P10263v1.2 Lab 8 Text
... blocked by the interstellar medium in our galaxy and the fact that it has a very low surface brightness. The structure of the Milky Way also affects our observations of objects within the galaxy. For example, even though we know that stars are more or less uniformly distributed around the Milky Way ...
... blocked by the interstellar medium in our galaxy and the fact that it has a very low surface brightness. The structure of the Milky Way also affects our observations of objects within the galaxy. For example, even though we know that stars are more or less uniformly distributed around the Milky Way ...
Introduction to Galaxies 5/23/2013 BR: Milky Way Scale The Milky
... centered on a specific point and appear to orbit the center of the Milky Way. The center of the Milky Way is a region of very high star density, most of which is obscured by interstellar gas and dust. Motion of stars that orbit close to the galactic center indicate that this area has about 2.6 milli ...
... centered on a specific point and appear to orbit the center of the Milky Way. The center of the Milky Way is a region of very high star density, most of which is obscured by interstellar gas and dust. Motion of stars that orbit close to the galactic center indicate that this area has about 2.6 milli ...
"Dark Matter in the Milky Way - how to find it using Gaia and other
... potential fits known constraints. This Φ will have some vertical disc density profile at the Sun 2. Fit f(J) to (binned) kinematics of RAVE giants, which predicts a different disc density profile. 3. Iterate until these two vertical profiles agree with each other 4. Compare to vertical density profi ...
... potential fits known constraints. This Φ will have some vertical disc density profile at the Sun 2. Fit f(J) to (binned) kinematics of RAVE giants, which predicts a different disc density profile. 3. Iterate until these two vertical profiles agree with each other 4. Compare to vertical density profi ...
Dark Matter in the Milky Way - how to find it using Gaia and other
... that is on near circular orbits in the Milky Way We can measure the proper motion of (and distance to) Sgr A* We roughly know the structure bulge, halo, disc(s) with ~known scale lengths There are existing constraints on the Milky Way’s mass from other dynamical modeling (you don’t have to do everyt ...
... that is on near circular orbits in the Milky Way We can measure the proper motion of (and distance to) Sgr A* We roughly know the structure bulge, halo, disc(s) with ~known scale lengths There are existing constraints on the Milky Way’s mass from other dynamical modeling (you don’t have to do everyt ...
The Milky Way - Chandra X
... At a distance of a few hundred light years we encounter clouds of dust and gas illuminated by brilliant clusters of young stars. These clouds and star clusters are part of the Orion spiral arm. As we move further out, fifty thousand light years from the Sun, other spiral arms of the Galaxy come into ...
... At a distance of a few hundred light years we encounter clouds of dust and gas illuminated by brilliant clusters of young stars. These clouds and star clusters are part of the Orion spiral arm. As we move further out, fifty thousand light years from the Sun, other spiral arms of the Galaxy come into ...
The Milky Way - Chandra X
... At a distance of a few hundred light years we encounter clouds of dust and gas illuminated by brilliant clusters of young stars. These clouds and star clusters are part of the Orion spiral arm. As we move further out, fifty thousand light years from the Sun, other spiral arms of the Galaxy come into ...
... At a distance of a few hundred light years we encounter clouds of dust and gas illuminated by brilliant clusters of young stars. These clouds and star clusters are part of the Orion spiral arm. As we move further out, fifty thousand light years from the Sun, other spiral arms of the Galaxy come into ...
15.4 Star Systems and Galaxies
... I. Star Systems and Planets A. Star system-groups of two or more stars 1. Binary stars - two stars or double stars a. Eclipsing binary-a system in which one star blocks the light from another II. Planets Around Other Stars A. Astronomers study gravitational effects on stars to see if there is a pla ...
... I. Star Systems and Planets A. Star system-groups of two or more stars 1. Binary stars - two stars or double stars a. Eclipsing binary-a system in which one star blocks the light from another II. Planets Around Other Stars A. Astronomers study gravitational effects on stars to see if there is a pla ...
ASTR 1120 STUDY GUIDE FOR MIDTERM III This guide is to aid
... are familiar with all the phases of the cycle, and how we observe them, depending on their temperature. 2. How does the Milky Way look at various wavelengths? Which wavelengths are mostly absorbed and which ones are not? 3. The cosmic “distance ladder”: what are the various ways by which astronomers ...
