Stars and Galaxies
... shifted towards the red part of the visible spectrum The faster they move away from us, the more they are redshifted. Thus, redshift is a reasonable way to measure the speed of an object. When we observe the redshift of galaxies, almost every galaxy appears to be moving away from us – the Univer ...
... shifted towards the red part of the visible spectrum The faster they move away from us, the more they are redshifted. Thus, redshift is a reasonable way to measure the speed of an object. When we observe the redshift of galaxies, almost every galaxy appears to be moving away from us – the Univer ...
Observational Data
... 1) actively star forming galaxies (>100-500Mo/yr) 2) irregular light distribution, clumpy SF regions, high detected asymmetries, ongoing mergers? 3) low light concentration similar to local starbursts and ULIRGs 4) old underlyings, half light radii~6kpc (large) ...
... 1) actively star forming galaxies (>100-500Mo/yr) 2) irregular light distribution, clumpy SF regions, high detected asymmetries, ongoing mergers? 3) low light concentration similar to local starbursts and ULIRGs 4) old underlyings, half light radii~6kpc (large) ...
Test 3 Review
... • Get plenty of rest the night before • Bring at least 2 pencils, UNM student ID, and a calculator 2) During the Test: • Write out and bubble your last name, space, first name and Exam color in the name space of the scantron form. Write out and bubble your Banner ID in the ID space. • Draw simple sk ...
... • Get plenty of rest the night before • Bring at least 2 pencils, UNM student ID, and a calculator 2) During the Test: • Write out and bubble your last name, space, first name and Exam color in the name space of the scantron form. Write out and bubble your Banner ID in the ID space. • Draw simple sk ...
Lecture 8a Star Formation 10/15/2014
... • formed at the same time • similar chemical composition • about the same distance from us Can classify by appearance and use to: ...
... • formed at the same time • similar chemical composition • about the same distance from us Can classify by appearance and use to: ...
The Solar Neighborhood
... The globular star clusters are bright, and can be seen for a long distance. Their distances can be estimated accurately from their main sequence turnoffs, as well as by measuring the periods of variable stars that belong to each cluster. In the table below are listed several dozen Galactic globular ...
... The globular star clusters are bright, and can be seen for a long distance. Their distances can be estimated accurately from their main sequence turnoffs, as well as by measuring the periods of variable stars that belong to each cluster. In the table below are listed several dozen Galactic globular ...
Today in Astronomy 102: black hole observations, v.2
... Observe two or more of these features to find a black hole: Gravitational deflection of light, by an amount requiring black hole masses and sizes. X-ray and/or g-ray emission from ionized gas falling into the black hole. Orbital motion of nearby stars or gas clouds that can be used to infer th ...
... Observe two or more of these features to find a black hole: Gravitational deflection of light, by an amount requiring black hole masses and sizes. X-ray and/or g-ray emission from ionized gas falling into the black hole. Orbital motion of nearby stars or gas clouds that can be used to infer th ...
distribution and properties of a sample of massive young stars
... the distance ambiguity for RMS sources located within 18◦ |l| 54◦ . These two steps yield kinematic distances to 291 sources out of a possible 326, located within the GRS longitude range. Combining distances and integrated fluxes derived from spectral energy distributions, we estimate luminosities ...
... the distance ambiguity for RMS sources located within 18◦ |l| 54◦ . These two steps yield kinematic distances to 291 sources out of a possible 326, located within the GRS longitude range. Combining distances and integrated fluxes derived from spectral energy distributions, we estimate luminosities ...
Equipartition magnetic fields in normal galaxies
... shows comparatively steeper value of a than NGC 6946, indicating efficient magnetic field amplification, perhaps caused due to bar action. However, more data are required to firmly establish our results. In Fig. 2(c) we plot the ratio of the magnetic field energy density (U mag = B2eq /8π) to that o ...
... shows comparatively steeper value of a than NGC 6946, indicating efficient magnetic field amplification, perhaps caused due to bar action. However, more data are required to firmly establish our results. In Fig. 2(c) we plot the ratio of the magnetic field energy density (U mag = B2eq /8π) to that o ...
