FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W2057906648> ?p ?o ?g. }

• W2057906648 endingPage "1006" @default.
• W2057906648 startingPage "990" @default.
• W2057906648 abstract "We analyze the dynamics of gas-dust coupling in the presence of stellar radiation pressure in circumstellar disks, which are in a transitional stage between the gas-dominated, optically thick, primordial nebulae, and the dust-dominated, optically thin Vega-type disks. Dust grains undergo radial migration, either leaving the disk owing to a strong radiation pressure or seeking a stable equilibrium orbit in corotation with gas. In our models of A-type stars surrounded by a total gas mass from a fraction to dozens of Earth masses, the outward migration speed of dust is comparable with the gas sound speed. Equilibrium orbits are circular, with exception of those significantly affected by radiation pressure, which can be strongly elliptic with apocenters extending beyond the bulk of the gas disk. The migration of dust gives rise to radial fractionation of dust and creates a variety of possible observed disk morphologies, which we compute by considering the equilibrium between the dust production and the dust-dust collisions removing particles from their equilibrium orbits. Large grains (typically ≳200 μm) are distributed throughout most of the gas disk. Smaller grains (in the range of 10-200 μm) concentrate in a prominent ring structure in the outer region of the gas disk (presumably at radius ~100 AU), where gas density is rapidly declining with radius. The width and density, as well as density contrast of the dust ring with respect to the inner dust disk, depend on the distribution of gas and the mechanical strength of the particles. Our results open the prospect for deducing the distribution of gas in circumstellar disks by observing their dust. We have qualitatively compared our models with two observed transitional disks around HR 4796A and HD 141569A. Dust migration can result in observation of a ring or a bimodal radial dust distribution, possibly very similar to the ones produced by gap-opening planets embedded in the disk, or shepherding it from inside or outside. We conclude that a convincing planet detection via dust imaging should include specific nonaxisymmetric structure (spiral waves, streamers, resonant arcs) following from the dynamical simulations of perturbed disks." @default.
• W2057906648 created "2016-06-24" @default.
• W2057906648 creator A5037499522 @default.
• W2057906648 creator A5086254822 @default.
• W2057906648 date "2001-08-20" @default.
• W2057906648 modified "2023-09-24" @default.
• W2057906648 title "Dust Migration and Morphology in Optically Thin Circumstellar Gas Disks" @default.
• W2057906648 cites W1620503833 @default.
• W2057906648 cites W1965917463 @default.
• W2057906648 cites W1966079298 @default.
• W2057906648 cites W1967383708 @default.
• W2057906648 cites W1975298624 @default.
• W2057906648 cites W1977509740 @default.
• W2057906648 cites W1979623117 @default.
• W2057906648 cites W1984949110 @default.
• W2057906648 cites W1998759826 @default.
• W2057906648 cites W2001281840 @default.
• W2057906648 cites W2002923409 @default.
• W2057906648 cites W2005473903 @default.
• W2057906648 cites W2008385987 @default.
• W2057906648 cites W2027135516 @default.
• W2057906648 cites W2030970292 @default.
• W2057906648 cites W2041672820 @default.
• W2057906648 cites W2042967366 @default.
• W2057906648 cites W2054681472 @default.
• W2057906648 cites W2063932574 @default.
• W2057906648 cites W2068433364 @default.
• W2057906648 cites W2071555310 @default.
• W2057906648 cites W2089937350 @default.
• W2057906648 cites W2093586159 @default.
• W2057906648 cites W2094528159 @default.
• W2057906648 cites W2094844733 @default.
• W2057906648 cites W2095786720 @default.
• W2057906648 cites W2096568039 @default.
• W2057906648 cites W2103158982 @default.
• W2057906648 cites W2111480616 @default.
• W2057906648 cites W2119680152 @default.
• W2057906648 cites W2124845382 @default.
• W2057906648 cites W2129772716 @default.
• W2057906648 cites W2132191748 @default.
• W2057906648 cites W2139997228 @default.
• W2057906648 cites W2149520698 @default.
• W2057906648 cites W2156255672 @default.
• W2057906648 cites W2156627705 @default.
• W2057906648 cites W3098297217 @default.
• W2057906648 cites W3098885964 @default.
• W2057906648 cites W3100630914 @default.
• W2057906648 cites W3101158613 @default.
• W2057906648 cites W3102391372 @default.
• W2057906648 cites W3102854319 @default.
• W2057906648 cites W343244306 @default.
• W2057906648 cites W4243057562 @default.
• W2057906648 cites W4250864308 @default.
• W2057906648 cites W4251585788 @default.
• W2057906648 doi "https://doi.org/10.1086/322252" @default.
• W2057906648 hasPublicationYear "2001" @default.
• W2057906648 type Work @default.
• W2057906648 sameAs 2057906648 @default.
• W2057906648 citedByCount "185" @default.
• W2057906648 countsByYear W20579066482012 @default.
• W2057906648 countsByYear W20579066482013 @default.
• W2057906648 countsByYear W20579066482014 @default.
• W2057906648 countsByYear W20579066482015 @default.
• W2057906648 countsByYear W20579066482016 @default.
• W2057906648 countsByYear W20579066482017 @default.
• W2057906648 countsByYear W20579066482018 @default.
• W2057906648 countsByYear W20579066482019 @default.
• W2057906648 countsByYear W20579066482020 @default.
• W2057906648 countsByYear W20579066482021 @default.
• W2057906648 countsByYear W20579066482022 @default.
• W2057906648 countsByYear W20579066482023 @default.
• W2057906648 crossrefType "journal-article" @default.
• W2057906648 hasAuthorship W2057906648A5037499522 @default.
• W2057906648 hasAuthorship W2057906648A5086254822 @default.
• W2057906648 hasBestOaLocation W20579066481 @default.
• W2057906648 hasConcept C121332964 @default.
• W2057906648 hasConcept C150846664 @default.
• W2057906648 hasConcept C178635117 @default.
• W2057906648 hasConcept C190841160 @default.
• W2057906648 hasConcept C38652104 @default.
• W2057906648 hasConcept C41008148 @default.
• W2057906648 hasConcept C44870925 @default.
• W2057906648 hasConcept C68337447 @default.
• W2057906648 hasConcept C8865038 @default.
• W2057906648 hasConceptScore W2057906648C121332964 @default.
• W2057906648 hasConceptScore W2057906648C150846664 @default.
• W2057906648 hasConceptScore W2057906648C178635117 @default.
• W2057906648 hasConceptScore W2057906648C190841160 @default.
• W2057906648 hasConceptScore W2057906648C38652104 @default.
• W2057906648 hasConceptScore W2057906648C41008148 @default.
• W2057906648 hasConceptScore W2057906648C44870925 @default.
• W2057906648 hasConceptScore W2057906648C68337447 @default.
• W2057906648 hasConceptScore W2057906648C8865038 @default.
• W2057906648 hasIssue "2" @default.
• W2057906648 hasLocation W20579066481 @default.
• W2057906648 hasLocation W20579066482 @default.
• W2057906648 hasOpenAccess W2057906648 @default.
• W2057906648 hasPrimaryLocation W20579066481 @default.

• next