coronae around compact objects are the result of strong magnetic activity in the inner regions of accretion disks. Part of the accreting energy is dissipated in te corona and can be observed as hard X-ray emission with a time variability caused by the coronal structures. The interaction of disk coronae with neutron stars and black holes may cause quaslperiodlc oscillations respectively flare type emission.
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Daemgen, Sebastian, Monika G. Petr-Gotzens, and Serge Correia. "T Tauri Binaries in Orion: Evidence for Accelerated and Synchronized Disk Evolution." Proceedings of the International Astronomical Union 7, S282 (July 2011): 452–53. http://dx.doi.org/10.1017/s1743921311028043.

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AbstractIn order to trace the role of binarity for disk evolution and hence planet formation, we started the currently largest spatially resolved near-infrared photometric and spectroscopic study of the inner dust and accretion disks of the individual components of 27 visual, 100–400 AU binaries in the Orion Nebula Cluster (ONC). We study the frequency of Brackett-γ (2.165μm) emitters to assess the frequency of accretion disk-bearing stars among the binaries of the ONC: only 34±9% of the binary components show signs of accretion and, hence, the presence of gaseous inner disks—less than the fraction of gas accretion disks among single stars of the ONC of ~50%. Additionally, we find a significant difference between binaries above and below 200 AU separation: no close systems with only one accreting component are found. The results suggest shortened disk lifetimes as well as synchronized disk evolution.
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Gárate, Matías, Timmy N. Delage, Jochen Stadler, Paola Pinilla, Til Birnstiel, Sebastian Markus Stammler, Giovanni Picogna, Barbara Ercolano, Raphael Franz, and Christian Lenz. "Large gaps and high accretion rates in photoevaporative transition disks with a dead zone." Astronomy & Astrophysics 655 (November 2021): A18. http://dx.doi.org/10.1051/0004-6361/202141444.

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Context. Observations of young stars hosting transition disks show that several of them have high accretion rates, despite their disks presenting extended cavities in their dust component. This represents a challenge for theoretical models, which struggle to reproduce both features simultaneously. Aims. We aim to explore if a disk evolution model, including a dead zone and disk dispersal by X-ray photoevaporation, can explain the high accretion rates and large gaps (or cavities) measured in transition disks. Methods. We implemented a dead zone turbulence profile and a photoevaporative mass-loss profile into numerical simulations of gas and dust. We performed a population synthesis study of the gas component and obtained synthetic images and SEDs of the dust component through radiative transfer calculations. Results. This model results in long-lived inner disks and fast dispersing outer disks that can reproduce both the accretion rates and gap sizes observed in transition disks. For a dead zone of turbulence αdz = 10−4 and an extent rdz = 10 AU, our population synthesis study shows that 63% of our transition disks are still accreting with Ṁg ≥ 10−11 M⊙ yr−1 after opening a gap. Among those accreting transition disks, half display accretion rates higher than 5.0 × 10−10 M⊙ yr−1. The dust component in these disks is distributed in two regions: in a compact inner disk inside the dead zone, and in a ring at the outer edge of the photoevaporative gap, which can be located between 20 and 100 AU. Our radiative transfer calculations show that the disk displays an inner disk and an outer ring in the millimeter continuum, a feature that resembles some of the observed transition disks. Conclusions. A disk model considering X-ray photoevaporative dispersal in combination with dead zones can explain several of the observed properties in transition disks, including the high accretion rates, the large gaps, and a long-lived inner disk at millimeter emission.
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Haerken 哈斯铁, Hasitieer 尔·哈尔肯, Guang-Wei 广伟 Li 李, Min 敏. Li 李, Fuqing 福庆 Duan 段, and Yongheng 永恒 Zhao 赵. "Discovery of Two Different Full Disk Evolutionary Patterns of M-type T Tauri Stars with LAMOST DR8." Astrophysical Journal 960, no. 1 (December 22, 2023): 58. http://dx.doi.org/10.3847/1538-4357/ad04d3.

