Relevant bibliographies by topics / Disks

Contents

  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers
  6. Reports

Academic literature on the topic 'Disks'

Author: Grafiati
Published: 4 June 2021
Last updated: 6 September 2023

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Journal articles on the topic "Disks"

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ZHONG, HONGJIE, and CUNBIAO LEE. "PATHS OF FREELY FALLING DISKS." Modern Physics Letters B 23, no. 03 (January 30, 2009): 373–76. http://dx.doi.org/10.1142/s0217984909018436.

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The free falling motion of round thin disks in quiescent water was investigated experimentally. The mean density of the disks were about 1.05 g/cm3, slightly larger than water, and thickness to diameter ratio is 0.1. In this letter, We reported two cases with different mass distributions, in one case the disk's center of mass coincided with the geometry center and in another case it was deviated. Two CCD cameras were used to photograph the falling disk simultaneously, the disk's six degrees of freedom were obtained via a stereoscopic vision method. In the first case fluttering motion was observed, the disk's oscillatory motion confined in a vertical plane, and the pitching motion occurred about an axis normal to the plane. In the second case, steady helical falling was observed, the disk moved in a helical path at constant speed, the attacking angle is constant.
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Montgomery, M. M. "Modeling Fluid Flow Effects in Close Binary and Protoplanetary Systems." Proceedings of the International Astronomical Union 7, S282 (July 2011): 549–50. http://dx.doi.org/10.1017/s1743921311028365.

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AbstractAccretion disks around some white dwarfs in Cataclysmic Variables are thought to tilt around the line of nodes by the lift force acting at the disk's center of pressure. We investigate whether protoplanetary disks can also experience disk tilt. We find that lift may be possible by an asymmetric, net uni-directional, in-falling gas/dust stream overflowing a bluff body (e.g., Class I sources) or inner annuli of young Class II sources if gas/dust is still in-falling and the aspect ratio and disk surface area are large enough. However, inner disks of Class II sources LkCa 15, UX Tau A, and Rox 44 are not large enough, and therefore disk tilt is not likely.
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Yakhin, Sergey, Il'fat Aliakberov, and Adel Vakhitov. "SUBSTANTIATION OF PARAMETERS OF A ROTARY IMPLEMENT FOR SURFACE TREATMENT OF SOIL WITH INCLINED HEXAGONAL DISC." Vestnik of Kazan State Agrarian University 17, no. 4 (January 27, 2023): 106–11. http://dx.doi.org/10.12737/2073-0462-2023-106-111.

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For surface tillage, rotary implements with disk working bodies are widely used. In recent decades, intensive research has been carried out on the development of rotary tools with polygonal disks. They were implemented in practice in the form of hexagonal disks mounted on a shaft at an angle of 90° and performing the usual rotational movement around its axis. Of interest are polygonal discs, which are fixed obliquely on the shaft. The well-known tillage tool with inclined square discs was not implemented in practice, since it turned out to be technologically unstable and did not provide a uniform depth of tillage. In the developed soil-cultivating tool, these shortcomings are eliminated. As a result of the study, analytical dependences were obtained, which made it possible to substantiate the parameters of a tillage tool containing obliquely fixed hexagonal disks: the width of the tool (module) capture B = 1.8 m; number of rotary batteries - 2; disk diameter D = 0.32…0.48 m; angle of fastening of discs on the shaft  > 50°…55°; distance between disc centers S = 0.100…0.105 m; the number of disks in the battery n = 17; the angle of rotation (displacement) of the disks one relative to the other around the axis of the shaft ɛ = 11.25°. A formula was also obtained to reveal the regularity of the change in the angle of entry of the disk into the soil. The calculation showed that this angle during the rotation of the disk is a variable parameter and varies within 72.5° ... 107.5°. This contributes to the self-cleaning of the inter-disk space from adhering soil and plant residues and is used in determining the traction resistance of the implement.
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Angelo, Isabel, Gaspard Duchene, Karl Stapelfeldt, Zoie Telkamp, François Ménard, Deborah Padgett, Gerrit Van der Plas, et al. "Demographics of Protoplanetary Disks: A Simulated Population of Edge-on Systems." Astrophysical Journal 945, no. 2 (March 1, 2023): 130. http://dx.doi.org/10.3847/1538-4357/acbb01.