Ch 11c and 12 ( clusters 3-31-11)
... If the brightest main sequence star in cluster 1 is a B star and the brightest main sequence star in cluster 2 is an M star. What can we say about the age of these two clusters? A. Nothing, there is not enough information B. Cluster 1 is older than cluster 2 C. Cluster 2 is older than cluster 1 ...
... If the brightest main sequence star in cluster 1 is a B star and the brightest main sequence star in cluster 2 is an M star. What can we say about the age of these two clusters? A. Nothing, there is not enough information B. Cluster 1 is older than cluster 2 C. Cluster 2 is older than cluster 1 ...
Galaxies - University of Iowa Astrophysics
... hidden mass in the Galaxy? A) We observe cool clouds of hydrogen. B) We infer this from the oscillation periods of RR Lyrae variable stars in globular clusters. C) We observe flat rotation curve for stars in the Milky Way at large distances from the Galactic center? D) We observe dusty regions in th ...
... hidden mass in the Galaxy? A) We observe cool clouds of hydrogen. B) We infer this from the oscillation periods of RR Lyrae variable stars in globular clusters. C) We observe flat rotation curve for stars in the Milky Way at large distances from the Galactic center? D) We observe dusty regions in th ...
Chapter 27 Quasars, Active Galaxies, and Gamma
... Rotation curves of stars near the centers of most galaxies show the presence of supermassive black holes with mass ranging from 106 to 109 solar masses. Essentially all galaxies contain supermassive black holes and were likely active galaxies at some point in their lives. ...
... Rotation curves of stars near the centers of most galaxies show the presence of supermassive black holes with mass ranging from 106 to 109 solar masses. Essentially all galaxies contain supermassive black holes and were likely active galaxies at some point in their lives. ...
Chapter 7 in the LSST Science Book
... to form within dark matter halos that are themselves growing through gravitational collapse and mergers. In fact, we are very fortunate to live in a hierarchical Universe where the LV galaxies contain the signatures not only of their own formation, but also of the hundreds of galaxies that they accr ...
... to form within dark matter halos that are themselves growing through gravitational collapse and mergers. In fact, we are very fortunate to live in a hierarchical Universe where the LV galaxies contain the signatures not only of their own formation, but also of the hundreds of galaxies that they accr ...
... rates of about 2 to 50 oC per hour. Most chondrules cooled faster, about 100-1000 oC per hour. The experiments also suggest that chondrules and CAIs formed from pre-existing solids, and chondrules were probably recycled through the melting process several times. Thus, these components record the eff ...
Lecture 3 - University of Washington
... Galaxies • Galaxies are (mostly) made of stars (also gas, dust, active galactic nuclei – AGN); hence have similar (but not identical!) color distributions • They come in various shapes and forms (spiral vs. ellipticals; aka exponential vs. de Vaucouleurs profiles) • Some host AGNs, some have high s ...
... Galaxies • Galaxies are (mostly) made of stars (also gas, dust, active galactic nuclei – AGN); hence have similar (but not identical!) color distributions • They come in various shapes and forms (spiral vs. ellipticals; aka exponential vs. de Vaucouleurs profiles) • Some host AGNs, some have high s ...
Multiple Linear Regression
... Weather modification, or cloud seeding, is the treatment of individual clouds or storm systems with various inorganic and organic materials in the hope of achieving an increase in rainfall. Introduction of such material into a cloud that contains supercooled water, that is, liquid water colder than ...
... Weather modification, or cloud seeding, is the treatment of individual clouds or storm systems with various inorganic and organic materials in the hope of achieving an increase in rainfall. Introduction of such material into a cloud that contains supercooled water, that is, liquid water colder than ...
Topic 4 - The University of Sheffield
... a high enough central temperature for the fusion reactions that convert H into He normal in larger mass stars to start and produce high luminosity. ...
