How do stars orbit in our galaxy?
... out of spiral arms Density Wave: think of traffic! Cars on the freeway bunch up as they approach a slow moving construction crew working along the hard shoulder. Bunching up is the density wave. The wave keeps moving forward, and each car gets through … eventually. ...
... out of spiral arms Density Wave: think of traffic! Cars on the freeway bunch up as they approach a slow moving construction crew working along the hard shoulder. Bunching up is the density wave. The wave keeps moving forward, and each car gets through … eventually. ...
PH607lec10-4gal2
... Disks: metal rich stars and ISM, nearly circular orbits with little random motion, spiral patterns Bulge: metal poor to super-rich stars, high stellar densities, mostly random motion – similar to ellipticals Bar: present in 50 % of disk galaxies, long lived, flat, linear distribution of stars ...
... Disks: metal rich stars and ISM, nearly circular orbits with little random motion, spiral patterns Bulge: metal poor to super-rich stars, high stellar densities, mostly random motion – similar to ellipticals Bar: present in 50 % of disk galaxies, long lived, flat, linear distribution of stars ...
9 Dwarf Galaxies
... Disks: metal rich stars and ISM, nearly circular orbits with little random motion, spiral patterns Bulge: metal poor to super-rich stars, high stellar densities, mostly random motion – similar to ellipticals Bar: present in 50 % of disk galaxies, long lived, flat, linear distribution of stars ...
... Disks: metal rich stars and ISM, nearly circular orbits with little random motion, spiral patterns Bulge: metal poor to super-rich stars, high stellar densities, mostly random motion – similar to ellipticals Bar: present in 50 % of disk galaxies, long lived, flat, linear distribution of stars ...
Every large galaxy seems to have a supermassive black hole at its
... Coevolution implies that the evolution of black holes and galaxies is some sort of tandem process in which the two parties “communicate” through feedback. Since 2000, Kormendy adds, “all sorts of people have tried to come up with theories for how black holes and galaxies talk to each other, and how ...
... Coevolution implies that the evolution of black holes and galaxies is some sort of tandem process in which the two parties “communicate” through feedback. Since 2000, Kormendy adds, “all sorts of people have tried to come up with theories for how black holes and galaxies talk to each other, and how ...
Giannone
... more stellar populations 4. Es are characterized by different space mass densities 5. Gas distributions (and therefore star formations) differed in Es ...
... more stellar populations 4. Es are characterized by different space mass densities 5. Gas distributions (and therefore star formations) differed in Es ...
... • Galaxies and other objects may have motions that have nothing to do with the expansion of space • When galaxies orbit each other, sometimes their orbital speed is much larger than the redshift caused by expansion. • We cannot use Hubble’s law for nearby galaxies, and certainly not for any objects ...
How we know black holes exist
... Using this velocity and the amount of time stars take to complete a full orbit around the center of M87, Gebhardt and colleagues determined that the object at the center of the accretion disk holds some 6.6 billion times our Sun’s mass — that’s more than 1,000 times that of the Milky Way’s central b ...
... Using this velocity and the amount of time stars take to complete a full orbit around the center of M87, Gebhardt and colleagues determined that the object at the center of the accretion disk holds some 6.6 billion times our Sun’s mass — that’s more than 1,000 times that of the Milky Way’s central b ...
PH607lec12-5gal3
... Disks: metal rich stars and ISM, nearly circular orbits with little random motion, spiral patterns Bulge: metal poor to super-rich stars, high stellar densities, mostly random motion – similar to ellipticals Bar: present in 50 % of disk galaxies, long lived, flat, linear distribution of stars ...
... Disks: metal rich stars and ISM, nearly circular orbits with little random motion, spiral patterns Bulge: metal poor to super-rich stars, high stellar densities, mostly random motion – similar to ellipticals Bar: present in 50 % of disk galaxies, long lived, flat, linear distribution of stars ...
Estimating the mass and star formation rate in galaxies
... temperature they also emit infared radiation. As a consequence the infrared sky from the ground is much “brighter” as we say than in the optical. The signal reaching us from space is a small addition to this emission from the atmosphere. This has severe consequences to the way we collect and anal ...