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Abstract The structure of protoplanetary disks plays an essential role in planet formation. A disk that is highly inclined, or “edge-on,” is of particular interest since its geometry provides a unique opportunity to study the disk’s vertical structure and radial extent. Candidate edge-on protoplanetary disks are typically identified via their unique spectral energy distributions (SEDs) and subsequently confirmed through high-resolution imaging. However, this selection process is likely biased toward the largest, most-massive disks, and the resulting sample may not accurately represent the underlying disk population. To investigate this, we generated a grid of protoplanetary disk models using radiative transfer simulations and determined which sets of disk parameters produce edge-on systems that could be recovered by the aforementioned detection techniques—i.e., identified by their SEDs and confirmed through follow-up imaging with the Hubble Space Telescope. In doing so, we adopt a quantitative working definition of “edge-on disks” (EODs) that is observation driven and agnostic about the disk inclination or other properties. Folding in empirical disk demographics, we predict an occurrence rate of 6.2% for EODs and quantify biases toward highly inclined, massive disks. We also find that EODs are underrepresented in samples of Spitzer-studied young stellar objects, particularly for disks with host masses of M ≲ 0.5 M ⊙. Overall, our analysis suggests that several dozen EODs remain undiscovered in nearby star-forming regions, and provides a universal selection process to identify EODs for consistent, population-level demographic studies.
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Khaibrakhmanov, Sergey A., Alexander E. Dudorov, and Andrey M. Sobolev. "Rising magnetic flux tubes as a source of IR-variability of the accretion disks of young stars." Proceedings of the International Astronomical Union 14, S345 (August 2018): 295–96. http://dx.doi.org/10.1017/s1743921319001431.

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AbstractWe investigate dynamics of slender magnetic flux tubes (MFT) in the accretion disks of young stars. Simulations show that MFT rise from the disk and can accelerate to 20-30 km/s causing periodic outflows. Magnetic field of the disk counteracts the buoyancy, and the MFT oscillate near the disk’s surface with periods of 10-100 days. We demonstrate that rising and oscillating MFT can cause the IR-variability of the accretion disks of young stars.
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Hincapié Mejía, Gina María, Juan Miguel Marín S., Luis Alberto Rios, and Gloria Restrepo. "Evaluating E. coli degradation using a rotatory disk photoreactor." Ingeniería e Investigación 27, no. 3 (September 1, 2007): 65–69. http://dx.doi.org/10.15446/ing.investig.v27n3.14846.

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Degradation of the bacterium E. coli was studied using a rotatory disk photoreactor manufactured in stainless steel to ascertain this photoreaction system’s behavior in different operating conditions. The photoreactor was equipped with 6 black light bulbs (BLB) used as a source of UV light and fitted with 7 removable disks made of common frosted glass impregnated with TiO2 photocatalyzer which were coupled to a rotation system. TiO2 was impregnated on the disks using the sol-gel method varying molar precursor gel ratios. Abrasion resistance, disk adhesion and surface uniformity tests were carried out for selecting the film presenting the best characteristics. Bacterial photodegradation studies were carried out using the following variable parameters: the disks’ rotation speed, radiation intensity and the number of discs which were directly related to the concentration of photocatalyzer in the system. Up to 64.3% degradation was achieved in 4 hours using 7 disks, low intensity and low rotation speed.
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Kormendy, John. "Internal secular evolution in disk galaxies: the growth of pseudobulges." Proceedings of the International Astronomical Union 3, S245 (July 2007): 107–12. http://dx.doi.org/10.1017/s1743921308017407.

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AbstractObservational and theoretical evidence that internal, slow (“secular”) evolution reshapes galaxy disks is reviewed in Kormendy & Kennicutt (2004). This update has three aims. First, I emphasize that this evolution is very general – it is as fundamental to the evolution of galaxy disks as (e. g.) core collapse is to globular clusters, as the production of hot Jupiters is to the evolution of protoplanetary disks, and as evolution to red giants containing proto-white-dwarfs is to stellar evolution. One consequence for disk galaxies is the buildup of dense central components that get mistaken for classical (i. e., merger-built) bulges but that were grown out of disk stars and gas. We call these pseudobulges. Second, I review new results on pseudobulge star formation and structure and on the distinction between boxy and disky pseudobulges. Finally, I highlight how these results make a galaxy formation problem more acute. How can hierarchical clustering produce so many pure disk galaxies with no evidence for merger-built bulges?
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Ryzhkov, A. V., A. V. Machkarin, and K. V. Kazakov. "Comparative analysis of soil discarding by spherical disks." IOP Conference Series: Earth and Environmental Science 845, no. 1 (November 1, 2021): 012138. http://dx.doi.org/10.1088/1755-1315/845/1/012138.

