PowerPoint Presentation - ASTR498E High energy
... The mass of the star M The fraction of the stellar mass that can participate in the fusion reactions f ...
... The mass of the star M The fraction of the stellar mass that can participate in the fusion reactions f ...
CC Lin
... Toomre (1964) analyzed the stability of gas (and stars) in disks to local gravitational instabilities. Simply, gravitational collapse occurs if Q < 1. For Gas Q = κ CS / (π G Σ) For Stars Q = κ σR / (3.36 G Σ) where Σ is again the local surface mass density, κ is the local epicyclic frequency, σR is ...
... Toomre (1964) analyzed the stability of gas (and stars) in disks to local gravitational instabilities. Simply, gravitational collapse occurs if Q < 1. For Gas Q = κ CS / (π G Σ) For Stars Q = κ σR / (3.36 G Σ) where Σ is again the local surface mass density, κ is the local epicyclic frequency, σR is ...
Skymapper and Kepler K2: Finding the Origin of Hot Gas Giants
... Planet formation with migraiton where one set of initial conditions gives the solar system and another gives a solitary hot Jupiter. ...
... Planet formation with migraiton where one set of initial conditions gives the solar system and another gives a solitary hot Jupiter. ...
Characteristics of Stars
... • The scientific name for the twinkling of stars is stellar scintillation • Stars twinkle when we see them from the Earth's surface because we are viewing them through thick layers of turbulent (moving) air in the Earth's atmosphere. ...
... • The scientific name for the twinkling of stars is stellar scintillation • Stars twinkle when we see them from the Earth's surface because we are viewing them through thick layers of turbulent (moving) air in the Earth's atmosphere. ...
ES High mass star life cycle plus black holes
... What is the life cycle of a low mass star (5 stages)? What is the life cycle of a high mass star? What is the heaviest element forms in the center of a high mass star? Why is supernova crucial to our existence? Where is calcium formed in the life a high mass star? What is a supernova? What are the 2 ...
... What is the life cycle of a low mass star (5 stages)? What is the life cycle of a high mass star? What is the heaviest element forms in the center of a high mass star? Why is supernova crucial to our existence? Where is calcium formed in the life a high mass star? What is a supernova? What are the 2 ...
Study Guide: Use your notes and handouts to
... 11. What are the three types of galaxies? 12. What is the name of our galaxy? What type of galaxy is it? ...
... 11. What are the three types of galaxies? 12. What is the name of our galaxy? What type of galaxy is it? ...
Chapter 15 Stars, Galaxies
... but still high-mass stars become neutron stars. f. They all start out as a part of nebulas that contract to form protostars. g. Low-mass and medium-mass stars turn into red giants as they use up their fuel. They later form planetary nebulas and white dwarfs. High-mass stars turn into supergiants as ...
... but still high-mass stars become neutron stars. f. They all start out as a part of nebulas that contract to form protostars. g. Low-mass and medium-mass stars turn into red giants as they use up their fuel. They later form planetary nebulas and white dwarfs. High-mass stars turn into supergiants as ...
here
... total radiative fluxes going through their atmospheres. In the ionised atmosphere, the dominating opacity is Thomson scattering on free electrons. As the gas absorbs the radiative flux it also absorbs the outward directed momentum of the photons which leads to an additional outward force – radiation ...
... total radiative fluxes going through their atmospheres. In the ionised atmosphere, the dominating opacity is Thomson scattering on free electrons. As the gas absorbs the radiative flux it also absorbs the outward directed momentum of the photons which leads to an additional outward force – radiation ...
Life Cycle of Star Flipbook
... 6. What is going to happen to our Sun’s magnitude and temperature when it goes to its next stage? 7. What is the final stage of our Sun’s life? 8. What will happen to our Sun’s magnitude and temperature when it goes to its final stage? 9. What determines which star will go supernova? 10. What two fo ...
... 6. What is going to happen to our Sun’s magnitude and temperature when it goes to its next stage? 7. What is the final stage of our Sun’s life? 8. What will happen to our Sun’s magnitude and temperature when it goes to its final stage? 9. What determines which star will go supernova? 10. What two fo ...
- MrKowalik.com
... 4. If Earth and another celestial object were coming closer together, the electromagnetic waves are bunched together resulting in _____________________________________ 5. If Earth and another celestial object were moving apart, the electromagnetic waves are spread out causing a _____________________ ...
... 4. If Earth and another celestial object were coming closer together, the electromagnetic waves are bunched together resulting in _____________________________________ 5. If Earth and another celestial object were moving apart, the electromagnetic waves are spread out causing a _____________________ ...
Name: ____________________________ Date: _____________ Per. _________ Stars Study Guide (Ch. 21)
... 13. What is a graph that shows the relationship between absolute brightness and surface temperature of a star? __________________ ...
... 13. What is a graph that shows the relationship between absolute brightness and surface temperature of a star? __________________ ...
White Dwarf Stars
... • These objects act as cosmic clocks and are useful for probing the dynamics of stars. ...
... • These objects act as cosmic clocks and are useful for probing the dynamics of stars. ...
