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The objective of this study was to assess the cost-effectiveness of the Argus® II Retinal Prosthesis System (Argus II) in Retinitis Pigmentosa (RP) patients. ... Second Sight Medical Products Inc. developed Argus II, a retinal prosthesis system for treating RP. ... Markov model for the Argus II Retinal Prosthesis System begins at the age of 46 years as most of the RP patients are legally blind by this age. ...doi:10.1186/1471-2415-14-49 pmid:24731533 pmcid:PMC3990272 fatcat:xvnykepvnjc7bdytitcs7ncdc4
Monthly Notices of the Royal Astronomical Society: Letters
The physical sizes of TDE accretion discs are regularly inferred, from modelling of the TDEs X-ray spectrum as a single temperature blackbody, to be smaller than the plausible event horizons of the black ... We further demonstrate that the disc-observer inclination angle and absorption of X-ray photons may both lead to additional underestimation of the radial sizes of TDE discs, but by smaller factors. ... The distribution of R bb is plotted in blue, and Rp in red. The ISCO radius of each disc system is represented by a black dashed line. ...doi:10.1093/mnrasl/slab088 fatcat:m7lvyjok55a2rfexwead3afewq
This inescapable evolution of disc structure speeds up type I planetary migration for lower mass bodies by up to a factor of about 2. ... within the gaseous disc lifetime (∼ 1-3 Myrs). ... REP is supported by a Discovery Grant from the Natural Sciences and Engineering Research Council (NSERC) of Canada. ...doi:10.1111/j.1365-2966.2010.18135.x fatcat:okbzmergnfdltjf2a6y4vntppm
Here we show that ∼10^4 interstellar objects such as the recently detected 1I/2017-U1 ('Oumuamua) could have been captured, and become part of the young Solar System, together with up to hundreds of ∼ ... Planet formation begins with collisional growth of small planetesimals accumulating into larger ones. Such growth occurs while planetesimals are embedded in a gaseous protoplanetary disc. ... CAPTURE RATES Protoplanetary disc structure The radial and vertical structure of the PPD can be modeled from the Chiang-Goldreich simple flared disc model (Chiang & Goldreich 1997) . ...arXiv:1804.09716v4 fatcat:ru5gxrtbmnbibc7cg3oi23d3pq
Inward migration of low-mass planets and embryos of giant planets can be stopped at the disc-cavity boundaries due to co-orbital corotation torque. ... A protoplanetary disc may have several such trapping regions at various distances from the star, such as at the edge of the stellar magnetosphere, the inner edge of the dead zone, the dust-sublimation ... For comparisons with our model, we take the value of softening = 0.025, used in our model, and obtain b = /rp = 0.025/rp ≈ 0.0167 (at rp = 1.5) andb = 0.4/(b/h) ≈ 0.72. ...doi:10.1093/mnras/stz535 fatcat:aa7xf2mfxbbspkc7lgr6jctpiq
We develop a new numerical approach to describe the action of ram pressure stripping (RPS) within a semi-analytic model of galaxy formation and evolution which works in combination with non-radiative hydrodynamical ... This allows a self-consistent estimation of the RPS experienced by satellite galaxies. ... Bottom: relation between disc scalelength R d and I-band luminosity for disc galaxies, for a run of the SAG model that includes the RPS effect. ...doi:10.1111/j.1365-2966.2010.17262.x fatcat:o74tkxud3reqlm6npfperrsyj4
I have constructed a three-parameter grid of bulge/disc/halo models broadly consistent with ΛCDM, and simulated an extensive series of encounters using these models. ... The tidal morphology of an interacting system can provide useful constraints on progenitor structure. ... this system is roughly perpendicular to our line of sight. ...doi:10.1093/mnras/stv2381 fatcat:gpk4aqvuqzacdog7s4sctiuxju
To do so, we performed N-body simulations to reproduce the late phases of satellite formation and use a massive circum-planetary disc to explain the mass of this satellite. ... In our simulations of satellite formation many satellites were formed close to the planet, this scenario changed after the tidal evolution of the systems. ... In Section 2, we detail our models, explain the parameters used and study the stability of the system. ...arXiv:2005.10138v1 fatcat:uveqtzioinhufpq3xscojfilmy
I have constructed a three-parameter grid of bulge/disc/halo models broadly consistent with ΛCDM, and simulated an extensive series of encounters using these models. ... The tidal morphology of an interacting system can provide useful constraints on progenitor structure. ... this system is roughly perpendicular to our line of sight. ...arXiv:1510.03653v1 fatcat:xprxj3jo7nhn3o4hxpqu22r3ly
Using a simple analytic model for satellite galaxies in the cluster, we evaluate the effect of ram pressure stripping on the gas in the inner discs and in the haloes at different distances from the cluster ... This scenario explains the presence of quenched galaxies, preferentially discs, at the outskirts of galaxy clusters, and the delayed quenching of satellites compared to central galaxies. ... This work was supported by ISF grant 24/12, by GIF grant G-1052-104.7/2009, by a DIP grant, by the I-CORE Program of the PBC, by ISF grant 1829/12, and by NSF grants AST-1010033, AST-1405962 and AST-1412768 ...doi:10.1093/mnras/stx3329 fatcat:wuf4kjcpavecllr6w5zkegduge
We find that the onset of bar formation occurs more slowly in models with thicker discs. ... We also simulate disc-halo systems in the cosmological environment using a disc-insertion technique developed in a previous paper. ... JSB acknowledges the assistance of Matthew Chequers and Keir Darling in understanding the AGAMA program interface. ...doi:10.1093/mnras/stz478 fatcat:4eq2u3ipvzbfnj6r6jcwegi34u
Existing approaches to the modelling of RPS delays do not seem to include a simple and reasonably accurate analysis of realistic configurations. ... Depending on the con- figuration, the resulting missed reconnection (or RPS) delay is a potentially important load-dependent compon- ent of the disc service time. ...
We first construct well-behaved 3-D models of self-gravitating discs, and then create a suite of numerical experiments of parabolic encounters, exploring the effects of pericenter separation r_p, disc ... orientation and disc-star mass ratio (M_d/M_*) on the orbital evolution of the host stars. ... ACKNOWLEDGEMENTS The research presented here was largely carried out as part of DJM's PhD thesis at Harvard University. ...doi:10.1093/mnras/stu2220 fatcat:yqecllmewjgixg3frskhhcufvm
Previous results, obtained by Lin & Papaloizou from two-dimensional (2D) disc models, are reproduced in 3D. ... Numerical simulations of global three-dimensional (3D), self-gravitating discs with a gap opened by an embedded planet are presented. ... The setup for these runs are identical except that the disc potential is neglected in Case 0, which corresponds to the standard approach to model disc-planet systems (e.g. D'Angelo & Lubow 2010). ...doi:10.1111/j.1365-2966.2012.21955.x fatcat:ozqbd3a3izh6xgobix54trmvlq
Astronomy and Astrophysics
roughly (1/3)Rp and (2/3)Rp which May result in a rimlike or torus shaped disc structure. ... 0cm (taking into account the in- clination angle of 65°). This is quite well in accordance with (1/3)Rp (hot inner part of the disc) and (2/3)Rp (outer radius of the torus) respectively. ...
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