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Stars Powerpoint
Stars Powerpoint

... Life span of a star depends on its size. ...
PH709-assn-answers
PH709-assn-answers

... Planetesimals form as dust/grains separate/diffuse from the gas, forming a denser dust disc near the mid-plane. Inelastic ollisions between grains are more common in this disc and sticking/coalescence occurs. Turbulence stirs up the gas increasing the collision rate OR Gravity becomes more important ...
presentation source
presentation source

... “[Owing to nuclear physicists good proposal of a ‘big bang’ origin of the Universe some 3 million years ago…] We are indeed forced to conclude that the present variety of stars in the sky is the result of the original method of star formation rather than of any evolutionary process.” --Lyman Sptitze ...
Astro 27 Solar System Formation and ExoPlanets Slide Show
Astro 27 Solar System Formation and ExoPlanets Slide Show

... “Slow” Core Accretion goes faster when gravity gets strong enough, but… • Once the core grows past ~0.5-1 mile across, gravity becomes significant and accelerates the process. • Growth rate goes as radius to the 4th power (for constant density). • So, those cores which get to the self-gravity point ...
I Cloudy with a Chance of Making a star is no easy thing
I Cloudy with a Chance of Making a star is no easy thing

... Consequently, those of us who seek to observe star formation face a fundamental problem: stars cloak their own birth. The material that goes into creating a star is thick and dark; it needs to become dense enough to initiate nuclear fusion but has not done so yet. Astronomers can see how this proces ...
LETTERS A giant planet orbiting the ‘extreme horizontal
LETTERS A giant planet orbiting the ‘extreme horizontal

Forming disk galaxies in magneto-hydro
Forming disk galaxies in magneto-hydro

... SuperMUC has played a decisive role in making the present simulations possible. Within our project, we are currently working on substantially scaling up the numerical resolution and dynamic range achieved in our simulations of the formation of Milky Way-sized galaxies, thereby allowing a treatment o ...
Presentation
Presentation

1. How old is our sun now? How does its present luminosity
1. How old is our sun now? How does its present luminosity

Birth and Life of a Star
Birth and Life of a Star

... Many white dwarfs are about the same size as the Earth, and about 100 times smaller than the Sun. They may weigh the same as the sun, which would make them very dense. The heavier the white dwarf is, then the smaller its size will be. A star like our Sun will become a white dwarf when it has run out ...
November 2013 - Pomona Valley Amateur Astronomers
November 2013 - Pomona Valley Amateur Astronomers

... a concept is consistent with all observations it can be considered reasonable. If it can hold up under intense scrutiny and many attempts to falsify it, it may be considered reliable. The concept presented here is just beginning to be scrutinized. As of now, consider it speculation but generally acc ...
Birth and Life of a Star
Birth and Life of a Star

... Many white dwarfs are about the same size as the Earth, and about 100 times smaller than the Sun. They may weigh the same as the sun, which would make them very dense. The heavier the white dwarf is, then the smaller its size will be. A star like our Sun will become a white dwarf when it has run out ...
Methods for the detection of exoplanets
Methods for the detection of exoplanets

... Definition: region around a star where the temperature on the surface of an eventual planet or moon can afford the ...
Discovery of Extrasolar Planets - WSU Astronomy.
Discovery of Extrasolar Planets - WSU Astronomy.

Powerpoint file
Powerpoint file

IOSR Journal of Applied Physics (IOSR-JAP) ISSN: 2278-4861.
IOSR Journal of Applied Physics (IOSR-JAP) ISSN: 2278-4861.

... material was drawn towards the centre of the nebula. This made gravity stronger, making condensation faster. This theory was justified by a well know experiment in which astronomers used a transparent glass tube of water with dissolved salt crystals (mingled in spaces). It was observed that salt cry ...
How are stars formed
How are stars formed

... Giant molecular clouds: • 1,000’s pc across • 1,000’s Msun ...
Today`s Powerpoint
Today`s Powerpoint

... and computer simulations show this situation can be maintained for a long time. ...
To know that planets etc. move in elliptical orbits around the Sun.
To know that planets etc. move in elliptical orbits around the Sun.

Document
Document

... • Must not have Ca II H&K emission variations with the planet period ...
THE DEFINITION OF PLANET: A DYNAMICIST`S POINT OF VIEW
THE DEFINITION OF PLANET: A DYNAMICIST`S POINT OF VIEW

Study Guide for the 4TH Astronomy Exam
Study Guide for the 4TH Astronomy Exam

Star Formation - Leslie Looney
Star Formation - Leslie Looney

... giant. •! Elements blown from across galaxy by supernovae. ...
Planets Beyond the Solar System
Planets Beyond the Solar System

... mph), mostly due to Jupiter. • The size of this path is about 0.001 arcsec (less than a millionth of a degree) as seen from 10 parsecs (33 light years) away. ...
eneb_form
eneb_form

... star has a huge volume. That means the atoms are not close to each other near the surface. They have virtually no effect on the given energy levels. • In a giant star (luminosity class III) the star has a large radius but not as large as the supergiant. The atoms near the surface interact more with ...
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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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