2.3 Peculiar galaxies
... skirt by each other they will perhaps pull out tidal tails from each other and then carry on. If they head close towards each other, the material is likely to orbit around in a complex manner until eventually they completely merge. Star formation in galaxies. We now move to an apparently separate su ...
... skirt by each other they will perhaps pull out tidal tails from each other and then carry on. If they head close towards each other, the material is likely to orbit around in a complex manner until eventually they completely merge. Star formation in galaxies. We now move to an apparently separate su ...
Document
... The Universe is filled with these star systems which themselves cluster together into larger systems. ...
... The Universe is filled with these star systems which themselves cluster together into larger systems. ...
Large Scale Structure of the Universe Lab
... Since the mid-1980’s astronomers have gathered data allowing, for the first time, a view of the structure of the Universe in three-dimensions. You might speculate that an image of this structure could be determined by photographing stars to see if they form some kind of pattern. An example of a star ...
... Since the mid-1980’s astronomers have gathered data allowing, for the first time, a view of the structure of the Universe in three-dimensions. You might speculate that an image of this structure could be determined by photographing stars to see if they form some kind of pattern. An example of a star ...
Chapter 7: The Galaxy, structure and content File
... a cartoon to remind you of its different components. The luminous parts are mostly a disc of population I stars and a bulge of older population II stars. We live in the disc, with the Sun at a distance R0 = 8.0 kpc from the centre. There is also gas and dust: the gas is mostly observed as an H I lay ...
... a cartoon to remind you of its different components. The luminous parts are mostly a disc of population I stars and a bulge of older population II stars. We live in the disc, with the Sun at a distance R0 = 8.0 kpc from the centre. There is also gas and dust: the gas is mostly observed as an H I lay ...
Galaxy Formation, Reionization, the First Stars and Quasars
... If the gas cools and contracts without angular momentum loss to form a thin, angular momentum supported exponential disc, the disc scale radius is given by Mo, Mao & White (1998): ...
... If the gas cools and contracts without angular momentum loss to form a thin, angular momentum supported exponential disc, the disc scale radius is given by Mo, Mao & White (1998): ...
Galaxies and the Universe bb
... Galaxies ______________ galaxy • Structure • Determined by using ______ telescopes • Large spiral galaxy • About 100,000 light-years wide • Thickness at the galactic nucleus is about 10,000 light-years • _____ spiral arms of stars • Sun is 30,000 light-years from the center ...
... Galaxies ______________ galaxy • Structure • Determined by using ______ telescopes • Large spiral galaxy • About 100,000 light-years wide • Thickness at the galactic nucleus is about 10,000 light-years • _____ spiral arms of stars • Sun is 30,000 light-years from the center ...
Traka Resources Limited ABN 63 103 323 173
... Forward looking statements in this document are based on Galaxy’s beliefs, opinions and estimates of Galaxy as of the dates the forward looking statements are made, and no obligation is assumed to update forward looking statements if these beliefs, opinions and estimates should change or to reflect ...
... Forward looking statements in this document are based on Galaxy’s beliefs, opinions and estimates of Galaxy as of the dates the forward looking statements are made, and no obligation is assumed to update forward looking statements if these beliefs, opinions and estimates should change or to reflect ...
An Analysis of Collisional Ring Galaxies
... galaxy rotate at a higher rate than those stars located further from the galactic center. The stars found in the halo do not seem to show any uniform rotation about the center.1 Overall these inner motions tend to keep to themselves, with the galactic stars rotating “calmly” about a central axis. W ...
... galaxy rotate at a higher rate than those stars located further from the galactic center. The stars found in the halo do not seem to show any uniform rotation about the center.1 Overall these inner motions tend to keep to themselves, with the galactic stars rotating “calmly” about a central axis. W ...
Galaxies - cloudfront.net
... • Elliptical galaxies are more-or-less egg shaped. The smallest elliptical galaxies are as small as some globular clusters. The largest elliptical galaxies can contain over a trillion stars. Most stars in elliptical galaxies are reddish to yellowish in color because they are old stars. Most elliptic ...