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Abstract The article presents data on the influence of various types of spherical disks on the discarding of soil in the horizontal and vertical planes during its processing. These studies were conducted in order to optimize the selection of working bodies of disk tillage machines in terms of resistance and processing quality. Three types of disks were used in the comparative analysis. Two types of discs with cutouts and one solid spherical disc. On one type of disk, the cutouts are made in the form of circular arcs, and on the other-in the form of arcs of a logarithmic spiral. The conducted studies have shown that within the working surface of the disk, the trajectories of movement of soil particles under the influence of the three types of disks under study differ little from each other. Although it can be noted that the steeper rise of the trajectory in the vertical plane provides a solid disk, and the smallest rise of the trajectory - at the disk with cutouts in the form of a logarithmic spiral. In the horizontal plane, the longitudinal movement of the soil mass is less in disks with cutouts, especially in a disk with cutouts along the arc of a logarithmic spiral. As a result of these studies, it was revealed that the disk working bodies with cutouts on the cutting edge in the form of arcs of a logarithmic spiral showed the best quality and energy indicators.
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Kamali, F., C. Henkel, S. Koyama, C. Y. Kuo, J. J. Condon, A. Brunthaler, M. J. Reid, et al. "Accretion disk versus jet orientation in H2O megamaser galaxies." Astronomy & Astrophysics 624 (April 2019): A42. http://dx.doi.org/10.1051/0004-6361/201834600.

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Context. An essential part of the paradigm describing active galactic nuclei is the alignment between the radio jet and the associated rotation axis of the sub-pc accretion disks. Because of the small linear and angular scales involved, this alignment has not yet been checked in a sufficient number of low luminosity active galactic nuclei (LLAGNs). Aims. The project examines the validity of this paradigm by measuring the radio continuum on the same physical scale as the accretion disks to investigate any possible connection between these disks and the radio continuum. Methods. We observed a sample of 18 LLAGNs in the 4.8 GHz (6 cm) radio continuum using the Very Long Baseline Array (VLBA) with 3.3–6.5 ms resolution. The sources were selected to show both an edge-on accretion disk revealed by 22 GHz H2O megamaser emission and signatures of a radio jet. Furthermore, the sources were previously detected in 33 GHz radio continuum observations made with the Very Large Array. Results. Five out of 18 galaxies observed were detected at 8σ or higher levels (Mrk 0001, Mrk 1210, Mrk 1419, NGC 2273, and UGC 3193). While these five sources are known to have maser disks, four of them exhibit a maser disk with known orientation. For all four of these sources, the radio continuum is misaligned relative to the rotation axis of the maser disk, but with a 99.1% confidence level, the orientations are not random and are confined to a cone within 32° of the maser disk’s normal. Among the four sources the misalignment of the radio continuum with respect to the normal vector to the maser disk is smaller when the inner radius of the maser disk is larger. Furthermore, a correlation is observed between the 5 GHz VLBA radio continuum and the [OIII] luminosity and also with the H2O maser disk’s inner radius.
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Kondo, Katsushi, Satoshi Okuzumi, and Shoji Mori. "The Roles of Dust Growth in the Temperature Evolution and Snow Line Migration in Magnetically Accreting Protoplanetary Disks." Astrophysical Journal 949, no. 2 (June 1, 2023): 119. http://dx.doi.org/10.3847/1538-4357/acc840.

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Abstract The temperature structure of protoplanetary disks provides an important constraint on where in the disks rocky planets like our own form. Recent nonideal magnetohydrodynamical (MHD) simulations have shown that the internal Joule heating associated with magnetically driven disk accretion is inefficient at heating the disk midplane. A disk temperature model based on the MHD simulations predicts that in a disk around a solar-mass young star, the water snow line can move inside the current Earth’s orbit within 1 Myr after disk formation. However, the efficiency of the internal Joule heating depends on the disk’s ionization and opacity structures, both of which are governed by dust grains. In this study, we investigate these effects by combining the previous temperature model for magnetically accreting disks with a parameterized model for the grain size and vertical distribution. Grain growth enhances the gas ionization fraction and thereby allows Joule heating to occur closer to the midplane. However, growth beyond 10 μm causes a decrease in the disk opacity, leading to a lower midplane temperature. The combination of these two effects results in the midplane temperature being maximized when the grain size is in the range 10–100 μm. Grain growth to millimeter sizes can also delay the snow line’s migration to the 1 au orbit by up to a few million years. We conclude that accounting for dust growth is essential for accurately modeling the snow line evolution and terrestrial planet formation in magnetically accreting protoplanetary disks.
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Dissertations / Theses on the topic "Disks"

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Grundstrom, Erika Dawn. "Hot Stars with Disks." Digital Archive @ GSU, 2007. http://digitalarchive.gsu.edu/phy_astr_diss/19.