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Abstract The full disk, full of gas and dust, determines the upper limit of planet masses, and its lifetime is critical for planet formation, especially for giant planets. In this work, we studied the evolutionary timescales of the full disks of T Tauri stars (TTSs) and their relations to accretion. Combined with Gaia EDR3, Two Micron All Sky Survey, and Wide-field Infrared Survey Explorer data, 1077 disk-bearing TTS candidates were found in LAMOST DR8, and stellar parameters were obtained. Among them, 783 are newly classified by spectra as classical T Tauri stars (CTTSs; 169) or weak-lined T Tauri stars (WTTSs). Based on EW and FWHM of Hα, 157 TTSs in accretion were identified, with ∼82% also having full disks. For TTSs with M < 0.35M ☉, about 80% seem to already lose their full disks at ∼0.1 Myr, which may explain their lower mass, while the remaining 20% with full disks evolve at similar rates of non-full disks within 5 Myr, allowing enough time and material to form giant planets. The fraction of accreting TTSs to disk-bearing TTSs is stable at ∼10% and can last ∼5–10 Myr, suggesting that full disks and accretion evolve with similar rates as non-full disks. For TTSs with M > 0.35 M ☉, almost all full disks can survive more than 0.1 Myr, most for 1 Myr and some even for 20 Myr. For TTSs with M > 0.35 M ☉, almost all full disks can survive more than 0.1 Myr, most for 1 Myr, and some even for 20 Myr, which implies planets are more likely to be formed in their disks than those of M < 0.35 M ☉, and thus M dwarfs with M > 0.35 M ☉ can have more planets. The fraction of full-disk TTSs to disk-bearing TTSs decreases with age following the relation f ∝ t −0.35, and similar relations existed in the fraction of accreting TTSs and the fraction of full-disk CTTSs, suggesting faster full disks and accretion evolution than non-full disks. For full-disk stars, the ratio of accretion of lower-mass stars is systematically lower than that of higher-mass stars, confirming the dependence of accretion on stellar mass, which may be reflective of an observational bias in the detection of accretion levels, with the lower-mass stars crossing below the detection threshold earlier than higher-mass stars.
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Venuti, Laura, Ann Marie Cody, Giacomo Beccari, Luisa M. Rebull, Michael J. Irwin, Apoorva Thanvantri, Sowmya Thanvantri, et al. "Circumstellar Disk Accretion Across the Lagoon Nebula: The Influence of Environment and Stellar Mass." Astronomical Journal 167, no. 3 (February 20, 2024): 120. http://dx.doi.org/10.3847/1538-3881/ad1f65.

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Abstract Pre-main-sequence disk accretion is pivotal for determining the final stellar properties and the early conditions for close-in planets. We aim to establish the impact of internal (stellar mass) and external (radiation field) parameters on the disk evolution in the Lagoon Nebula massive star-forming region. We employ simultaneous u, g, r, i, Hα time-series photometry, archival infrared data, and high-precision K2 light curves to derive the stellar, disk, and accretion properties for 1012 Lagoon Nebula members. We estimate that of all young stars in the Lagoon Nebula, 34%–37% have inner disks traceable down to ∼12 μm, while 38%–41% are actively accreting. We detect disks ∼1.5 times more frequently around G, K, and M stars than around higher-mass stars, which appear to deplete their inner disks on shorter timescales. We find tentative evidence for a faster disk evolution in the central regions of the Lagoon Nebula, where the bulk of the O/B population is located. Conversely, disks appear to last longer at the nebula outskirts, where the measured fraction of disk-bearing stars tends to exceed that of accreting and disk-free stars. The derived mass accretion rates show a nonuniform dependence on stellar mass between ∼0.2 and 5 M ⊙. In addition, the typical accretion rates appear to differ across the Lagoon Nebula extension, with values twice lower in the core region than at its periphery. Finally, we detect tentative radial density gradients in the surface accretion shocks, leading to lags in the appearance of light curve brightness features as a function of wavelength that can amount to ∼7%–30% of the rotation period.
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Zhou, Shuying, Mouyuan Sun, Tong Liu, Jian-Min Wang, Jun-Xian Wang, and Yongquan Xue. "Stellar Black Holes Can “Stretch” Supermassive Black Hole Accretion Disks." Astrophysical Journal Letters 966, no. 1 (April 24, 2024): L9. http://dx.doi.org/10.3847/2041-8213/ad3c3f.

