Galaxies - Center for Astrostatistics
... Tauri stars, open clusters, supernova remnants and X-ray binaries. The maps below show the disk at infrared, 21-cm hydrogen, CO molecules, and visible light. There is an intricate relationship between the interstellar medium and stars in the Galactic disk. Star are born in cold molecular clouds., or ...
... Tauri stars, open clusters, supernova remnants and X-ray binaries. The maps below show the disk at infrared, 21-cm hydrogen, CO molecules, and visible light. There is an intricate relationship between the interstellar medium and stars in the Galactic disk. Star are born in cold molecular clouds., or ...
Section9 - University of Chicago
... by observing radio sources. In this case the galaxies found are the hosts of active radio emitting jets – distant analogs of objects like Centaurus A Cygnus A and M87 in the nearby universe. ...
... by observing radio sources. In this case the galaxies found are the hosts of active radio emitting jets – distant analogs of objects like Centaurus A Cygnus A and M87 in the nearby universe. ...
Return both exam and scantron sheet when you
... (d) highly elliptical. 42. If you lived in a galaxy far away from the Local Group, your redshift measurements would show that galaxies move (a) away from you in the same way as observed from the Milky Way. (b) away from the Milky Way but toward you. (c) toward you out to the distance of the Milky wa ...
... (d) highly elliptical. 42. If you lived in a galaxy far away from the Local Group, your redshift measurements would show that galaxies move (a) away from you in the same way as observed from the Milky Way. (b) away from the Milky Way but toward you. (c) toward you out to the distance of the Milky wa ...
review
... Our Milky Way galaxy is disk shaped with a central bulge, and a low density spherical halo. Disk and halo are about 30kpc across. The central bulge is a few kpc across. There are about 1011 (100 billion) solar masses in the galaxy, so about that many stars. Measuring distances in the galaxy uses var ...
... Our Milky Way galaxy is disk shaped with a central bulge, and a low density spherical halo. Disk and halo are about 30kpc across. The central bulge is a few kpc across. There are about 1011 (100 billion) solar masses in the galaxy, so about that many stars. Measuring distances in the galaxy uses var ...
key - Scioly.org
... a) 321.5 seconds (5.4 minutes); It is the shortest orbital period of any binary system discovered. b) Xray c) The observation of such systems pushes to the limit of current technology because they are so dim that only the largest telescopes can sense them. d) Approximately one ton (~.5 solar masses ...
... a) 321.5 seconds (5.4 minutes); It is the shortest orbital period of any binary system discovered. b) Xray c) The observation of such systems pushes to the limit of current technology because they are so dim that only the largest telescopes can sense them. d) Approximately one ton (~.5 solar masses ...
Introduction to Galaxies and Cosmology Exercises 2
... at 10% of its Eddinton luminosity? c) What is the Schwarzschild radius of the black hole? 9. (Challenging) A quasar emits two radiating clouds in our general direction at 13/14 the speed of light. They are first observed when they appear to have been first produced at the central powerhouse, and are ...
... at 10% of its Eddinton luminosity? c) What is the Schwarzschild radius of the black hole? 9. (Challenging) A quasar emits two radiating clouds in our general direction at 13/14 the speed of light. They are first observed when they appear to have been first produced at the central powerhouse, and are ...
Section 1 Notes on Stars
... • When the central temperature of a red giant reaches about 100 million K, helium fusion begins in the core. • A process called the triple alpha process, converts helium to carbon and oxygen. ...
... • When the central temperature of a red giant reaches about 100 million K, helium fusion begins in the core. • A process called the triple alpha process, converts helium to carbon and oxygen. ...
Document
... • When the central temperature of a red giant reaches about 100 million K, helium fusion begins in the core. • A process called the triple alpha process, converts helium to carbon and oxygen. ...
... • When the central temperature of a red giant reaches about 100 million K, helium fusion begins in the core. • A process called the triple alpha process, converts helium to carbon and oxygen. ...
Document
... • When the central temperature of a red giant reaches about 100 million K, helium fusion begins in the core. • A process called the triple alpha process, converts helium to carbon and oxygen. ...
... • When the central temperature of a red giant reaches about 100 million K, helium fusion begins in the core. • A process called the triple alpha process, converts helium to carbon and oxygen. ...
The Stellar Cycle
... electrons apart is called electron degeneracy pressure – this is what balances the weight. • Only if more energy drives the electrons into higher energy states, can the density increase. • Adding mass can drive electrons to higher energies so star shrinks. • At 1.4 solar masses—the Chandrasekhar Lim ...
... electrons apart is called electron degeneracy pressure – this is what balances the weight. • Only if more energy drives the electrons into higher energy states, can the density increase. • Adding mass can drive electrons to higher energies so star shrinks. • At 1.4 solar masses—the Chandrasekhar Lim ...
A Star is
... elements which compose Earth. • The most common elements in stars are hydrogen and helium, in that order. • Small quantities of carbon, oxygen, and nitrogen are also found in stars, but stars are primarily composed of…. • HYDROGEN and HELIUM ...
... elements which compose Earth. • The most common elements in stars are hydrogen and helium, in that order. • Small quantities of carbon, oxygen, and nitrogen are also found in stars, but stars are primarily composed of…. • HYDROGEN and HELIUM ...
low surface brightness galaxies
... • Compared to ellipticals, the spirals cover a distinctly smaller range in absolute magnitude (and mass). They are limited to −16 > MB > −23 and 109M < סּM < 1012Mסּ • Looking at the sequence of early-type spirals (i.e., Sa’s or SBa’s) to late-type spirals, we find a number of differences that can ...
