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Cosmology, galaxies, stars and the sun
Cosmology, galaxies, stars and the sun

... The black hole cannot be seen but can be observed by what it is “eating” as the stars simply disappear under its enormous gravity. ...
Figueira, Pont, Mordasini, Alibert, Georgy, Benz
Figueira, Pont, Mordasini, Alibert, Georgy, Benz

... arXiv:0904.2979v1 [astro-ph.EP] 20 Apr 2009 ...
An exoplanetary drama: a planet collapses on its star
An exoplanetary drama: a planet collapses on its star

... The bigger an exoplanet and/or the closer it is to its star, the greater the induced tidal effects. "We believe that if an exoplanet bigger than Jupiter were to venture too close to its star, it would disappear into it. This would explain why we detect so few enormous planets gravitating around thei ...
Towards a Classification System of Terrestrial Planets
Towards a Classification System of Terrestrial Planets

... dependent pattern of small refractory rocks, then large gas giants, then smaller ice giants, was taken as the standard model of planetary systems until the discovery of exoplanetary systems that did not conform to this pattern. Detected Exoplanets and their Implications for Extrasolar Terrestrial Pl ...
test - Scioly.org
test - Scioly.org

... E) HM Canqi B) Tycho's SNR C) SN 20l1fe 69) ) Which astronomical object on this year's list is unique because of its 'light echo"? ---o Researchers at the Space Tblescope Science Institute in Baltimore, Md. have idenffied light from the supernova that was reflected offof interstellar dust, delaying ...
supernova - Michigan State University
supernova - Michigan State University

Introduction This book will teach you all you need to know about the
Introduction This book will teach you all you need to know about the

... A black dwarf is when a white dwarf cools off over millions of years and it no longer emits light so it is simple now just a black floating object in space. We are now moving onto the life cycle of a high mass star. Just like the low mass star the high mass star starts out as a nebula. The nebula co ...
Stellar Evolution
Stellar Evolution

B - Department of Physics and Astronomy
B - Department of Physics and Astronomy

... D. They are burning helium into carbon and oxygen in a shell around their cores 4. In the process of helium shell fusion in low-mass stars near the end of their lives, the stars moves upward and to the right on the asymptotic giant branch of the Hertzsprung-Russell diagram. In this process, the star ...
Supplementary Information
Supplementary Information

... consistent with independent estimates that lie in the range 100 – 200 M yr-1, based on the H flux corrected for an extinction of about 1 mag and using the Kennicutt (6) conversion between H luminosity and star formation rate, based on the extinctioncorrected rest-frame UV continuum luminosity and ...
Sample Schedule 2012
Sample Schedule 2012

...  have no rings orbiting them. Outer planets formed further away from the sun in the protoplanetary disk where conditions were cooler. This cool environment meant that volatile icy compounds could remain solid. There is an abundance of these compared to the high melting point compounds (metals and s ...
Foundation 1 - Discovering Astronomy
Foundation 1 - Discovering Astronomy

... continues to contract and eventually becomes hot enough (100 million Kelvin) for helium to begin to fuse into carbon and oxygen – core helium fusion – 3 He  C + energy and C + He  O + energy ...
Recipes for ULX formation: necessary ingredients and garnishments
Recipes for ULX formation: necessary ingredients and garnishments

... provides the second ingredient, ensuring that a massive BH remnant is formed. The normalization of the high-mass X-ray binary luminosity function, and probably also the number of fainter ULXs with luminosities ∼ a few 1039 erg s−1 , is directly proportional to the SFR. However, the location of the u ...
NATS1311_112008_bw
NATS1311_112008_bw

... The Solar wind cleared the leftover gas, but not the leftover planetesimals. Those leftover rocky planetesimals which did not accrete into a planet, crash into inner planets, or get ejected from solar system are the present-day asteroids. Most inhabit the asteroid belt between Mars & Jupiter. Jupite ...
The Search for Worlds Like Our Own
The Search for Worlds Like Our Own

... however, that a complete study of a terrestrial exoplanet at interstellar distances would ultimately require complete spectral coverage. A step-wise approach to the problem would require development and deployment of the technologies sequentially. A key problem then would be which system is to be de ...
ph709-15-testrevision
ph709-15-testrevision

Slides
Slides

...  A. Small stars cool to form a white dwarf  B. Large stars undergo rapid gravitational collapse – Violent collapse creates implosion – High-pressure, high-temperature conditions force nuclei into neutron-rich mix – Secondary fusion process (rapid process) initiated – Violent rebound produces a sup ...
ppt
ppt