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Abstract Stellar black holes (sBHs) are widely believed to exist in the accretion disks of active galactic nuclei (AGNs). Previous studies often focus on the transient emission produced by embedded sBHs. Here, we explore the possible observational consequences of an AGN accretion disk that contains a population of accreting sBHs. Embedded accreting sBHs change the effective temperature distribution of the AGN accretion disk by heating gas in the outer regions. Two possible observational consequences are presented. First, the spectral energy distribution has a turnover feature at ∼4700 Å when the supermassive black hole mass is ∼108 M ⊙, which can help explain the observed shallow spectral shape at wavelengths >5000 Å for the Sloan Digital Sky Survey quasar composite spectrum. Second, the half-light radius of a given relatively long wavelength is significantly larger than for an AGN disk without sBHs, which can be tested by microlensing observations. With appropriate sBH distributions, the model can be reconciled with quasar microlensing disk sizes. We propose that the half-light radius–wavelength relation can be utilized to investigate the distributions of embedded sBHs in AGN accretion disks.
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Liu, Xiang, Ning Chang, Xin Wang, and Qi Yuan. "The Origin of Radio Emission in Black Hole X-ray Binaries." Galaxies 9, no. 4 (October 17, 2021): 78. http://dx.doi.org/10.3390/galaxies9040078.

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We studied the relation of accretion-jet power and disk luminosity, especially the jet efficiencies and disk radiative efficiencies for different accretion disks as well as black hole (BH) spin, in order to explore the origin of radio emission in black hole X-ray binaries (BHXBs). We found that jet efficiency increases more rapidly (efficient) than the nearly constant disk radiative efficiency for thin disk component in high accretion regime, which could account for the steep track (μ>1) in the observed radio and X-ray luminosity relations (LR∝LXμ), but the thin disk component may not be able to explain the standard track (μ≈0.6) in the BHXBs. For hot accretion flows (HAF), the resulting jet efficiency changes along with the large range of accretions from quiescent state to nearly Eddington state, which could account for the standard track in the BHXBs. The BH spin-jet is discussed for the magnetic arrested disk (MAD) state; in this state, the spin-jet power might contribute to a linear correlation between jet power and mass accretion rate for a given source. More accurate observations are required to test the results.
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Dissertations / Theses on the topic "Accretion disk"

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Popham, Robert George. "Accretion disk boundary layers." Diss., The University of Arizona, 1993. http://hdl.handle.net/10150/186435.

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We examine the nature of the boundary layer in α-viscous accretion disks. The boundary layer is the interface between the disk and the accreting central star or black hole. We develop two models for the boundary layer by expanding and generalizing the standard disk equations, and then solving our new set of equations numerically using a relaxation method. First, we use a model which includes a polytropic equation of state to examine the disk dynamics. This allows us to ignore the energetics and radiative transfer and simplifies the problem considerably. We find two types of boundary layer solutions with this model, depending on the rotation rate of the accreting star. One of these is a new type of solutions in which the angular momentum accretion rate can be small or negative. These solutions allow accretion to continue even after the star spins up to breakup speed. We apply a causally-limited viscosity prescription to our solutions, and find that it prevents the radial velocities from becoming supersonic in the boundary layer, thus preserving causality. We apply the same prescription to a model for disks around black holes, and find that it allows us to calculate solutions for reasonable values of α, where none existed before. We develop a more complete model, which includes the energetics and radiative transfer of the boundary layer, for comparison with observations. We apply this model to cataclysmic variables, and find that the nature of the boundary layer in these systems depends strongly on the optical depth, which in turn depends largely on the mass accretion rate and the rotation rate of the accreting star. The dependence of our results on the accretion rate agrees well with X-ray observations of these systems. We also apply the model to accretion disks in pre-main sequence stars, such as T Tauri and FU Orionis stars, and find that the temperatures and radial widths of the boundary layer in our solutions agree well with those inferred from observations.
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Higginbottom, Nicholas. "Modelling accretion disk winds in quasars." Thesis, University of Southampton, 2014. https://eprints.soton.ac.uk/368584/.

