optical disk

Definitions

  • WordNet 3.6
    • n optical disk a disk coated with plastic that can store digital data as tiny pits etched in the surface; is read with a laser that scans the surface
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Usage

In literature:

An appreciation of the condition of the optic disk is one of the chief objects of the ophthalmoscope.
"Encyclopaedia Britannica, 11th Edition, Volume 10, Slice 1" by Various
Nevertheless, disks of optical glass, both crown and flint, have been produced up to 39 in.
"Encyclopaedia Britannica, 11th Edition, Volume 12, Slice 1" by Various
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In news:

Your client has decided to shoot their weekly services and share them via streaming and optical disk.
Toshiba and Samsung Electronics to Integrate Optical Disk Device Businesses Sep 22, 2003 Printable format Email this Article Search.
Toshiba Corporation and Samsung Electronics Co. Ltd signed a memorandum of terms covering integration of the companies' respective optical disk drive businesses in a joint venture.
Langford, "Queueing Analysis of an Optical Disk Jukebox Based Office System," IEEE Transactions on Computers, vol 39, no.
Has three-in-one functionality as an optical disk drive, a hard disk drive and a NAS.
"Over time, an optical disc will be as much of an historical curiosity as a floppy disk ," said Michael Gartenberg, a tech-industry analyst with research firm Gartner Inc.
Added and added customer notebooks are actuality delivered after any affectionate of optical disk.
A reserved area on a computer's storage device (hard disk, optical disc, etc.
LAS VEGAS — Velocity Micro will introduce a new tablet PC at International CES this year, along with a combo hard disk/optical drive.
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In science:

Since the disk is very optically thick, the spectrum that emerges will be significantly processed, and close to a black–body shape (sometimes referred to as “grey–body”; e.g.
Hydrodynamical Response of a Circumbinary Gas Disk to Black Hole Recoil and Mass Loss
We also estimated the effective black–body temperature of the radiation emerging from the optically thick disk.
Hydrodynamical Response of a Circumbinary Gas Disk to Black Hole Recoil and Mass Loss
The new spectrum is approximately centered on the optical systemic velocity estimate of 2720 ± 15 km s−1 (Fisher et al. 1995), which is suggestive of emission from a highly inclined disk with ∼ 300 km s−1 orbital velocity, though extended line wings may suggest a somewhat more rapid rotation.
Discovery of Candidate H$_2$O Disk Masers in AGN and Estimations of Centripetal Accelerations
In general, systematic velocities that result from disk models may provide the best estimates of systemic velocity, and these might usefully be compared to the results of pointed optical and molecular line studies that include dynamical modeling.
Discovery of Candidate H$_2$O Disk Masers in AGN and Estimations of Centripetal Accelerations
YE05 Equation 4; see YE05 for a discussion of the effects of varying this initial optical depth) until the disk outer radius exceeds this value (see below); once this occurs the inner envelope radius is set equal to the disk outer radius.
Evolutionary Signatures in the Formation of Low-Mass Protostars. II. Towards Reconciling Models and Observations
In the model it thus remains fixed at the previous gridpoint, but as the mass is increasing at each timestep, the optical depth through the disk is also increasing.
Evolutionary Signatures in the Formation of Low-Mass Protostars. II. Towards Reconciling Models and Observations
Optical continuum images show a dusty circumnuclear gas disk with a well-defined spiral pattern (Gonz´alez Delgado et al. 2002, also see panel 5 in Fig. 3 of this paper).
The Nuclear Outflow in NGC 2110
None of the tested models reproduces the feature in the rotation curve satisfactorily (see Fig. 10 and Tab. 4). A truncated optical disk (see, e.g., van der Kruit, 2007) is not observed and, therefore, neither explains the feature in the rotation curve.
Cold gas in massive early-type galaxies: The case of NGC 1167
In the case of NGC 1167 it is unlikely that the H i results from stellar mass loss because the H i disk extends well beyond the optical disk (DHI = 3 × R25 ) and carries therefore more angular momentum than the stars.
Cold gas in massive early-type galaxies: The case of NGC 1167
The problem of Monte-Carlo radiation transfer in very optically thick regions – such as in the midplane of circumstellar disk s – is challenging.
On the Modified Random Walk for Monte-Carlo Radiation Transfer
For both WR winds and Be disks, the free-free flux is a function of electron density (Ne ), electron temperature (Te ), the physical size of the emitting source (Rff ), and the wavelength at which the emission becomes optically thick (λt ).
Red Eyes on Wolf-Rayet Stars: 60 New Discoveries via Infrared Color Selection
For simplicity, we assume that the dust and gas are well-mixed and the optical properties of the dust particles do not vary in the disk.
The Structure of a Self-Gravitating Protoplanetary Disk and its Implications to Direct Imaging Observations
This is because in the sub-mm wavelength, the disk is optically thin, and the observed flux is proportional to the disk surface density.
The Structure of a Self-Gravitating Protoplanetary Disk and its Implications to Direct Imaging Observations
We define the surface of the disk as the place where the optical depth towards the central star, τrad , becomes unity.
The Structure of a Self-Gravitating Protoplanetary Disk and its Implications to Direct Imaging Observations
We first calculate the optical depth, τrad , between the central star and a point (r, z ) in the disk.
The Structure of a Self-Gravitating Protoplanetary Disk and its Implications to Direct Imaging Observations
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