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The evolutionary paths of the massive O and B type stars are often defined by angular momentum transformations that involve circumstellar gas disks. This circumstellar gas is revealed in several kinds of observations, and here I describe a series of investigations of the hydrogen line emission from such disk using detailed studies of five massive binaries and a survey of 128 Be stars. By examining three sets of spectra of the active mass-transfer binary system RY Scuti, I determined masses of 7.1 +/- 1.2 M_sun for the bright supergiant and 30.0 +/- 2.1 M_sun for the massive companion that is hidden by an accretion torus. I also present a cartoon model of the complex mass flows in the system. Using optical spectroscopy and X-ray flux data, I investigated the mass transfer processes in four massive X-ray binaries (a massive B star with mass flowing onto a compact, neutron star companion). The B-supergiant system LS I +65 010 transfers mass via stellar winds. I find the X-ray flux modulates with the orbital period. In the other three X-ray binary systems (LS I +61 303, HDE 245770, and X Persei), an outflowing circumstellar disk is responsible for the mass transfer, and in all three systems, the disk appears to be truncated by gravitational interactions with the compact companion. The disk in the microquasar system LS I +61 303 is limited in radius by the periastron separation and an increase in both H-alpha equivalent width and X-ray flux following periastron may be due to a density wave in the disk induced by tidal forces. Observations of HDE 245770 document what appears to be the regeneration of a circumstellar disk. The disk of X Persei appears to have grown to near record proportions and the X-ray flux has dramatically increased. Tidal interaction may generate a spiral density wave in the disk and cause an increase in H-alpha equivalent width and mass transfer to the compact companion. During the course of the analysis of the X-ray binaries, I developed numerical models for estimating the size of the Be star disks using just the H-alpha equivalent width. Finally, I present the results of a three year spectroscopic survey of both the H-alpha and H-gamma regions of 128 Be stars. I find that the median fractional variation in the equivalent width of the disk emission lines is 15% over a two year period. I also find that two-thirds of the sample displays evidence of Fe II emission or absorption resulting from surrounding circumstellar material. Many candidates for non-radial pulsation and binary systems are also found. Spectra and notes for all of the sample stars are presented in an appendix.
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Muranushi, Takayuki. "Lightning in Protoplanetary Disks." 京都大学 (Kyoto University), 2013. http://hdl.handle.net/2433/180374.

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Cavallius, Maria. "Gas in Debris Disks." Licentiate thesis, Stockholms universitet, Institutionen för astronomi, 2020. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-186017.

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Chiang, Eugene Goldreich Peter Martin. "Circumstellar and circumplanetary disks /." Diss., Pasadena, Calif. : California Institute of Technology, 2000. http://resolver.caltech.edu/CaltechETD:etd-09172008-151500.

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Pohlen, Michael. "The radial structure of galactic stellar disks surface photometric study on disk galaxies /." [S.l.] : [s.n.], 2001. http://deposit.ddb.de/cgi-bin/dokserv?idn=964128535.

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Lobo, Gomes Aiara [Verfasser], and Hubert [Akademischer Betreuer] Klahr. "Planet-disk interactions in non-isothermal disks / Aiara Lobo Gomes ; Betreuer: Hubert Klahr." Heidelberg : Universitätsbibliothek Heidelberg, 2015. http://d-nb.info/1180502523/34.

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Li, Guijun, and 李桂君. "Development of recording technology with FePt recording media and magnetic tunnel junction sensors with conetic alloy." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 2013. http://hub.hku.hk/bib/B50899776.

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With highly demanding requirement in current emerging cloud storage and personal computers, hard disk drive recording with high stability and high volume has attached much attention in industry and academy. Recording media and recording head feasible for future high-density recording are both crucial to utilize magnetic recording with 1T bit/in2 recording density. Recoding media with FePt for high density and high stability was investigated in this thesis using FePt polymers with imprinting methods and FePt thin films with ion-beam bombardment technologies. The FePt polymers can be patterned using imprint at micro-and nano-scales. The micro-and nano-patterns could be retained on substrates after sintering at high temperatures. The high magnetic coercivity was proved with line and dot patterns at different scales. Recording heads with Al2O3based magnetic tunneling junction sensors were also studied in thesis. The magnetic tunneling junction sensors were proved to work stable at different temperatures varying from -30oC to 100oC. The long time running test up to 100 hours also proved the stability of the magnetic tunneling junction sensors working in extreme temperatures. Withstate-of-art patterning and depositing technologies, new ideas about using FePt polymer to work as magnetic recording media and using ion beam bombardments to tune the FePt magnetic properties were verified. The feasibility of using Al2O3 based magnetic tunneling junction sensors as recording head was also discussed.
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Electrical and Electronic Engineering
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Bastos, Martins Ledo Hugo Ricardo. "A census of nuclear stellar disks in early-type galaxies." Thesis, University of Hertfordshire, 2016. http://hdl.handle.net/2299/17184.