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Outflows are ubiquitous in active galactic nuclei (AGN). They can take the form of either dramatic radio jets, which extend vast distances into the inter-galactic medium, or of much smaller scale winds - whose existence can be inferred only indirectly via their influence on the observed spectra. There is good evidence to show that winds are likely to arise from the accretion disks thought to form the central engine of all AGN; they should therefore be observable in all such systems. The clearest observational signature comes in the form of the broad, blue-shifted absorption features seen in the spectra of broad absorption line quasars (BALQSOs) and the aim of this work is to investigate how the geometry and physical parameters of disk winds affect their absorption spectra. We first discuss the changes made to an existing Monte Carlo radiative transfer code, python, in order to extend its capabilities to include modelling of AGN. These changes include the implementation of an approximate ionization scheme which takes account of arbitrary illuminating spectral energy distributions (SEDs), and the inclusion of heating and cooling effects likely to be important in the presence of high energy photons. Next, we describe the second stage of the project which was to gain insight into the general properties of a wind exhibiting broad absorption line (BAL) features. We did this by performing radiative transfer and ionization calculations on a simple kinematic wind representation using python. We show that BAL features can be produced for plausible AGN parameters. Finally, we present calculations carried out on a more complex wind geometry, generated from a hydrodynamic simulation of a line driven disk wind. This calculation does not produce BAL features at all, and in fact the wind is too highly ionised to permit efficient line driving. This result is significant because it illustrates the importance of detailed radiative transfer in hydrodynamic modelling, and suggests future work.
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Watarai, Kenya. "Super-Critical Accretion Disk around a Black Hole." 京都大学 (Kyoto University), 2003. http://hdl.handle.net/2433/149067.

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Kubsch, Marcus, Tobias F. Illenseer, and Wolfgang J. Duschl. "Accretion disk dynamics alpha-viscosity in self-similar self-gravitating models." EDP SCIENCES S A, 2016. http://hdl.handle.net/10150/614710.

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Aims. We investigate the suitability of alpha-viscosity in self-similar models for self-gravitating disks with a focus on active galactic nuclei (AGN) disks. Methods. We use a self-similar approach to simplify the partial di ff erential equations arising from the evolution equation, which are then solved using numerical standard procedures. Results. We find a self-similar solution for the dynamical evolution of self-gravitating alpha-disks and derive the significant quantities. In the Keplerian part of the disk our model is consistent with standard stationary alpha-disk theory, and self-consistent throughout the self-gravitating regime. Positive accretion rates throughout the disk demand a high degree of self-gravitation. Combined with the temporal decline of the accretion rate and its low amount, the model prohibits the growth of large central masses. Conclusions. alpha-viscosity cannot account for the evolution of the whole mass spectrum of super-massive black holes (SMBH) in AGN. However, considering the involved scales it seems suitable for modelling protoplanetary disks.
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Caunt, Stuart Edward. "Analytical and numerical models of accretion disks." Thesis, University of Newcastle Upon Tyne, 1998. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.265485.

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劉長軍 and Cheung-kwan Andy Lau. "High energy processes around the accretion disk of AGN." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 1995. http://hub.hku.hk/bib/B31213236.

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Hamper, Randall T. "Accretion disk radii changes in IP Peg during outburst." Virtual Press, 2007. http://liblink.bsu.edu/uhtbin/catkey/1371843.

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The focus of this study is the change in accretion disk size in Dwarf Novae (DN), IP Peg. DN systems are a type of cataclysmic variable that experience periodic outbursts. These outbursts are caused by the release of gravitational potential energy from an increased rate of matter flow through the accretion disk. Throughout outburst, the radius of the accretion disk of the DN changes. Recent research done at Ball State University has suggested that the disk radius may not change as the disk instability model predicts. According to the disk instability model, the accretion disk should be at its largest radial size when the DN is at the peak of outburst. IP Peg in September and October of 2006 underwent outburst. It was found that during that particular outburst that the accretion disk was at its largest radial size on the decline from outburst and not peak. Further research into how the accretion disk changes with time is needed.
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Lau, Cheung-kwan Andy. "High energy processes around the accretion disk of AGN /." Hong Kong : University of Hong Kong, 1995. http://sunzi.lib.hku.hk/hkuto/record.jsp?B17664925.

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Yamazaki, Tatsuya. "Two Topics on Accretion Disk Variabilities Related to Thermal Instability." 京都大学 (Kyoto University), 1997. http://hdl.handle.net/2433/202439.

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Shah, Jay. "Understanding the origin of meteoritic magnetism : implications for protoplanetary disk accretion." Thesis, Imperial College London, 2017. http://hdl.handle.net/10044/1/56625.