... EXISTED FOR BILLIONS OF YEAR Spiral galaxies reveal places in the universe where life can exist  The presence of large amounts of dust and gas indicates stellar processes have produced sufficient heavy elements to support the existence of planets.  These galaxies contain population I stars simila ...
“From Planetesimals to Brown Dwarfs: What is a Planet
“From Planetesimals to Brown Dwarfs: What is a Planet

α Cen A + iodine cell spectrum - Department of Physics and Astronomy
α Cen A + iodine cell spectrum - Department of Physics and Astronomy

... Results from planet formation simulations by Guedes et al. for α CenB. All simulations yield 1 to 4 Earth-mass planets of which 42% lie inside the star’s habitable zone (dashed lines). The planetary configuration of the solar system is shown for reference. Starting conditions: N lunar-mass bodies in ...
CHAPTER 14
CHAPTER 14

... (a) Type Ib, and Ic are caused by massive stars that have lost different proportions of their outer layers before exploding. (b) Type Ia result from white dwarfs. 6. A Type Ia supernova reaches maximum brightness in a few days, fades quickly for about a month, and then declines in brightness more gr ...
Galaxies
Galaxies

... • Extends 50,000 light years beyond the central bulge • Forms spiral arms that contain a lot of gas and dust • Population I stars are found in the spiral arms – these are young O and B main-sequence stars – they are often found in open clusters ...
exam1guide - Chemistry at Winthrop University
exam1guide - Chemistry at Winthrop University

... in old stars, star death for small and large stars, supernova and production of heavy elements, kilonovas, stars as agents of change in the universe. The Solar System: Earth’s Sun (Sol), hydrogen fusion, yellow star (surface temperature=6,000o C), Sol’s electromagnetic radiation, structure of Sol, r ...
Small images
Small images

... • A carbon-oxygen white dwarf accretes at a slow rate ...
File - Science Partnership
File - Science Partnership

... Satellite — any body in orbit around another larger body. At least 144 (depends on who’s counting) have been discovered in our solar system. Asteroid — a small planetary body composed mostly of rock or metal. Most asteroids are found in a belt between the orbits of Mars and Jupiter. Asteroids have d ...
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Nebular hypothesis

The nebular hypothesis is the most widely accepted model in the field of cosmogony to explain the formation and evolution of the Solar System. It suggests that the Solar System formed from nebulous material. The theory was developed by Immanuel Kant and published in his Universal Natural History and Theory of the Heaven. Originally applied to our own Solar System, this process of planetary system formation is now thought to be at work throughout the universe. The widely accepted modern variant of the nebular hypothesis is the solar nebular disk model (SNDM) or simply solar nebular model. This nebular hypothesis offered explanations for a variety of properties of the Solar System, including the nearly circular and coplanar orbits of the planets, and their motion in the same direction as the Sun's rotation. Some elements of the nebular hypothesis are echoed in modern theories of planetary formation, but most elements have been superseded.According to the nebular hypothesis, stars form in massive and dense clouds of molecular hydrogen—giant molecular clouds (GMC). These clouds are gravitationally unstable, and matter coalesces within them to smaller denser clumps, which then rotate, collapse, and form stars. Star formation is a complex process, which always produces a gaseous protoplanetary disk around the young star. This may give birth to planets in certain circumstances, which are not well known. Thus the formation of planetary systems is thought to be a natural result of star formation. A Sun-like star usually takes approximately 1 million years to form, with the protoplanetary disk evolving into a planetary system over the next 10-100 million years.The protoplanetary disk is an accretion disk that feeds the central star. Initially very hot, the disk later cools in what is known as the T tauri star stage; here, formation of small dust grains made of rocks and ice is possible. The grains eventually may coagulate into kilometer-sized planetesimals. If the disk is massive enough, the runaway accretions begin, resulting in the rapid—100,000 to 300,000 years—formation of Moon- to Mars-sized planetary embryos. Near the star, the planetary embryos go through a stage of violent mergers, producing a few terrestrial planets. The last stage takes approximately 100 million to a billion years.The formation of giant planets is a more complicated process. It is thought to occur beyond the so-called frost line, where planetary embryos mainly are made of various types of ice. As a result, they are several times more massive than in the inner part of the protoplanetary disk. What follows after the embryo formation is not completely clear. Some embryos appear to continue to grow and eventually reach 5–10 Earth masses—the threshold value, which is necessary to begin accretion of the hydrogen–helium gas from the disk. The accumulation of gas by the core is initially a slow process, which continues for several million years, but after the forming protoplanet reaches about 30 Earth masses (M⊕) it accelerates and proceeds in a runaway manner. Jupiter- and Saturn-like planets are thought to accumulate the bulk of their mass during only 10,000 years. The accretion stops when the gas is exhausted. The formed planets can migrate over long distances during or after their formation. Ice giants such as Uranus and Neptune are thought to be failed cores, which formed too late when the disk had almost disappeared.
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