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In this thesis we explored the use of nuclear stellar discs as tracers of the merging history of early-type galaxies. These small structures, just a few tens to a few hundreds of parsecs across, are a common but poorly studied feature of early-type galaxies. They are formed during or shortly after merging events due to the infall of gas, which settles in a disc and leads to the formation of new stars. Initial simulations showed that they should not survive a following major merger and could, therefore, be used to trace the epoch when their host galaxies experienced their last major merger event. We produced the first census of nuclear discs and established that their incidence is 20%, fairly independent of the host-galaxy mass or galactic environment. Furthermore, we have more than doubled the sample of nuclear discs with known photometric properties, finding that they give a hint of possessing different characteristics from those of large, galactic discs. Using these nuclear discs as clocks for the assembly history of galaxies requires dating their stellar populations. By combining the use of integral-field spectroscopy with the a priori knowledge of the relative bulge- and disc-light contribution to the observed spectra, as determined by a photometric disc-bulge decomposition, we have shown that it is possible to reduce the degeneracies that affect the study of two superimposed populations and thus that the age of stellar discs can be measured more precisely. To illustrate our method, we present VLT-VIMOS data for NGC 4458, a low-mass slowly rotating early-type galaxy with a disc that we found to be at least 5-6 Gyr old. The presence of such an old central disc in such a small, slowly-rotating and, mostly likely, round galaxy is particularly puzzling and presents a challenge to existing models. Disc fragility is central to our studies and we have expanded the limited initial simulations to study it in more detail. By means of N-body simulations, we have reproduced the final stages of a galaxy encounter by exposing a nuclear disc rotating in the gravitational potential of its host bulge and central supermassive black hole to the impact of a secondary massive black hole. We explored not only major mergers (1:1 mass ratio), but also large minor mergers (1:5 and 1:10), across a variety of collision angles, and assessed the survival of the disc, as perceived by current observational limits, both for photometry and spectroscopy. As expected, the discs do not survive a major merger whereas it is in general possible to detect their presence after a 1:5 or 1:10 encounter, in particular when looking at kinematic signatures with spectroscopy. This thesis has demonstrated that nuclear discs constitute both a common and accurate tool for constraining the assembling history of nearby early-type galaxies. The advent of more sensitive integral-field spectrographs, such as MUSE, will make measuring the stellar age of nuclear discs not only more precise, but also more economical in terms of telescope time. This will allow embarking on a more systematic age dating campaign for nuclear stellar discs across a wider range of type, mass and galactic environments for their host galaxies. Combining such a census with a larger set of numerical simulations aimed at calibrating better the range of merger event that would erase any photometric or kinematic signature of a nuclear disc, should finally allow us to put firm constraints on the merging history of early-type galaxies.
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Dånmark, Anders. "Volume measurement of wood disks." Thesis, Uppsala universitet, Bildanalys och människa-datorinteraktion, 2013. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-212199.

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At the Department of Forest Products at Swedish University of Agricultural Sciences different metrics for wood are used. The volume of wood disks' is measured using archimedes principle.There are concerns of how accurate this measurement is and a different measuringsystem is wanted. This thesis has investigated the possibility of measuring the disks' volumes with imageanalysis. The recovery error should be less than 1% of the actual volume. In general, there are two methods for recovering an object using imageanalysis, active and passive methods. Compairing active and passive methods, active methods usually require simple algorithms but more expensive equipment compared to passive methods. Different methods for measuring objects' volumes have been evaluated and the choosen method was ``shape from silhouette''. Shape from silhouette is a passive method, only using the silhouette of anobject from multiple views to recover the objects volume. Passive methods have one drawback, they can only recover the visual hull of an object and the wood disks can be slightly concave. Due to the questionable accuracy of the current measurement method it was still deemed as possible to achieve at least equal performance. When the volume measuring algorithm was developed it was first tested in two simulations using on a sphere to determine its performance with different voxel sizes and different number of images. The algorithm performed well and an error of less than 1 % was achieved with a sphere. A third simulation was performed using a simulated wood disk, which is a much more complex object, and 5 % accuracy was achieved. Finally, an experiment on real images was performed. This experiment did, however, fail due to the low quality imaging setup. The conclusion of this thesis is that itis not possible to achieve less than 1 % accuracy of the recovered volume using the shape from silhouette technique.
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Yoachim, Peter. "Thick disks in external galaxies /." Thesis, Connect to this title online; UW restricted, 2007. http://hdl.handle.net/1773/5444.