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Chondritic meteorites largely formed 4.6 billion years ago, and can range from being metamorphosed as a result of processing on their asteroid parent bodies to entirely unaltered since their formation in the protoplanetary disk. The magnetic grains within these meteorites can potentially record and retain the magnetic conditions on the parent body and the conditions in the protoplanetary disk during the formation of our planetary system. However, the complex history of these meteorites can make their magnetic records difficult to interpret, and their age prompts the question of whether a magnetic remanence can be retained for so long. In this thesis, to help identify the origin of the magnetic remanence, a new method for the palaeomagnetic conglomerate test that uses micro-CT scans to accurately mutually orient chondrules from chondrites was developed. When applied to Vigarano (CV3) and Bjurböle (L/LL4), a more in-depth understanding of parent body processing was achieved that provides evidence for magnetic dynamo activity on their parent bodies. To understand the magnetic record of CK chondrites, a palaeomagnetic analysis of Karoonda (CK4) was conducted, and found no evidence of a significant magnetic field recording, supporting the solar radiative heating model for the CV-CK chondrites. To determine whether magnetic remanence can be retained from the early Solar System, the high thermal stability of single and multi-vortex kamacite grains from Bishunpur (LL3.1) was demonstrated by performing in-situ temperature-dependent nanometric magnetic measurements using electron holography and numerical micromagnetic energy barrier calculations. This study found that the majority of kamacite grains in dusty olivines are capable of retaining magnetic field information from the early Solar System, a key finding in our quest to understand the formation of our Solar System.
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Books on the topic "Accretion disk"

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Isaac, Shlosman, and United States. National Aeronautics and Space Administration., eds. UV line diagnostics of accretion disk winds in cataclysmic variables. [Washington, DC?: National Aeronautics and Space Administration, 1992.

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Jörn, Wilms, Begelman Mitchell C, and United States. National Aeronautics and Space Administration., eds. Self-consistent thermal accretion disk corona models for compact objects. [Washington, DC: National Aeronautics and Space Administration, 1997.

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B, Dove James, and United States. National Aeronautics and Space Administration., eds. Self-consistent thermal accretion disk corona models for compact objects. [Washington, DC: National Aeronautics and Space Administration, 1997.

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Jörn, Wilms, Begelman Mitchell C, and United States. National Aeronautics and Space Administration., eds. Self-consistent thermal accretion disk corona models for compact objects. [Washington, DC: National Aeronautics and Space Administration, 1997.

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B, Dove James, and United States. National Aeronautics and Space Administration., eds. Self-consistent thermal accretion disk corona models for compact objects. [Washington, DC: National Aeronautics and Space Administration, 1997.

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B, Dove James, and United States. National Aeronautics and Space Administration., eds. Self-consistent thermal accretion disk corona models for compact objects. [Washington, DC: National Aeronautics and Space Administration, 1997.

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Jörn, Wilms, Begelman Mitchell C, and United States. National Aeronautics and Space Administration., eds. Self-consistent thermal accretion disk corona models for compact objects. [Washington, DC: National Aeronautics and Space Administration, 1997.

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Stern, Alan. Collisional time scales in the Kuiper disk and their implications. [Washington, DC: National Aeronautics and Space Administration, 1995.

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United States. National Aeronautics and Space Administration., ed. Collisional time scales in the Kuiper disk and their implications. [Washington, DC: National Aeronautics and Space Administration, 1995.

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E, Kuulkers, and United States. National Aeronautics and Space Administration., eds. Absorption dips in GRO J1655-40: Mapping the inner accretion disk. Oxford, England: University of Oxford, Oxford Astrophysics, 1997.

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Book chapters on the topic "Accretion disk"

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Mineshige, S. "Accretion Disk Instabilities." In Nonlinear Phenomena in Stellar Variability, 83–103. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-1062-4_8.

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Kuperus, M. "Accretion Disk Electrodynamics." In Gravitation in Astrophysics, 195–208. Boston, MA: Springer US, 1987. http://dx.doi.org/10.1007/978-1-4613-1897-2_5.

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Kuperus, Max. "Accretion Disk Coronae." In Highlights of Astronomy, 535–38. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0977-9_78.

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Coroniti, F. V. "Accretion Disk Electrodynamics." In Unstable Current Systems and Plasma Instabilities in Astrophysics, 453–69. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-6520-1_49.

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Sturrock, P. A., and W. Yang. "Accretion Disk Flares." In Quasars, 411–12. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4716-0_95.

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Bath, G. T. "Accretion Disk Evolution." In Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments, 293–302. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3801-4_44.

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Narayan, R., and R. Popham. "Accretion Disk Boundary Layers." In Theory of Accretion Disks — 2, 293–307. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0858-4_30.

