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Neutron stars, pulsars
Neutron stars, pulsars

Publication - Centre for Star and Planet Formation
Publication - Centre for Star and Planet Formation

Slide 1
Slide 1

Astrobiology: The Search for Extraterrestrial Life
Astrobiology: The Search for Extraterrestrial Life

Our galaxy, the Milky Way, has about 3 billion solar masses of HI
Our galaxy, the Milky Way, has about 3 billion solar masses of HI

... established as constant for all objects of that class, then the luminosity of one of these standard candles can be safely assumed when it is seen in another location. 12. How can you use the period-luminosity relation to find distances? The luminosity of a Cepheid is found to correlate very closely ...
Alien Planets - Eccles Science
Alien Planets - Eccles Science

... galaxy could actually be teeming with planets of all sizes and types. Scientists call planets orbiting stars other than our sun extrasolar planets, or exoplanets for short. ...
Life on Earth Came From Other Planets
Life on Earth Came From Other Planets

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Day_29

Astronomy Astrophysics The HARPS search for southern extra-solar planets &
Astronomy Astrophysics The HARPS search for southern extra-solar planets &

... present at a longer period, probably caused by a 65-M⊕ object. Moreover, another body with a minimum mass as low as 1.4 M⊕ may be present at 0.02 AU from the star. This is the most populated exoplanetary system known to date. The planets are in a dense but still well separated configuration, with si ...
Name Date Life and Death of a Star 2015 1. In the main
Name Date Life and Death of a Star 2015 1. In the main

... In the main-sequence, the core is slowly shrinking because A. the mass of the star is slowly increasing B. hydrogen fusing to helium makes the core more dense C. carbon and iron are accumulating in the core In a timeline that shows the sequence of events that occurs during the formation of a star, w ...
Mark Rubin
Mark Rubin

... • As a result of the rapid pollution within high-density regions due to the first SN/pair instability SN, local metallicity is quickly boosted above the critical metallicity for the transition. • For this reason, pop III stars dominate only during the very first stages of structure formation, with a ...
tremaine_lecture_1
tremaine_lecture_1

... “an intelligence knowing, at a given instant of time, all forces acting in nature, as well as the momentary positions of all things of which the universe consists, would be able to comprehend the motions of the largest bodies of the world and those of the smallest atoms in one single formula, provid ...
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... Instead, the mass of the iron core increases as nuclear fusion of lighter elements takes place, and its temperature increases. Eventually the temperature becomes so high that the iron begins to break down (disintegrate) into smaller units like ...
11-Massive Stars
11-Massive Stars

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The First Stars - Amazon Web Services

... than white dwarfs. So much energy is released in this final collapse that a huge explosion blows off the outer layers of the star. This is a supernova explosion. The light released in this immense explosion heralding the death throes of a massive star is about that of the luminosity of an entire gal ...
Ay123 Homework 1 Solutions
Ay123 Homework 1 Solutions

The Fate of the X-ray Emitting Gas in the Early
The Fate of the X-ray Emitting Gas in the Early

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1 The Solar System - e
1 The Solar System - e

... sky? There is evidence that man had shown an interest in knowing about them since ancient times. At present man can explore more than what is visible to the naked eye, as scientists have invented modern equipment to observe the sky. It has been discovered that there are eight planets, shapeless piec ...
Stellar Characteristics and Evolution
Stellar Characteristics and Evolution

The Stellar Cycle
The Stellar Cycle

... WD has a size slightly less than that of the earth. It is so dense, one teaspoon weights 15 tons! WD from an isolated star will simply cool, temperature dropping until it is no ...
Pulsars - Chabot College
Pulsars - Chabot College

... Not fusing: Generates no new energy ...
The Discovery of Planets beyond the Solar System
The Discovery of Planets beyond the Solar System

... With a pair of exceptions, all discovered planets move very close to their stars. . This is due to the Doppler effect used in most discoveries: the star motion is larger when the planet going around is closer ...
Planets orbiting stars more massive than the Sun
Planets orbiting stars more massive than the Sun

... from these difficulties. The only challenges of transit surveys is that the planetary transit are shallower than for solar-like stars, and that many IMSs oscillate. Groundbased transit surveys have already discovered planets of IMSs, for example HD15082b (Collier Cameron et al. 2010). However, detec ...
Sirius Astronomer - Orange County Astronomers
Sirius Astronomer - Orange County Astronomers

PPT Format of Slides
PPT Format of Slides

... Conservation of angular momentum says that product of radius and rotation rate must be constant ...
< 1 ... 48 49 50 51 52 53 54 55 56 ... 158 >

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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