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Osteolysis of the Cervical Spine after M6-C Disk Replacement due to Allergy to Polycarbonate Urethane: A Case Report and Literature Review. [PDF]

HSS J
Gonzalez D, Tang F, Khalifé M, Bitan F.
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Correction to: Gene therapy for retinitis pigmentosa and Leber congenital amaurosis caused by defects in AIPL1: effective rescue of mouse models of partial and complete Aipl1 deficiency using AAV2/2 and AAV2/8 vectors. [PDF]

Hum Mol Genet
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Evolution of Debris Disks

Annual Review of Astronomy and Astrophysics, 2008
Circumstellar dust exists around several hundred main sequence stars. For the youngest stars, that dust could be a remnant of the protoplanetary disk. Mostly it is inferred to be continuously replenished through collisions between planetesimals in belts analogous to the Solar System's asteroid and Kuiper belts, or in collisions between growing ...
Mark C Wyatt
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From Protoplanetary to Debris Disks

2002
We discuss the physical difference between protoplanetary and debris (Vega-like) disks and consider the course of evolution which leads from the first to the latter. We discuss a simple evolutionary model for debris disks and predict 20μm fluxes for future observations with VISIR.
Dominik, C., Dullemond, C.P.
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Giant Impacts and Debris Disks

Proceedings of the International Astronomical Union, 2012
AbstractDuring the last stage of terrestrial planet formation, Mars-sized protoplanets often collides with each other. Our high-resolution impact simulations show that such giant impacts produce a significant amount of fragments within the terrestrial planet region. These ejected fragments form a hot debris disk around the central star.
H. Genda, H. Kobayashi, E. Kokubo
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Planetary Perturbers in Debris Disks

Earth, Moon, and Planets, 2003
Neptune dominates the dynamics of the Kuiper Belt. By examining images of debris disks around other stars, we may be able to infer what kinds of planets shape the outer edges of other planetary systems. The last few years have seen a burst of progress in the modeling of azimuthal structures in debris disks created by planetary perturbers; new models ...
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Dynamical Processes in Debris Disks

EAS Publications Series, 2010
Debris disks are dusty and/or gasous disk that are viewed in scattered light and thermal emission around stars around 10 7 –10 8  yr. It is well known that the dust in these system is not primodial. It is short lived and must be continuously replenished by colliding planetesimals.
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