Sentences with phrase «outer disk»

"Outer disk" refers to the part of a disk or hard drive located on the outer edge. It contains the data that is stored farthest from the center of the disk. Full definition
The well - known outer disk is clearly detected, at higher resolution than before, and shows previously unknown sub-structures, including spirals going inwards into the cavity.
Moving out from this central galactic bulge, the panorama sweeps from the galaxy's central bulge across lanes of stars and dust to the sparser outer disk.
When comparing the chemical compositions of these stars with the ones found in other cosmic structures, the scientists were surprised to find that the chemical compositions are almost identical, both within and between these groups, and closely match the abundance patterns of the Milky Way outer disk stars.
The inner edge of the optically - thick outer disk must be heated almost frontally by the star to account for the excess flux at mid-IR wavelengths.
These images further allow us to trace the gap edge in scattered light at all position angles and search the inner and outer disks for morphological substructure.
We construct a radiative transfer model that accounts for the main characteristics of the features with an inner and outer disk misaligned by ~ 72 degrees.
The well - known outer disk is clearly detected, at higher resoluti... ▽ More We have observed the protoplanetary disk of the well - known young Herbig star HD 142527 using ZIMPOL Polarimetric Differential Imaging with the VBB (Very Broad Band, ~ 600 - 900nm) filter.
Astronomers who studied these images eventually realized that the nascent solar system had twisted inner and outer disks, not just one flat disk, and the moving material was causing the shadows, much like a bird flying in front of a lighthouse's lamp.
Meanwhile the outer disk, which rotates slower than the planet, pushes it inward.
In the case of a lonely planet, the inner disk is significantly depleted relative to the outer disk because the planet blocks part of the gas flow from the outer to the inner part, so the outer disk wins.
Thus, the direction of migration of a planet depends on the relative importance of the inner versus outer disks.
But in the inner disk, warm gas would fight against the planet's weak gravity, so the cold and dense gas of the outer disk is the more likely womb.
Maybe turbulence in the disk took the grains outward, or maybe crystallization occurred in the outer disk under the influence of cosmic rays or lightning.
The gravitational interactions created in the outer disk by this massive star apparently acted as a catalyst for the gathering of debris to form other smaller, more distant moons.
The authors suggest that the materials the Moon initially accumulates from the outer disk could be volatile - rich, followed by a final 100 - to 500 - kilometer layer of volatile - poor material.
In reality, since we are looking at SS 433 almost along the disk plane, our line - of - sight view towards the inner disk is blocked by the outer disk.
These spontaneous traps then concentrate the grains coming from the outer disk regions, creating a very dense ring of solids, and giving a helping hand to the formation of planets.
The stars appear to be associated with a dwarf galaxy Chakrabarti predicted in 2009 based on her analysis of ripples in the Milky Way's outer disk.
The oxygen would have «burned up» the carbon to produce gases such as carbon dioxide and monoxide, which would have moved into the outer disk along with water vapor before chilling into ices, so that any solid carbon in the inner solar system would have been destroyed within a few years.
Or, such shadows may also change the temperature of the outer disk (it will be cooler in the shadows), which would in turn change the overall structure of the disk, giving rise to a spiral arms as changes propagate in the disk — translating a shadow to a physical evolution in the disk.
At dozens of points throughout the outer disk of the galaxy, we see knots of light representing the emission glow from enormous clouds of hydrogen gas.
If this were our own Solar System, the Voyager 1 probe — the most distant manmade object from Earth — would be at approximately the inner edge of the outer disk.
It was proposed that shadows from in the inner, faster - orbiting disks may be projected to the outer disk, creating the illusion of structures (like the larger dark gaps where the spiral arms join the rings, and elsewhere), where none exists.
Because a «small» protoplanet (up to a few Earth masses) lacks sufficient gravitational pull to open a gap in the protostar's disk, it will move inward as the disk lying inside the protoplanet's orbit transfers angular momentum to it at a slower rate than it is transferring angular momentum to the outer disk (through interactions with Lindblad resonances induced in the disk).
Subtler evidence of star formation can also be seen marking the outer disk of NGC 1512.
The vortex throws a non-axisymmetric shadow on the outer disk.
I will describe how scattered light from the outer disk can match the T Cha datasets, why such a model is unsuitable for LkCa 15, and the characteristics of the LkCa 15 protoplanetary system.
Close to the star, dust scattering is detected at high signal - to - noise ratio, but it is unclear whether the signal represents the inner disk, which has been linked to the two prominent local minima in the scattering of the outer disk, interpreted as shadows.
We confirm that the dominant source of emission is forward scattered light from the near edge of the outer disk.
Previous disk observations have focused mainly on the outer disk, which is cleared inward of ~ 50 au.
The outer disk, which extends to at least 140 AU in radius, is very optical... ▽ More We have developed a self - consistent model of the disk around the nearby 10 Myr old star TW Hya which matches the observed spectral energy distribution and 7 mm images of the disk.
The outer disk, which extends to at least 140 AU in radius, is very optically thick at IR wavelengths and quite massive ~ 0.06 Msun for the relatively advanced age of this T Tauri star.
The disk around T Cha is detected in all observing modes and its outer disk is resolved in scattered light with unprecedented angular resolution and signal - to - noise.
The outer disk appears smooth with slight azimuthal variations in polarized surface brightness, which may be due to shadowing from the inner disk or a two - peaked polarized phase function.
Our model requires a distinct transition in disk properties at ~ 4 AU, separating the inner and outer disk.
We speculate that this truncation of the outer disk may be the signpost of a developing gap due to the effects of a growing protoplanet; the gap is still presumably evolving because material still resides in it, as indicated by the silicate emission, the molecular hydrogen emission, and by the continued accretion onto the central star (albeit at a much lower rate than typical of younger T Tauri stars).
Our optimal axisymmetric radiative transfer model considers two coplanar inner and outer disks, separated by a gap of 0.28» (~ 30au) in size.
«ALMA Sheds Light on Planet - Forming Gas Streams — Tantalising signs of flows feeding gas - guzzling giant planets» The above article published in January 2013 by S. Casassus describes the planet formation in the disk closer to the central star, but there is no discussion on the planet formation in the outer disk.
Inside 100 AU, the emission from cyclic - C3H2 is very weak, which indicates chemical differentiation between the inner and outer disk.
The outer disk begins to form planets, as matter sticks together in an orbit around the core [source: HubbleSite].
Through their prior observations of the disk around HD142527 with the Subaru Telescope, they discovered a gap inside the disk and peculiar shape of the outer disk (* 3).
The outflow is launched from the surface of the outer disk.
The distribution of the cold dust is mostly concentrated near the center, and exhibits smoothly distributed over the entire extent of the galaxy, whereas the distribution of the warm dust indicates some correlation with the spiral arms, and has spotty structures such as four distinctive bright spots in the outer disk in addition to a bar - like feature near the center tracing the CO intensity map.
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