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Books on the topic "Disks"

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Fridman, Alexei M., Mikhail Ya. Marov, and Ilya G. Kovalenko, eds. Astrophysical disks. Dordrecht: Springer Netherlands, 2006. http://dx.doi.org/10.1007/1-4020-4348-1.

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F, Dermott S., Hunter J. H, and Wilson R. E. 1937-, eds. Astrophysical disks. New York: New York Academy of Sciences, 1992.

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Sinclair, Ian Robertson. Hard disks. Oxford: Newtech, 1992.

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Kato, Shoji. Oscillations of Disks. Tokyo: Springer Japan, 2016. http://dx.doi.org/10.1007/978-4-431-56208-5.

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Barden, R. A. Using floppy disks. Manchester: National Computing Centre, 1987.

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Taylor, Allen G. Using hard disks with PCs. Englewood Cliffs: Prentice-Hall, 1987.

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Blanc, Michel, Gregory J. Herczeg, Veerle Sterken, Helmut Lammer, Willy Benz, Stéphane Udry, Rafael Rodrigo, and Maurizio Falanga, eds. From Disks to Planets. Dordrecht: Springer Netherlands, 2018. http://dx.doi.org/10.1007/978-94-024-1518-6.

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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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Saffady, William. Optical disks vs. micrographics. Westport: Meckler, 1993.

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Book chapters on the topic "Disks"

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Kundt, Wolfgang. "Disks." In Astronomy and Astrophysics Library, 75–81. Berlin, Heidelberg: Springer Berlin Heidelberg, 2001. http://dx.doi.org/10.1007/978-3-662-04347-9_6.

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Eschenauer, H., N. Olhoff, and W. Schnell. "Disks." In Applied Structural Mechanics, 93–99. Berlin, Heidelberg: Springer Berlin Heidelberg, 1997. http://dx.doi.org/10.1007/978-3-642-59205-8_8.

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Fridman, Alexei M., E. V. Polyachenko, Yu M. Torgashin, S. G. Yanchenko, and E. N. Snezhkin. "The Over-Reflection Instability: Myth or Reality?" In Astrophysical disks, 3–22. Dordrecht: Springer Netherlands, 2006. http://dx.doi.org/10.1007/1-4020-4348-1_1.

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Barkov, Maxim V., and Gennady S. Bisnovatyi-Kogan. "Gamma-Ray Burst Interaction with Dense Interstellar Medium." In Astrophysical disks, 197–204. Dordrecht: Springer Netherlands, 2006. http://dx.doi.org/10.1007/1-4020-4348-1_10.

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Kaigorodov, P. V., D. V. Bisikalo, A. A. Boyarchuk, and O. A. Kuznetsov. "Morphology of the Interaction between the Stream and Cool Accretion Disc in Semidetached Binaries." In Astrophysical disks, 205–16. Dordrecht: Springer Netherlands, 2006. http://dx.doi.org/10.1007/1-4020-4348-1_11.

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Khoperskov, Alexander V., and Sergej S. Khrapov. "Computer Modeling of Non-Stationary Gas Quasi-Keplerian Disk." In Astrophysical disks, 217–29. Dordrecht: Springer Netherlands, 2006. http://dx.doi.org/10.1007/1-4020-4348-1_12.

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Kovalenko, I. G., M. A. Eremin, and V. V. Korolev. "3D Structure of Gaseous Disks in Spiral Galaxies." In Astrophysical disks, 231–40. Dordrecht: Springer Netherlands, 2006. http://dx.doi.org/10.1007/1-4020-4348-1_13.

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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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Okuda, Toru. "2D-Simulations of Subcritical and Supercritical Accretion Disks Around Black Holes." In Astrophysical disks, 259–74. Dordrecht: Springer Netherlands, 2006. http://dx.doi.org/10.1007/1-4020-4348-1_15.

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Sil'chenko, O. K. "Separate Circumnuclear Stellar and Gaseous Disks in Disk Galaxies." In Astrophysical disks, 275–90. Dordrecht: Springer Netherlands, 2006. http://dx.doi.org/10.1007/1-4020-4348-1_16.

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Conference papers on the topic "Disks"

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Komma, Yoshiaki, Shin-ichi Kuwamoto, Hideki Aikou, Kenichiro Urairi, Michihiro Yamagata, and Yasuhiro Tanaka. "Holographic Optical Element For A Dual Focus Optical Head." In Diffractive Optics and Micro-Optics. Washington, D.C.: Optica Publishing Group, 1998. http://dx.doi.org/10.1364/domo.1998.dwb.1.