... temperature they also emit infared radiation. As a consequence the infrared sky from the ground is much “brighter” as we say than in the optical. The signal reaching us from space is a small addition to this emission from the atmosphere. This has severe consequences to the way we collect and anal ...
Interacting Galaxies
... galaxies the brightest infrared objects in the sky—emitting up to several trillion times the luminosity of our Sun, but radiated as infrared energy, not as visible light. There were concerns, in fact, that using Hubble within the GOALS project to study star formation in visible light in these lumino ...
... galaxies the brightest infrared objects in the sky—emitting up to several trillion times the luminosity of our Sun, but radiated as infrared energy, not as visible light. There were concerns, in fact, that using Hubble within the GOALS project to study star formation in visible light in these lumino ...
30-3 Directed Reading
... _____ 2. Although the stars that make up a pattern appear to be close together, a. they are not all the same distance from Earth. b. they are not all stars. c. they are all the same distance from Earth. d. they are not all visible from Earth. _____ 3. If you look at the same region of the sky for se ...
... _____ 2. Although the stars that make up a pattern appear to be close together, a. they are not all the same distance from Earth. b. they are not all stars. c. they are all the same distance from Earth. d. they are not all visible from Earth. _____ 3. If you look at the same region of the sky for se ...
flare swg usa
... Many protostars are clustered within a single “core” as typically A filament seen at 70-160-250 filament as seen with Spitzer (24-8-3.5) defined by the large beam of Herschel observations. Á ...
... Many protostars are clustered within a single “core” as typically A filament seen at 70-160-250 filament as seen with Spitzer (24-8-3.5) defined by the large beam of Herschel observations. Á ...
14. The Milky Way Galaxy: A Spiral in Space
... • An accretion disk surrounding the black hole emits enormous amounts of radiation. ...
... • An accretion disk surrounding the black hole emits enormous amounts of radiation. ...
Part 2 - Aryabhat
... All stars shine but none do it like Sirius, the brightest star in the night sky. Aptly named, Sirius comes from the Greek word Seirius, meaning, "searing" or "scorching." Blazing at a visual magnitude of –1.42, it is twice as bright as any other star in our sky. Sirius resides in the constellation C ...
... All stars shine but none do it like Sirius, the brightest star in the night sky. Aptly named, Sirius comes from the Greek word Seirius, meaning, "searing" or "scorching." Blazing at a visual magnitude of –1.42, it is twice as bright as any other star in our sky. Sirius resides in the constellation C ...
Messier 87
Messier 87 (also known as Virgo A or NGC 4486, and generally abbreviated to M87) is a supergiant elliptical galaxy in the constellation Virgo. One of the most massive galaxies in the local universe, it is notable for its large population of globular clusters—M87 contains about 12,000 compared to the 150-200 orbiting the Milky Way—and its jet of energetic plasma that originates at the core and extends outward at least 1,500 parsecs (4,900 light-years), travelling at relativistic speed. It is one of the brightest radio sources in the sky, and is a popular target for both amateur astronomy observations and professional astronomy study.French astronomer Charles Messier discovered M87 in 1781, cataloguing it as a nebulous feature while searching for objects that would confuse comet hunters. The second brightest galaxy within the northern Virgo Cluster, M87 is located about 16.4 million parsecs (53.5 million light-years) from Earth. Unlike a disk-shaped spiral galaxy, M87 has no distinctive dust lanes. Instead, it has an almost featureless, ellipsoidal shape typical of most giant elliptical galaxies, diminishing in luminosity with distance from the centre. Forming around one sixth of M87's mass, the stars in this galaxy have a nearly spherically symmetric distribution, their density decreasing with increasing distance from the core. At the core is a supermassive black hole, which forms the primary component of an active galactic nucleus. This object is a strong source of multiwavelength radiation, particularly radio waves. M87's galactic envelope extends out to a radius of about 150 kiloparsecs (490,000 light-years), where it has been truncated—possibly by an encounter with another galaxy. Between the stars is a diffuse interstellar medium of gas that has been chemically enriched by elements emitted from evolved stars.