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Galaxies - Stockton University
Galaxies - Stockton University

... supermassive black-holes. The various types reflect differences in viewing angle and jet activity. The evidence that suggests this model can be summarized by:  high-velocity gas ( 10,000 Km/s) and relativistic jets imply a deep potential.  the tiny size of the energy generation region is impossibl ...
UK Exoplanet community meeting 2017
UK Exoplanet community meeting 2017

The Hydrogen 21-cm Emission Line
The Hydrogen 21-cm Emission Line

... always want to be in the lowest energy state possible, the electron will eventually flip to the anti-parallel spin direction if it were in the parallel spin direction. The energy difference is very small, so a hydrogen atom can wait on average a few million years before it undergoes this transition. ...
chapter18StarDeath
chapter18StarDeath

... electrons must move at nearly the speed of light • Because nothing can move faster than light, a white dwarf cannot be more massive than 1.4MSun, the white dwarf limit (or Chandrasekhar limit) ...
Constraints on the Birth Aggregate of the Solar System
Constraints on the Birth Aggregate of the Solar System

introduction to astronomy
introduction to astronomy

ES 104 Midterm Exam Study Guide 1
ES 104 Midterm Exam Study Guide 1

... compositional differences between these 2 categories of planets – look over the table that you completed for the first homework activity. Also know why the Jovian planets have thicker atmospheres than the terrestrial planets and why some bodies such as Earth’s moon lack an atmosphere. Know how the o ...
Chapter 18 The Bizarre Stellar Graveyard What is a white dwarf
Chapter 18 The Bizarre Stellar Graveyard What is a white dwarf

... • Quantum mechanics says that electrons must move faster as they are squeezed into a very small space • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light • Because nothing can move faster than light, a white dwarf cannot be more massive than 1.4MSun, th ...
Lecture12
Lecture12

allowed planetary orbits
allowed planetary orbits

Star Birth - Sierra College Astronomy Home Page
Star Birth - Sierra College Astronomy Home Page

Worked Problem In a spherical galaxy, the density of matter varies
Worked Problem In a spherical galaxy, the density of matter varies

... and Tremaine for details). For a Kepler orbit, for instance, this ratio Tθ /Tr = 1, and the planet, travelling around the Sun, goes over and over the same elliptical orbit as a result. The ratio of the two periods Tθ /Tr is in general not a rational number, and so the typical orbit of a star in a sp ...
On the Nature of the Dust in the Debris Disk Around HD69830
On the Nature of the Dust in the Debris Disk Around HD69830

UK Exoplanet community meeting 2017
UK Exoplanet community meeting 2017

... Earth is the best studied planet we know. A century’s work on terrestrial samples has interrogated 90% of its history, and revealed the physics of processes from the formation of the core to the rise of atmospheric oxygen. This detailed understanding can benefit our perspective of exo-planetary syst ...
Star Clusters and their stars
Star Clusters and their stars

... They typically have 105 – 106 stars. They are spherically distributed around the center of our Galaxy. They tend to concentrate towards the center of the Galaxy, with many in the constellations Sagittarius, Scorpio and Ophiunchus It was by studying the distribution of globular clusters that astronom ...
Star_Clusters
Star_Clusters

... They typically have 105 – 106 stars. They are spherically distributed around the center of our Galaxy. They tend to concentrate towards the center of the Galaxy, with many in the constellations Sagittarius, Scorpio and Ophiunchus It was by studying the distribution of globular clusters that astronom ...
Life as a Low Mass Red Giant
Life as a Low Mass Red Giant

... – As core temperature rises, fusion rate rises, so luminosity increases somewhat. – This is very important for understanding origin of life on earth. Sun's luminosity has grown at least 50% since birth of Earth. Planetary scientists having difficult time understanding why Earth was not in permanent ...
Post Main Sequence Evolution Since a star`s luminosity on the main
Post Main Sequence Evolution Since a star`s luminosity on the main

... The Hertzsprung Gap and the Subgiant Phase • When the Schönberg-Chandrasekhar limit is reached, the star must change its structure. First, core contraction begins to occur on the Kelvin-Helmholtz timescale, and the rapid increase in core density causes an increase in the temperatures and densities ...
Chapter14(4-7-11)
Chapter14(4-7-11)

... must have formed early in the galaxy’s history, before the gas settled into a disk. ...
Chapter 11
Chapter 11

... more and somewhat less massive than the Sun. The shape of the paths is similar, but they wind up in different places on the main sequence. ...
Stellar Evolution of low and intermediate mass stars
Stellar Evolution of low and intermediate mass stars

... A convection zone appears and dredges up processes material to the envelope -- C and O rich stars – reduces the mass of the core ...
Full Programme and Abstracts - UK Exoplanet community meeting
Full Programme and Abstracts - UK Exoplanet community meeting

... Earth is the best studied planet we know. A century’s work on terrestrial samples has interrogated 90% of its history, and revealed the physics of processes from the formation of the core to the rise of atmospheric oxygen. This detailed understanding can benefit our perspective of exo-planetary syst ...
The Mt John University Observatory search for Earth
The Mt John University Observatory search for Earth

... detected after 3 years of observations, if the noise distribution is sufficiently close to Gaussian (see Fig. 5 in their paper). They used a noise level of 3 m s− 1 and nearly 105 synthetic RV points. Thebault et al. (2008, 2009), however, argue that these Earth-like planets might not have formed aro ...
Document
Document

... • Over 4000 K giants were observed with precise radial velocity measurements to assure that they were constant ...
Hiroyuki_Hirashita
Hiroyuki_Hirashita

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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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