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A high density optical disk format named DVD adopts a 0.6 mm disk to simultaneously use a high numerical aperture (NA) lens and gain tolerance of disk tilt.1 Because of the immense popularity of the CD format, it is important to playback the current widely used Compact Discs (CDs) on DVD format players. This requires an optical head that can read both conventional 1.2 mm disks and the new 0.6 mm disk. To read both disks with the same optical head, it is necessary to overcome spherical aberration caused by the difference in disk thickness.
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Komina, Yoshiaki, Yasuhiro Tanaka, Kenichiro Urairi, Seiji Nishino, and Sadao Mizuno. "Dual Focus Optical Head with A Hologram-Integrated Lens." In Symposium on Optical Memory. Washington, D.C.: Optica Publishing Group, 1996. http://dx.doi.org/10.1364/isom.1996.othc.1.

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Development of a high density optical disk format named DVD was agreed upon last year (1995). The format adopts a 0.6 mm disk to simultaneously use a high numerical aperture (NA) lens and gain tolerance of disk tilt.1 Because of a Immense popularity of the CD format, it is important to playback the current, widely used Compact Discs (CDs) on the DVD format player. This requires an optical head that can read both conventional 1.2 mm disks and the new 0.6 mm disk. To read both disks with the same optical head, it is necessary to correct spherical aberration, which is caused by the difference in disk thickness.
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Khaibrakhmanov, S., and A. Dudorov. "Dynamics of magnetic flux tubes in accretion disks of Herbig Ae/Be stars." 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/vak2021.2022.1.1.048.

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The dynamics of magnetic flux tubes (MFTs) in accretion disks of Herbig Ae/Be stars with fossil large-scale magnetic fieldis modeled. The model takes into account the buoyant force, turbulent and aerodynamic drag, radiative heat exchange withthe surrounding gas, and the magnetic field of the disk. The structure of the disk is calculated using our MHD model,taking into account the heating of the surface layers of the disk with the intense stellar radiation. The simulations showthat MFTs periodically rise from the disk with speeds of 10 − 12 km s −1 and form an outflowing magnetized corona of thedisk. MFTs can experience magnetic oscillations under the action of the external magnetic field near the disk’s surface. Weargue that the oscillations can produce observed IR-variability of Herbig Ae/Be stars, which would be more intense thanin the case of T Tauri stars, since the disks of Herbig Ae/Be stars are hotter, denser and have stronger magnetic field.
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Tian, Shuqing, and Yatao Zhu. "Disk Heat Transfer Analysis in a Heated Rotating Cavity With an Axial Throughflow." In ASME Turbo Expo 2012: Turbine Technical Conference and Exposition. American Society of Mechanical Engineers, 2012. http://dx.doi.org/10.1115/gt2012-69185.

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In the rotating disk cavities of aero-engine compressors, buoyancy-induced flow and heat transfer can occur due to thermal gradients between cooling air and hot surfaces. The simplified rotating cavity with two plane discs, a shaft and a cylindrical rim has been investigated numerically and compared with the available measurements. Two models have been solved using a commercial CFD code, Fluent, with the RNG k-ε turbulence model. The first one is the conventional model with only fluid region solved, a temperature profile with the linear radial gradient imposed at the disk walls, and an isothermal boundary condition imposed at the shroud wall. The second one is the model with thick-walled disks and shroud, an adiabatic boundary condition imposed at the outer walls of the disks, and an isothermal boundary condition imposed at the outer wall of the shroud. The fluid and solid are coupled solved simultaneously. The disk temperatures are computed. In the present work, the numerical results are in reasonable agreement with the measurements. The computed disk temperatures in the second model have approximately linear radial gradients over the first three-quarters of the disks, and in the last quarter of the disks the temperature radial gradients are obviously non-linear. The different disk temperature profiles in these two models do not lead to obviously different disk heat transfers. The heat transfer in the rotating cavity leads to a considerable temperature increase of the cavity core fluid, therefore a corresponding increase of the outlet temperature. These two temperature increases are critical for the cooling design in aero-engines.
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Jin-Hong Kim, M. R. Kim, and Dae-Eun Kim. "Head-disk interface in near-field recording disks." In 2002 International Symposium on Optical Memory and Optical Data Storage Topical Meeting. Joint International Symposium on Optical Memory and Optical Data Storage 2002. Technical Digest. IEEE, 2002. http://dx.doi.org/10.1109/omods.2002.1028572.

