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Hungry Young Stars: A New Explanation for the FU Ori Outbursts
Hungry Young Stars: A New Explanation for the FU Ori Outbursts

AST101 Lecture 13 The Lives of the Stars
AST101 Lecture 13 The Lives of the Stars

... Evolution similar to Sun ...
AST101_lect_13
AST101_lect_13

... Evolution similar to Sun ...
RIPL Radio Interferometric Planet Search
RIPL Radio Interferometric Planet Search

... with RV method Planet fraction of low mass stars poorly determined Detects planets that can be studied with extreme AO Ties radio and optical astrometric reference frame ...
Extraterrestrial Life
Extraterrestrial Life

ref H-R Spectral types
ref H-R Spectral types

... • how H-R diagrams were developed, and • why the temperature scale goes “the wrong way”. In the next Activity, we will study a real example by continuing the story of how a huge, cool molecular cloud can become a blazing star, and we’ll use H-R diagrams to help us. ...
The Hertzsprung-Russell Diagram
The Hertzsprung-Russell Diagram

... Equal Radius Lines In general the hotter the star is the brighter it will be. Thus you would expect stars of the same size but different temperatures to form a diagonal line called an equal radius line. Equal Radius lines can be added to an H-R diagram ...
Star - AUSD Blogs
Star - AUSD Blogs

... and geophysics out of proportion to our numbers. Will my report on the Phoenix Nebula end our thousand years of history? It will end, I fear, much more than that. I do not know who gave the nebula its name, which seems to me a very bad one. If it contains a prophecy, it is one that cannot be verifie ...
Astronomy 100—Exam 2
Astronomy 100—Exam 2

... E. Iron 11. A white dwarf is supported against collapse by A. thermal pressure. C. electron degeneracy pressure. B. gravity. D. neutron degeneracy pressure. ...
word document - FacStaff Home Page for CBU
word document - FacStaff Home Page for CBU

... STUDY GUIDE FOR PART 4 ...
DYNAMICAL STABILITY OF SPHERICAL STARS
DYNAMICAL STABILITY OF SPHERICAL STARS

... by the same factor: r = r0 (1 + x), where x is a very small number that may vary with time, but not in space. Mass conservation expressed with eq. (d.1b) demands that ρ = ρ0 (1 − 3x). We shall assume that the change is adiabatic, with a constant adiabatic exponent γ : ...
TF_final3 - Arecibo Observatory
TF_final3 - Arecibo Observatory

... velocity width (W) of the lines is proportional to its luminosity (L) following an equation, L ∝ In a sample of 33 LIRGs the neutral hydrogen emission line width was measured. The luminosities of these galaxies from literature were found and a study was made of whether the Tully-Fisher law is mainta ...
William Paterson University Department of Physics General
William Paterson University Department of Physics General

... Every student at William Paterson has a student university e-mail address. Your university email address is attached to Blackboard, and that is the one that will be used to contact you about assignments and other matters related to the course. You should check it daily. AOL users: if you have AOL, y ...
the lives of stars
the lives of stars

... star, has been a main sequence star for about 5 billion years. It will continue to shine without changing for about 5 billion more years. Really large stars burn through their supply of hydrogen very quickly, so they ‘live fast and die young’! These very large stars may only be on the main sequence ...
Properties of Stars in general
Properties of Stars in general

... • But its mass (= fuel supply) is only ~ 17 times that of our Sun. • So its life cannot be so long: ~ 17/45,000 that of our Sun ************* ...
Exercise 8
Exercise 8

... such a way that the apparent size of a galaxy is related to its distance from Earth. This is method similar to the main-sequence fitting we did in an earlier exercise for star clusters. Figure 8.1 shows the images and visible spectra of five elliptical galaxies. The spectrum of each galaxy is shown ...
Test 2, Nov. 17, 2015 - Physics@Brock
Test 2, Nov. 17, 2015 - Physics@Brock

... 2. According to Kepler’s second law, a planet moves fastest when it is (a) closest to the Sun. (b) at the greatest distance from the Sun. (c) [The speed of the planet does not depend on its distance from the Sun.] 3. It is possible to determine the mass of a planet from the orbital data (the period ...
Stellar Evolution
Stellar Evolution

A stars
A stars

... Around Sirius (Spectral type A1: 26 times more luminous than the Sun), an Earth-sized planet would have to orbit at about the distance of Jupiter from the star. Around Epsilon Indi (Spectral type K5: about one-tenth the Sun's luminosity), an Earth-sized planet would have to orbit at about the distan ...
File
File

... The Solar System formed 4.568 billion years ago from the gravitational collapse of a region within a large molecular cloud. This initial cloud was likely several light-years across and probably birthed several stars. As is typical of molecular clouds, this one consisted mostly of hydrogen, with some ...
Lecture 9/10 Stellar evolution Ulf Torkelsson 1 Main sequence stars
Lecture 9/10 Stellar evolution Ulf Torkelsson 1 Main sequence stars

... flash as a dimming of the star. Presumably these event are also related to significant mass loss events in the evolution of the star. Eventually the surface layers of the star are expelled, and a degenerate carbon-oxygen core remains at the centre of the star. This core becomes a white dwarf. On the ...
Interstellar Cloud
Interstellar Cloud

The Hot-plate Model of a Star Model of Stars—5 Oct •
The Hot-plate Model of a Star Model of Stars—5 Oct •

... Luminosity & Flux of Stars ...
Neutron Stars
Neutron Stars

... If initial star mass < 8 MSun or so. (and remember: Maximum WD mass is 1.4 MSun , radius is about that of the Earth) ...
Teacher Guide - Astronomy Outreach at UT Austin
Teacher Guide - Astronomy Outreach at UT Austin

... which these stars differ as they progress through their various stages of life and death. A star, like our Sun, is an enormous and complex system. In order to model and understand their properties and how they change with time, astronomers and astrophysicists apply the basic ideas in physics to math ...
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Future of an expanding universe

Observations suggest that the expansion of the universe will continue forever. If so, the universe will cool as it expands, eventually becoming too cold to sustain life. For this reason, this future scenario is popularly called the Big Freeze.If dark energy—represented by the cosmological constant, a constant energy density filling space homogeneously, or scalar fields, such as quintessence or moduli, dynamic quantities whose energy density can vary in time and space—accelerates the expansion of the universe, then the space between clusters of galaxies will grow at an increasing rate. Redshift will stretch ancient, incoming photons (even gamma rays) to undetectably long wavelengths and low energies. Stars are expected to form normally for 1012 to 1014 (1–100 trillion) years, but eventually the supply of gas needed for star formation will be exhausted. And as existing stars run out of fuel and cease to shine, the universe will slowly and inexorably grow darker, one star at a time. According to theories that predict proton decay, the stellar remnants left behind will disappear, leaving behind only black holes, which themselves eventually disappear as they emit Hawking radiation. Ultimately, if the universe reaches a state in which the temperature approaches a uniform value, no further work will be possible, resulting in a final heat death of the universe.
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