... • Elliptical galaxies are more-or-less egg shaped. The smallest elliptical galaxies are as small as some globular clusters. The largest elliptical galaxies can contain over a trillion stars. Most stars in elliptical galaxies are reddish to yellowish in color because they are old stars. Most elliptic ...
Chapter 15, Galaxies
... How do we measure the distance of objects far away in the universe, much farther than the distance that can be measured by stellar parallax? • Measurement of distance farther than the reach of stellar parallax rely on our ability to find objects with known luminosity… • In 1924, Edwin Hubble determi ...
... How do we measure the distance of objects far away in the universe, much farther than the distance that can be measured by stellar parallax? • Measurement of distance farther than the reach of stellar parallax rely on our ability to find objects with known luminosity… • In 1924, Edwin Hubble determi ...
–1– 2. Milky Way We know a great deal, perhaps more than any
... • Herschel (1785) used star counts to infer a flattened distribution for the MW. • A similar, but much larger survey of nearby stars was done by Kapteyn around 1920. He used parallax, proper motions, radial velocities and spectra to infer the distance to stars. He inferred that the size of the MW is ...
... • Herschel (1785) used star counts to infer a flattened distribution for the MW. • A similar, but much larger survey of nearby stars was done by Kapteyn around 1920. He used parallax, proper motions, radial velocities and spectra to infer the distance to stars. He inferred that the size of the MW is ...
EvoluGon of high mass stars Solar-‐type stars end their lives by
... to the forma=on of a rapidly rota=ng neutron star because of conserva=on of angular momentum (if the Sun was compressed into a radius of 10 km it would rotate at 1000 =mes per second). ...
... to the forma=on of a rapidly rota=ng neutron star because of conserva=on of angular momentum (if the Sun was compressed into a radius of 10 km it would rotate at 1000 =mes per second). ...
Large Scale Structure of the Universe
... Since the mid-1980’s astronomers have gathered data allowing, for the first time, a view of the structure of the Universe in three-dimensions. You might speculate that an image of this structure could be determined by photographing stars to see if they form some kind of pattern. An example of a star ...
... Since the mid-1980’s astronomers have gathered data allowing, for the first time, a view of the structure of the Universe in three-dimensions. You might speculate that an image of this structure could be determined by photographing stars to see if they form some kind of pattern. An example of a star ...
Andromeda Galaxy
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The Andromeda Galaxy (/ænˈdrɒmɨdə/), also known as Messier 31, M31, or NGC 224, is a spiral galaxy approximately 780 kiloparsecs (2.5 million light-years) from Earth. It is the nearest major galaxy to the Milky Way and was often referred to as the Great Andromeda Nebula in older texts. It received its name from the area of the sky in which it appears, the constellation of Andromeda, which was named after the mythological princess Andromeda. Being approximately 220,000 light years across, it is the largest galaxy of the Local Group, which also contains the Milky Way, the Triangulum Galaxy, and about 44 other smaller galaxies.The Andromeda Galaxy is the most massive galaxy in the Local Group as well. Despite earlier findings that suggested that the Milky Way contains more dark matter and could be the most massive in the grouping, the 2006 observations by the Spitzer Space Telescope revealed that Andromeda contains one trillion (1012) stars: at least twice the number of stars in the Milky Way, which is estimated to be 200–400 billion.The Andromeda Galaxy is estimated to be 1.5×1012 solar masses, while the mass of the Milky Way is estimated to be 8.5×1011 solar masses. In comparison, a 2009 study estimated that the Milky Way and M31 are about equal in mass, while a 2006 study put the mass of the Milky Way at ~80% of the mass of the Andromeda Galaxy. The Milky Way and Andromeda are expected to collide in 3.75 billion years, eventually merging to form a giant elliptical galaxy or perhaps a large disk galaxy.At 3.4, the apparent magnitude of the Andromeda Galaxy is one of the brightest of any of the Messier objects, making it visible to the naked eye on moonless nights even when viewed from areas with moderate light pollution. Although it appears more than six times as wide as the full Moon when photographed through a larger telescope, only the brighter central region is visible to the naked eye or when viewed using binoculars or a small telescope and would it hence appear to be but another star.