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Chapter 19 Star Formation
Chapter 19 Star Formation

... Individual cloud fragments begin to collapse. Once the density is high enough, there is no further fragmentation. Reason: the star has become opaque to its own radiation: It has a photosphere! After this, the ‘trapped radiation heats the interior of the object as it contracts. Stage 3: Object become ...
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... BBN does not generate any heavy elements! He-ashes fuse in the hot (T ≈ 108 K) and dense (n ≈ 1028 cm−3 ) core Physics demands a tiny concentration of 8 Be (n8 /n4 ≈ 10−8 ) Carbon is formed: α + α → 8 Be + α → 12 C + γ (7.367 MeV) Every atom in our body has been formed in stellar cores! ...
1 Bruna Contro1,*, Rob Wittenmyer1,2,3, Jonti Horner2,3
1 Bruna Contro1,*, Rob Wittenmyer1,2,3, Jonti Horner2,3

... Over the course of the 60 Myr integrations described in the previous sections, the disk of debris orbiting HR 8799 undergoes drastic sculpting. The most readily apparent result of this sculpting is the rapid and complete clearing of debris from the outer region of the disk. Simply put, debris in thi ...
Lecture 1 & 2 Introduction and Origins – Chapter 1 & 2
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... Chronometers shown in brown. Accretion of planetary material was interrupted by energetic electromagnetic radiation (T Tauri phase) sweeping across the disk within a few Myr of the isolation of the solar nebula. Runaway growth of planetesimals produces Mars-sized planetary embryos, which, collision ...
a geocentric orrery
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... D) Sunspot activity virtually ceased between the years 1645 and 1715. E) The energy output from the Sun was at a minimum from the years 1843 through 1902 5) Stars like the Sun probably do not form iron cores during their evolution because … A) all of the iron is ejected when they become planetary ne ...
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... D) Sunspot activity virtually ceased between the years 1645 and 1715. E) The energy output from the Sun was at a minimum from the years 1843 through 1902 26) Stars like the Sun probably do not form iron cores during their evolution because … A) all of the iron is ejected when they become planetary n ...
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... B) Neutrinos were released from the Sun at record lows in 1987 C) Sunspot activity virtually ceased between the years 1645 and 1715. D) Gamma rays were released from the Sun at record lows in 1987 E) The energy output from the Sun was at a minimum from the years 1843 through 1902 27) Stars like the ...
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... B) Neutrinos were released from the Sun at record lows in 1987 C) Sunspot activity virtually ceased between the years 1645 and 1715. D) Gamma rays were released from the Sun at record lows in 1987 E) The energy output from the Sun was at a minimum from the years 1843 through 1902 27) Stars like the ...
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Unit 8 Chapter 28 Minor Bodies of the Solar System
Unit 8 Chapter 28 Minor Bodies of the Solar System

... More than a thousand asteroids have orbits that sometimes bring them very close to Earth. These asteroids have wide, elliptical orbits that bring them near Earth's orbit. Barringer Meteorite Crater, also known simply as Meteor Crater, in Arizona, has a diameter of more than 1 km which scientists bel ...
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... • How did we come to be? —The matter in our bodies came from the Big Bang, which produced hydrogen and helium. —All other elements were constructed from H and He in stars and then recycled into new star systems, including our solar system. • How can we know what the universe was like in the past? • ...
Jupiter`s ring
Jupiter`s ring

... object (e.g. a moon) can exist, as a body held together by its selfgravity, as it orbits a more massive body (e.g. its parent planet); closer in, and the smaller body is ripped to pieces by the tidal forces on it. ...
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Formation and evolution of the Solar System



The formation of the Solar System began 4.6 billion years ago with the gravitational collapse of a small part of a giant molecular cloud. Most of the collapsing mass collected in the center, forming the Sun, while the rest flattened into a protoplanetary disk out of which the planets, moons, asteroids, and other small Solar System bodies formed.This widely accepted model, known as the nebular hypothesis, was first developed in the 18th century by Emanuel Swedenborg, Immanuel Kant, and Pierre-Simon Laplace. Its subsequent development has interwoven a variety of scientific disciplines including astronomy, physics, geology, and planetary science. Since the dawn of the space age in the 1950s and the discovery of extrasolar planets in the 1990s, the model has been both challenged and refined to account for new observations.The Solar System has evolved considerably since its initial formation. Many moons have formed from circling discs of gas and dust around their parent planets, while other moons are thought to have formed independently and later been captured by their planets. Still others, such as the Moon, may be the result of giant collisions. Collisions between bodies have occurred continually up to the present day and have been central to the evolution of the Solar System. The positions of the planets often shifted due to gravitational interactions. This planetary migration is now thought to have been responsible for much of the Solar System's early evolution.In roughly 5 billion years, the Sun will cool and expand outward many times its current diameter (becoming a red giant), before casting off its outer layers as a planetary nebula and leaving behind a stellar remnant known as a white dwarf. In the far distant future, the gravity of passing stars will gradually reduce the Sun's retinue of planets. Some planets will be destroyed, others ejected into interstellar space. Ultimately, over the course of tens of billions of years, it is likely that the Sun will be left with none of the original bodies in orbit around it.
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