... a high enough central temperature for the fusion reactions that convert H into He normal in larger mass stars to start and produce high luminosity. ...
astronomy
... properties of the Earth’s atmosphere affect our ability to make astronomical observations at different wavelengths. Explain what is meant by the term ”black body” radiation” and describe the basic properties of such radiation. Tell how we can determine the temperature of an object by observing the r ...
... properties of the Earth’s atmosphere affect our ability to make astronomical observations at different wavelengths. Explain what is meant by the term ”black body” radiation” and describe the basic properties of such radiation. Tell how we can determine the temperature of an object by observing the r ...
PowerPoint
... a) Clouds fragment into smaller objects, forming many stars at one time. b) One star forms; other matter goes into planets, moons, asteroids, & comets. c) Clouds rotate & throw off mass until only enough is left to form one star. ...
... a) Clouds fragment into smaller objects, forming many stars at one time. b) One star forms; other matter goes into planets, moons, asteroids, & comets. c) Clouds rotate & throw off mass until only enough is left to form one star. ...
Population synthesis view of gravitational waves - Astro-PF
... Simulation to rates: normalisation Galactic supernova rate, Galactic blue luminosity + blue luminosity density in the local Universe: ...
... Simulation to rates: normalisation Galactic supernova rate, Galactic blue luminosity + blue luminosity density in the local Universe: ...
26.4 Groups of Stars
... caused by its rotation. The sun takes about 220 million years to complete one orbit around the galaxy’s center. Recent evidence suggests that there is a massive black hole at our galaxy’s center. Stars are forming in the galaxy's spiral arms. ...
... caused by its rotation. The sun takes about 220 million years to complete one orbit around the galaxy’s center. Recent evidence suggests that there is a massive black hole at our galaxy’s center. Stars are forming in the galaxy's spiral arms. ...
English Summary
... Enrichment of the interstellar medium We have seen that the gas from which the stars are formed consist mostly of hydrogen. Through the ejection of their envelope, Planetary Nebulae return gas to the interstellar medium from which future generations of stars will be formed. This gas still contains m ...
... Enrichment of the interstellar medium We have seen that the gas from which the stars are formed consist mostly of hydrogen. Through the ejection of their envelope, Planetary Nebulae return gas to the interstellar medium from which future generations of stars will be formed. This gas still contains m ...
151 - ESO
... During one of these pulsations the size of the star also changes. The radius of the star can alter with 10-20%. Harvard astronomer Miss Henrietta Leavitt was the first person to determine distances using Cepheids. Therefor in 1912 she made it possible to prove that “spiral-nebulas” (?) are independe ...
... During one of these pulsations the size of the star also changes. The radius of the star can alter with 10-20%. Harvard astronomer Miss Henrietta Leavitt was the first person to determine distances using Cepheids. Therefor in 1912 she made it possible to prove that “spiral-nebulas” (?) are independe ...
Astro 10B Study Questions for Each Chapter
... What would happen if the Sun were replaced by a 1M~ black hole? How big would a 1 M~ black hole be? How does the Schwarzschild radius vary with a black hole’s mass? How do we detected black holes if we cannot see them? Why would jumping into a black hole be suicide? Why aren’t black holes ‘cosmic va ...
... What would happen if the Sun were replaced by a 1M~ black hole? How big would a 1 M~ black hole be? How does the Schwarzschild radius vary with a black hole’s mass? How do we detected black holes if we cannot see them? Why would jumping into a black hole be suicide? Why aren’t black holes ‘cosmic va ...
PPT - ALFALFA survey
... • The ADBS sample provides an excellent means to investigate the environmental influences on gas-rich galaxies in low-to-intermediate densities, thereby permitting an assessment of how the local environment of a galaxy affects its evolution. ...
... • The ADBS sample provides an excellent means to investigate the environmental influences on gas-rich galaxies in low-to-intermediate densities, thereby permitting an assessment of how the local environment of a galaxy affects its evolution. ...
Lecture-25 Notes - Georgia Southern University Astrophysics
... different (apparently) from filament galaxies. ...
... different (apparently) from filament galaxies. ...