... are familiar with all the phases of the cycle, and how we observe them, depending on their temperature. 2. How does the Milky Way look at various wavelengths? Which wavelengths are mostly absorbed and which ones are not? 3. The cosmic “distance ladder”: what are the various ways by which astronomers ...
1. a. Collisionless Boltzmann—particles moving in smooth potential
... affected by dust so we can “see” the inner Galaxy. Optical depth in the line is also a relatively minor concern. The problems with R<3 kpc are a lack of gas disk tracers and the presence of a bar that produces strongly non-circular orbits, the x1 and x2 orbit families. If we use stars as tracers the ...
... affected by dust so we can “see” the inner Galaxy. Optical depth in the line is also a relatively minor concern. The problems with R<3 kpc are a lack of gas disk tracers and the presence of a bar that produces strongly non-circular orbits, the x1 and x2 orbit families. If we use stars as tracers the ...
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 ...
Milky Way Galaxy
... A main sequence star can shine for millions of years or more. The amount of time it lives is determined by how big it is. Medium stars In medium size stars, after the nuclear fusion has used up all the fuel it has, gravity will pull the remaining material closer together. The star will shrink. In fa ...
... A main sequence star can shine for millions of years or more. The amount of time it lives is determined by how big it is. Medium stars In medium size stars, after the nuclear fusion has used up all the fuel it has, gravity will pull the remaining material closer together. The star will shrink. In fa ...
The Milky Way - Clive Gifford
... The Milky Way is part of a cluster, or collection, of galaxies known as the Local Group. These include Andromeda, the Triangulam galaxy and Canis Major Dwarf as well as a further 40 galaxies, some of which have only recently been discovered. The Local Group has a diameter of about 10 million light y ...
... The Milky Way is part of a cluster, or collection, of galaxies known as the Local Group. These include Andromeda, the Triangulam galaxy and Canis Major Dwarf as well as a further 40 galaxies, some of which have only recently been discovered. The Local Group has a diameter of about 10 million light y ...
Final for Astro 322, Prof. Heinke, April 23rd, 2010 Formula sheet
... c) What are two possibilities for the original source of the energy we see? (Describe each in a couple of sentences.) They are not necessarily exclusive. d) What do you think this galaxy’s recent history has been, and what will happen to it now? Problem 3: Distorted galaxy, and dark matter a) We see ...
... c) What are two possibilities for the original source of the energy we see? (Describe each in a couple of sentences.) They are not necessarily exclusive. d) What do you think this galaxy’s recent history has been, and what will happen to it now? Problem 3: Distorted galaxy, and dark matter a) We see ...
Galaxies - Stockton University
... In the modern picture of our Galaxy, the Sun is 8 kpc from the center of the Galaxy. The Sun resides in a flattened circular disk which is of order 200 pc thick and extends out to about 15 Kpc. Thus the disk is of order 100,000 light-years across. At the center of the disk is the spheroid or bulge. ...
... In the modern picture of our Galaxy, the Sun is 8 kpc from the center of the Galaxy. The Sun resides in a flattened circular disk which is of order 200 pc thick and extends out to about 15 Kpc. Thus the disk is of order 100,000 light-years across. At the center of the disk is the spheroid or bulge. ...
PHYSICS 1500 ASTRONOMY Sample Exam Solutions Section B
... (a) It seems that all Type I supernovae have about the same intrinsic luminosity at their peak. Therefore, if we observe one in a distant galaxy, we can compare its apparent brightness with its expected intrinsic brightness to estimate its distance. This will also be the distance to the galaxy in wh ...
... (a) It seems that all Type I supernovae have about the same intrinsic luminosity at their peak. Therefore, if we observe one in a distant galaxy, we can compare its apparent brightness with its expected intrinsic brightness to estimate its distance. This will also be the distance to the galaxy in wh ...
No Slide Title
... orbits <=> the system has some prograde rotation. Spherical system (right panel) has completely disorganized motions, no rotation ...
... orbits <=> the system has some prograde rotation. Spherical system (right panel) has completely disorganized motions, no rotation ...
lecture20
... makes the universe evolve: the cycle of star formation and death, and the chemical enrichment of the cosmos. • ISM also “disturbs” observations, since it absorbs light and modifies (reddens) colors ...
... makes the universe evolve: the cycle of star formation and death, and the chemical enrichment of the cosmos. • ISM also “disturbs” observations, since it absorbs light and modifies (reddens) colors ...