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Cherepashchuk, A. M. "Supercritical Accretion Disk in SS433." In Astrophysical disks, 121–30. Dordrecht: Springer Netherlands, 2006. http://dx.doi.org/10.1007/1-4020-4348-1_6.

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Vishniac, Ethan T. "Galactic and Accretion Disk Dynamos." In Magnetic Helicity in Space and Laboratory Plasmas, 285–92. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm111p0285.

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Meyer, Friedrich, and Emmi Meyer-Hofmeister. "A Free Accretion Disk in SN 1987A?" In Theory of Accretion Disks, 307–11. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-1037-9_30.

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Conference papers on the topic "Accretion disk"

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Stein, Wayne A. "Accretion disk coronas in QSOs." In Testing the AGN paradigm diagnostics. AIP, 1992. http://dx.doi.org/10.1063/1.42194.

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Hanawa, Tomoyuki, Tomonori Usuda, Motohide Tamura, and Miki Ishii. "Gas Accretion from a Circumbinary Disk to Protoplanetary Disks." In EXOPLANETS AND DISKS: THEIR FORMATION AND DIVERSITY: Proceedings of the International Conference. AIP, 2009. http://dx.doi.org/10.1063/1.3215806.

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Belmont, R. "Magnetic Pumping in accretion disk coronae." In INTERACTING BINARIES: Accretion, Evolution, and Outcomes. AIP, 2005. http://dx.doi.org/10.1063/1.2130280.

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Inoue, Yoshiyuki. "Disk-Jet Connection in Active Super-massive Black Holes in the Standard Accretion Disk Regime." In Accretion Processes in Cosmic Sources – II. Trieste, Italy: Sissa Medialab, 2019. http://dx.doi.org/10.22323/1.342.0040.

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Hawley, John. "Magnetohydrodynamic turbulence in an accretion disk." In 25th Plasmadynamics and Lasers Conference. Reston, Virigina: American Institute of Aeronautics and Astronautics, 1994. http://dx.doi.org/10.2514/6.1994-2406.

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Huré, Jean-Marc, and Suzy Collin. "The accretion disk in NGC 4258." In Accretion processes in astrophysical systems: Some like it hot! - eigth astrophysics conference. AIP, 1998. http://dx.doi.org/10.1063/1.55908.

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Tammi, Joni. "Thermal flares from collapsed accretion disk?" In 8th INTEGRAL Workshop “The Restless Gamma-ray Universe”. Trieste, Italy: Sissa Medialab, 2011. http://dx.doi.org/10.22323/1.115.0143.

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Janiuk, Agnieszka. "GLADIS: GLobal Accretion Disk Instability Simulation." In Multifrequency Behaviour of High Energy Cosmic Sources - XIII. Trieste, Italy: Sissa Medialab, 2020. http://dx.doi.org/10.22323/1.362.0048.

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Chiappini, Cristina. "Galactic disk abundance ratios: constraining SNIa stellar yields." In INTERACTING BINARIES: Accretion, Evolution, and Outcomes. AIP, 2005. http://dx.doi.org/10.1063/1.2130270.

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De Gouveia Dal Pino, Elisabete, Maria Victoria del Valle, Luis H. S. Kadowaki, Behoruz Khiali, Grzergorz Kowal, Yosuke Mizuno, and Chandra B. Singh. "Magnetic Reconnection on Jet-Accretion Disk Systems." In Frontier Research in Astrophysics – II. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.269.0056.

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Reports on the topic "Accretion disk"

1

Kondratko, P. The Sub-parsec, Geometrically Thick, Self-Gravitating Accretion Disk in the Nucleus of NGC 3079. Office of Scientific and Technical Information (OSTI), June 2004. http://dx.doi.org/10.2172/827016.

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Mizuno, T. Accretion Disk Spectra of the Ultra-Luminous X-Ray Sources in Nearby Spiral Galaxies and Galactic Superluminal Jet Sources. Office of Scientific and Technical Information (OSTI), December 2003. http://dx.doi.org/10.2172/826596.

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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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Elicker, Lauren, and Gregory Salvesen. X-ray Spectral-Timing Pipeline to Investigate an Electron-Scattering Time Delay in Black Hole Accretion Disks. Office of Scientific and Technical Information (OSTI), April 2024. http://dx.doi.org/10.2172/2342024.

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