... • Compared to ellipticals, the spirals cover a distinctly smaller range in absolute magnitude (and mass). They are limited to −16 > MB > −23 and 109M < סּM < 1012Mסּ • Looking at the sequence of early-type spirals (i.e., Sa’s or SBa’s) to late-type spirals, we find a number of differences that can ...
Document
... a. Which star is the hottest? Achernar Coolest? GL 725A b. Which star looks most red? GL 725A Most blue? Achernar c. Which star is the most luminous? Canopus Least luminous? GL 725A d. Which star appears the brightest? Canopus Faintest? GL 725A e. Which star’s spectrum shows the strongest Balmer lin ...
... a. Which star is the hottest? Achernar Coolest? GL 725A b. Which star looks most red? GL 725A Most blue? Achernar c. Which star is the most luminous? Canopus Least luminous? GL 725A d. Which star appears the brightest? Canopus Faintest? GL 725A e. Which star’s spectrum shows the strongest Balmer lin ...
EXAM II REVIEW - University of Maryland: Department of
... Motion toward or away from an observer causes a shift in the observed wavelength of light: • blueshift (shorter wavelength) motion toward you ...
... Motion toward or away from an observer causes a shift in the observed wavelength of light: • blueshift (shorter wavelength) motion toward you ...
CO 2 Cycle
... carried sediment in the past several years…The atmosphere on Mars is so thin that liquid water cannot persist at the surface. However, researchers propose that water could remain liquid long enough, after breaking out from an underground source, to carry debris before totally evaporating and freezin ...
... carried sediment in the past several years…The atmosphere on Mars is so thin that liquid water cannot persist at the surface. However, researchers propose that water could remain liquid long enough, after breaking out from an underground source, to carry debris before totally evaporating and freezin ...
Hertzsprung-Russell (H-R) Diagram Hertzsprung-Russell Diagram March 16 −
... Model of the solar interior X How to read H-R Diagram Spectrum of black body: Hotter=>bluer Energy generation in the sun X ...
... Model of the solar interior X How to read H-R Diagram Spectrum of black body: Hotter=>bluer Energy generation in the sun X ...
An introduction to the HR diagram File
... sequence depends entirely on its mass. Low mass stars are found at the right and high mass stars at the left. • The mass of a star controls its radius, its temperature, its life expectancy and its eventual fate. ...
... sequence depends entirely on its mass. Low mass stars are found at the right and high mass stars at the left. • The mass of a star controls its radius, its temperature, its life expectancy and its eventual fate. ...
Answer - Brock physics
... 16. A type Ia supernova occurs because of (a) the core collapse of a high-mass star. (b) the core collapse of a medium-mass star. (c) * matter from a nearby star falling onto the surface of a white dwarf, becoming compressed and heated, and eventually resulting in an explosion. (d) matter from a nea ...
... 16. A type Ia supernova occurs because of (a) the core collapse of a high-mass star. (b) the core collapse of a medium-mass star. (c) * matter from a nearby star falling onto the surface of a white dwarf, becoming compressed and heated, and eventually resulting in an explosion. (d) matter from a nea ...
Stages of stars - University of Dayton
... Life of a massive star (10 solar masses) Stage 1: Massive stars evolve in a similar way to a small stars until it reaches its main sequence stage. The stars shine steadily until the hydrogen has fused to form helium ( it takes billions of years in a small star, but only millions in a massive star) ...
... Life of a massive star (10 solar masses) Stage 1: Massive stars evolve in a similar way to a small stars until it reaches its main sequence stage. The stars shine steadily until the hydrogen has fused to form helium ( it takes billions of years in a small star, but only millions in a massive star) ...
Mr. Scharff
... Introduction. The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were al the same distance away. Rather than speak of the ...
... Introduction. The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were al the same distance away. Rather than speak of the ...
Lecture 31: The Properties of Stars
... Luminosity, the total energy output expressed in Watts or Solar Luminosities, depends on the radius and temperature. The absorption spectra of stars form a distinct sequence with stellar temperature, giving us a way to classify stars. Spectral Classes of Stars: O B A F G K M L T The Hertzsprung-Russ ...
... Luminosity, the total energy output expressed in Watts or Solar Luminosities, depends on the radius and temperature. The absorption spectra of stars form a distinct sequence with stellar temperature, giving us a way to classify stars. Spectral Classes of Stars: O B A F G K M L T The Hertzsprung-Russ ...
Position in Solar System ppt
... The Universe contains billions of galaxies, each containing millions or billions of stars. Therefore, the galaxy in which our solar system and essentially all of us live, is just one of ...
... The Universe contains billions of galaxies, each containing millions or billions of stars. Therefore, the galaxy in which our solar system and essentially all of us live, is just one of ...
Stellar Classification - Solar Physics and Space Weather
... hydrogen lines • As O and B stars are so powerful, they live for a very short time and tend to cluster together in OB1 associations, which are associated with giant molecular clouds • The Orion OB1 association is an entire spiral arm of our Galaxy and contains all the constellation of Orion. ...
... hydrogen lines • As O and B stars are so powerful, they live for a very short time and tend to cluster together in OB1 associations, which are associated with giant molecular clouds • The Orion OB1 association is an entire spiral arm of our Galaxy and contains all the constellation of Orion. ...
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.