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Daniels, W. A., B. V. Johnson, and D. J. Graber. "Aerodynamic and Torque Characteristics of Enclosed Co/Counter Rotating Disks." In ASME 1989 International Gas Turbine and Aeroengine Congress and Exposition. American Society of Mechanical Engineers, 1989. http://dx.doi.org/10.1115/89-gt-177.

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Experiments were conducted to determine the aerodynamic and torque characteristics of adjacent rotating disks enclosed in a shroud. These experiments were performed to obtain an extended data base for advanced turbine designs such as the counter-rotating turbine. Torque measurements were obtained on both disks in the rotating frame of reference for co-rotating, counter-rotating and one-rotating/one-static disk conditions. The disk models used in the experiments included disks with typical smooth turbine geometry, disks with bolts, disks with bolts and partial bolt covers and flat disks. A windage diaphragm was installed at mid-cavity for some experiments. The experiments were conducted with various amounts of coolant throughflow injected into the disk cavity from the disk hub or from the disk OD with swirl. The experiments were conducted at disk tangential Reynolds number up to 1.6×107 with air as the working fluid. The results of this investigation indicated that the static shroud contributes a significant amount to the total friction within the disk system, the torque on counter-rotating disks is essentially independent of coolant flow total rate, flow direction and tangential Reynolds number over the range of conditions tested and a static windage diaphragm reduces disk friction in counter-rotating disk systems.
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Tsunoda, Yoshito, and Masahiro Ojima. "Advanced Technologies for the Next Generation Optical Disks." In Optical Data Storage. Washington, D.C.: Optica Publishing Group, 1987. http://dx.doi.org/10.1364/ods.1987.wd1.

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Application areas of optical disk systems have been expanding slowly but stably into the market during these few years. So far optical disks systems are widely used for image and document data storage. This application area is thought to be the most appropriate for the present performances and the functions of optical disks. One of the biggest limiting factor of the present optical disks for applying to directly competitive market with the conventional magnetic disk storage systems is their slow data processing time including data transfer rate, accessing time, and disk rotaion time. These problems have to be solved in order to apply optical disks to more general application areas where conventional magnetic disk storage systems are widely used.
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Doolin, Samuel, and Katherine M. Blundell. "Circumbinary Disks." In VII Microquasar Workshop: Microquasars and Beyond. Trieste, Italy: Sissa Medialab, 2009. http://dx.doi.org/10.22323/1.062.0103.

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Acharya, Anurag, Mustafa Uysal, and Joel Saltz. "Active disks." In the eighth international conference. New York, New York, USA: ACM Press, 1998. http://dx.doi.org/10.1145/291069.291026.

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Acharya, Swarup, Rafael Alonso, Michael Franklin, and Stanley Zdonik. "Broadcast disks." In the 1995 ACM SIGMOD international conference. New York, New York, USA: ACM Press, 1995. http://dx.doi.org/10.1145/223784.223816.

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Reports on the topic "Disks"

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Psaltis. Holographic 3D Disks. Fort Belvoir, VA: Defense Technical Information Center, January 2000. http://dx.doi.org/10.21236/ada377847.

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Tkac, P., G. F. Vandegrift, and J. Harvey. Dissolution of Sintered Mo Disks. Office of Scientific and Technical Information (OSTI), October 2013. http://dx.doi.org/10.2172/1132238.

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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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Psaltis, Demetri. Parallel Readout of Optical Disks. Fort Belvoir, VA: Defense Technical Information Center, August 1992. http://dx.doi.org/10.21236/ada256625.

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Tkac, Peter, and George Vandegrift. Dissolution of Sintered Mo Disks. Office of Scientific and Technical Information (OSTI), October 2014. http://dx.doi.org/10.2172/1159189.

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Fusco, A. M. Development report for dual-burst disks. Office of Scientific and Technical Information (OSTI), November 1996. http://dx.doi.org/10.2172/399720.

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Bahder, Thomas B. Stress in Rotating Disks and Cylinders. Fort Belvoir, VA: Defense Technical Information Center, October 2002. http://dx.doi.org/10.21236/ada407981.

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Fowley, M., and D. Herman. BACKPRESSURE TESTING OF ROTARY MICROFILTER DISKS. Office of Scientific and Technical Information (OSTI), April 2011. http://dx.doi.org/10.2172/1018680.

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Li, Yaping. IC project: Exploring Planet-disk Interaction in Dusty Protoplanetary Disks and Their Observational Implications. Office of Scientific and Technical Information (OSTI), January 2021. http://dx.doi.org/10.2172/1756776.

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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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