The Life Cycle of Stars
... When the hydrogen supply in the core begins to run out, and the star is no longer generating heat by nuclear fusion, the core becomes unstable and contracts. The outer shell of the star, which is still mostly hydrogen, starts to expand. As it expands, it cools and glows red. The star has now reached ...
... When the hydrogen supply in the core begins to run out, and the star is no longer generating heat by nuclear fusion, the core becomes unstable and contracts. The outer shell of the star, which is still mostly hydrogen, starts to expand. As it expands, it cools and glows red. The star has now reached ...
Stars and Galaxies
... 80. A _______________ is a large group of stars, gas, and dust held together by gravity. 81. Our galaxy is the _______________________ Galaxy and contains about 200 billion stars. 82. Galaxies are grouped together in clusters; our cluster is the ____________________. 83. There are 3 types of galaxie ...
... 80. A _______________ is a large group of stars, gas, and dust held together by gravity. 81. Our galaxy is the _______________________ Galaxy and contains about 200 billion stars. 82. Galaxies are grouped together in clusters; our cluster is the ____________________. 83. There are 3 types of galaxie ...
02-Voyage to the Planets
... The gases were too hot to condense due to the close location to the sun and blown away from the sun’s solar wind, leaving only the solid chunks behind. As they continued to circulate around the sun, they joined together forming larger chunks. This caused a strong gravity around them and pulled all t ...
... The gases were too hot to condense due to the close location to the sun and blown away from the sun’s solar wind, leaving only the solid chunks behind. As they continued to circulate around the sun, they joined together forming larger chunks. This caused a strong gravity around them and pulled all t ...
Chapter 10- Stars, Galaxies and the Universe
... 37. Telescopes work by collecting and focusing different forms of ____________________ radiation. 38. Astronomers can determine a star’s chemical composition by using a(n) _________________________ to observe the wavelengths of light the star emits. 39. The most massive stars collapse to form ______ ...
... 37. Telescopes work by collecting and focusing different forms of ____________________ radiation. 38. Astronomers can determine a star’s chemical composition by using a(n) _________________________ to observe the wavelengths of light the star emits. 39. The most massive stars collapse to form ______ ...
Stars - Madison County Schools
... If the remaining mass of the star is more than about three times that of the Sun, it will collapse so completely that it will literally disappear from the universe. What is left behind is an intense region of gravity called a black hole ...
... If the remaining mass of the star is more than about three times that of the Sun, it will collapse so completely that it will literally disappear from the universe. What is left behind is an intense region of gravity called a black hole ...
ASTR2050 Spring 2005 • In this class we will cover: Brief review
... Evolution off the Main Sequence First: “Low mass” stars (M < 5M!) Hydrogen in core is used up. Temperature in core is not high enough to burn helium. Hydrogen burns in “shell”. Helium core is “degenerate”. H burning He core is very ...
... Evolution off the Main Sequence First: “Low mass” stars (M < 5M!) Hydrogen in core is used up. Temperature in core is not high enough to burn helium. Hydrogen burns in “shell”. Helium core is “degenerate”. H burning He core is very ...
Astronomy Campus Assessment
... A. The star is composed of Li, H, He, and Na which means that the star is older than our star, the sun. B. The star is only composed of Hydrogen so it would be much younger than our star, the sun. C. The star is composed of H, He, and Lithium meaning it is a fairly young star that is starting to fus ...
... A. The star is composed of Li, H, He, and Na which means that the star is older than our star, the sun. B. The star is only composed of Hydrogen so it would be much younger than our star, the sun. C. The star is composed of H, He, and Lithium meaning it is a fairly young star that is starting to fus ...
dtu7ech13 - Fort Thomas Independent Schools
... dwarf in a binary star system. What are the origins of the carbon, silicon, oxygen, iron, uranium, and other heavy elements on Earth? These elements are created during stellar evolution, by supernovae, and by colliding neutron stars. What are cosmic rays? Cosmic rays are high-speed particles (mostly ...
... dwarf in a binary star system. What are the origins of the carbon, silicon, oxygen, iron, uranium, and other heavy elements on Earth? These elements are created during stellar evolution, by supernovae, and by colliding neutron stars. What are cosmic rays? Cosmic rays are high-speed particles (mostly ...
Stars Powerpoint
... • The matter inside the star will be compressed so tightly that its atoms are compacted into a dense shell of neutrons. If the remaining mass of the star is more than about three times that of the Sun, it will collapse so completely that it will literally disappear from the universe. What is left be ...
... • The matter inside the star will be compressed so tightly that its atoms are compacted into a dense shell of neutrons. If the remaining mass of the star is more than about three times that of the Sun, it will collapse so completely that it will literally disappear from the universe. What is left be ...
supernova!
... settle to the centre. It is merely a consequence of the fact that the progressively heavier elements are created near the centre, where the temperature progressively becomes high enough to do so! The outer envelope of the star is still the pristine material from which it was made (mainly Hydrogen an ...
... settle to the centre. It is merely a consequence of the fact that the progressively heavier elements are created near the centre, where the temperature progressively becomes high enough to do so! The outer envelope of the star is still the pristine material from which it was made (mainly Hydrogen an ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.