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Accretion Defined

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Off-site Accretion Links, User Submitted

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Mon May 4

• Astrophysical Code Library

Wed Apr 29

• Damn Interesting » Lake Peigneur: The Swirling Vortex of Doom: Never drill a hole in a lake above a mine.
• Black Hole Bipolar Jets: A fluid falling onto a small object usually cannot fall directly onto it --- most of the matter will miss the object initially, rotate around it, and only gradually be able to hit the central object. Think of draining your bathtub: Accretion disks are the celestial equivalent of this phenomenon, and can be found around black holes, neutron stars, white dwarfs, or around ordinary stars (planets are believed to form from an accretion disk around a protostar). Accretion disks around a variety of objects seem to be able to produce jets (protostars certainly do, in addition to accreting black holes). It is just that the ones from an accreting black hole tend to be the fastest and the most spectacular. A general rule of thumb is that the speed of a jet is about the same as the escape velocity of the central object --- so the jets from accreting black holes are at near the speed of light, while protostar jets are much more leisurely.

Fri Apr 17

• LRB · Hilary Mantel: What did her neighbours say when Gabriel had gone?

Wed Mar 4

• Nate Harrison

Fri Dec 26

• Astronomers Spy the Youngest Planet Ever Found

Wed Dec 10

• Reassessing the Aha! moment - International Herald Tribune

Wed Nov 19

• Kris Beckwith's Home Page

Wed Oct 29

• IPHAS, Centre for Astrophysics Research (University of Hertfordshire): Survey to be of a much use in search of accretion

Sun Sep 28

• Planetary accretion in the inner Solar System: Unlike gas-giant planets, we lack examples of terrestrial planets orbiting other Sun-like stars to help us understand how they formed. We can draw hints from elsewhere though. Astronomical observations of young stars; the chemical and isotopic compositions of Earth, Mars and meteorites; and the structure of the Solar System all provide clues to how the inner rocky planets formed. These data have inspired and helped to refine a widely accepted model for terrestrial planet formation?the planetesimal hypothesis. In this model, the young Sun is surrounded by a disk of gas and fine dust grains. Grains stick together to form mountain-size bodies called planetesimals. Collisions and gravitational interactions between planetesimals combine to produce a few tens of Moon-to-Mars-s ize planetary embryos in roughly 0.1?1 million years. Finally, the embryos collide to form the planets in 10?100 million years.

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