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The cost-effectiveness of the Argus II retinal prosthesis in Retinitis Pigmentosa patients
2014
BMC Ophthalmology
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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
Tidal disruption event discs are larger than they seem: removing systematic biases in TDE X-ray spectral modelling
2021
Monthly Notices of the Royal Astronomical Society: Letters
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2021 pre-print arXiv:2108.10160v1 fatcat:ozsfou3wpnayblgf54rhifhqwq
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
Dust settling and rapid planetary migration
2011
Monthly notices of the Royal Astronomical Society
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2010 pre-print arXiv:1012.0254v1 fatcat:w5zbt2gfrrfbxaou3u2rwetidi
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
Planet seeding through gas-assisted capture of interstellar objects
[article]
2019
arXiv
pre-print
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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
OUP accepted manuscript
2019
Monthly notices of the Royal Astronomical Society
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2018 pre-print arXiv:1809.04013v1 fatcat:xz7jbmzfdfcbxdesj5rojunwauOther Versions
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
Ram pressure stripping in a galaxy formation model - I. A novel numerical approach
2010
Monthly notices of the Royal Astronomical Society
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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
Transformations of galaxies – III. Encounter dynamics and tidal response as functions of galaxy structure
2015
Monthly notices of the Royal Astronomical Society
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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
Exploring formation scenarios for the exomoon candidate Kepler 1625b I
[article]
2020
arXiv
pre-print
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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
Transformations of galaxies. III. Encounter dynamics and tidal response as functions of galaxy structure
[article]
2015
arXiv
pre-print
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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
Quenching of satellite galaxies at the outskirts of galaxy clusters
2018
Monthly notices of the Royal Astronomical Society
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2016 pre-print arXiv:1610.02644v1 fatcat:tq2lkfkla5b7nkmfxpl7x7mwoeOther Versions
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
Can Stellar Discs in a Cosmological Setting Avoid Forming Strong Bars?
2019
Monthly notices of the Royal Astronomical Society
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2018 pre-print arXiv:1809.00090v1 fatcat:wj7uahdutzfdbhfeffo67zwar4
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
Page 40 of Computer Performance Vol. 3, Issue 1
[page]
1982
Computer Performance
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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. ...
Stellar orbit evolution in close circumstellar disc encounters
2014
Monthly notices of the Royal Astronomical Society
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2014 pre-print arXiv:1410.4561v1 fatcat:7fawtp3t2bgvda6wcpy5pgs5fiOther Versions
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
Vortex and spiral instabilities at gap edges in three-dimensional self-gravitating disc-satellite simulations
2012
Monthly notices of the Royal Astronomical Society
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2012 pre-print arXiv:1205.4034v2 fatcat:7w5vydzxobf7bnphakojlslz4mOther Versions
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
Page 175 of Astronomy and Astrophysics Vol. 109, Issue 1
[page]
1982
Astronomy and Astrophysics
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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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