Galaxies
... Galaxy mass measurements show that galaxies need between 3 and 10 times more mass than can be observed to explain their rotation curves. The discrepancy is even larger in galaxy clusters, which need 10 to 100 times more mass. The total needed is more than the sum of the dark matter associated with e ...
... Galaxy mass measurements show that galaxies need between 3 and 10 times more mass than can be observed to explain their rotation curves. The discrepancy is even larger in galaxy clusters, which need 10 to 100 times more mass. The total needed is more than the sum of the dark matter associated with e ...
Dynamics of elliptical galaxies
... Classification of stellar orbits in elliptical galaxies is much more complicated than for disk galaxies. Most important distinction is between axisymmetric galaxies (prolate or oblate) and triaxial galaxies. In an axisymmetric galaxy, there is a plane, perpendicular to the symmetry axis, in which gr ...
... Classification of stellar orbits in elliptical galaxies is much more complicated than for disk galaxies. Most important distinction is between axisymmetric galaxies (prolate or oblate) and triaxial galaxies. In an axisymmetric galaxy, there is a plane, perpendicular to the symmetry axis, in which gr ...
AJAstroProject
... • The pictures will appear before the data and then a smaller image will be included with the data on the next slide. ...
... • The pictures will appear before the data and then a smaller image will be included with the data on the next slide. ...
Long Ago and Far Away
... galaxy’s actual distance to the distance you worked out in Part II#3, estimate the angular size of this galaxy if it were observed at a distance corresponding to 5 billion years after the Big Bang. (The small angle formula breaks down for large cosmological distances, but just assume it works approx ...
... galaxy’s actual distance to the distance you worked out in Part II#3, estimate the angular size of this galaxy if it were observed at a distance corresponding to 5 billion years after the Big Bang. (The small angle formula breaks down for large cosmological distances, but just assume it works approx ...
Gas IN - STScI
... Gas OUT – joining the Hot Gas For ETGs, the ability to sustain a corona of hot, X-ray emitting gas could have played a key role in quenching their past star formation history. An halo of hot gas can indeed act as an effective shield against the acquisition of cold gas and can quickly absorb any ste ...
... Gas OUT – joining the Hot Gas For ETGs, the ability to sustain a corona of hot, X-ray emitting gas could have played a key role in quenching their past star formation history. An halo of hot gas can indeed act as an effective shield against the acquisition of cold gas and can quickly absorb any ste ...
On the role of GRBs on life extinction in the Universe
... center), making it inhospitable to life. Only at the outskirts of the Milky Way, at more than 10 kpc from the galactic center, this probability drops below 50%. When considering the Universe as a whole, the safest environments for life (similar to the one on Earth) are the lowest density regions in ...
... center), making it inhospitable to life. Only at the outskirts of the Milky Way, at more than 10 kpc from the galactic center, this probability drops below 50%. When considering the Universe as a whole, the safest environments for life (similar to the one on Earth) are the lowest density regions in ...
1 UNIT 3 EARTH HISTORY - POSSIBLE TEST QUESTIONS OUR
... 42. How long does it take light from our Sun to arrive to Earth? Classification of Stars 43. Based on temperature and brightness, our Sun is _________. 44. What are the two types of super-giant stars? Fate of Stars 45. Over time, what is the fate of our sun? 46. What might be the fate of our sun if ...
... 42. How long does it take light from our Sun to arrive to Earth? Classification of Stars 43. Based on temperature and brightness, our Sun is _________. 44. What are the two types of super-giant stars? Fate of Stars 45. Over time, what is the fate of our sun? 46. What might be the fate of our sun if ...
Document
... Chandra finds gas at 1kev with density ~ 30 cc in an area of size 10 arcsec surrounding the BH (Baganoff et al. 2001); the capture radius for this gas is ~ 1 arcsec. ...
... Chandra finds gas at 1kev with density ~ 30 cc in an area of size 10 arcsec surrounding the BH (Baganoff et al. 2001); the capture radius for this gas is ~ 1 arcsec. ...
The Formation of a Realistic Disk Galaxy in Lambda Dominated
... 0.15, but with the adopted scheme, the exact value has only a minor effect on the star formation rate (Katz 1992). SNe enrich the surrounding gas according to the respective metal yields. Star particles inherit the metal abundance of the parent gas particles. However, we did not allow for diffusion ...
... 0.15, but with the adopted scheme, the exact value has only a minor effect on the star formation rate (Katz 1992). SNe enrich the surrounding gas according to the respective metal yields. Star particles inherit the metal abundance of the parent gas particles. However, we did not allow for diffusion ...
Supernovae — Oct 21 10/21/2011 • Outline
... Pressure on the walls of the box is caused by the gas hitting the walls. Gas transfers momentum to the walls. Mental picture: Marbles hit the walls; wall pushes back. ...
... Pressure on the walls of the box is caused by the gas hitting the walls. Gas transfers momentum to the walls. Mental picture: Marbles hit the walls; wall pushes back. ...
Gas Accretion is Dominated by Warm Ionized Gas in Milky Way
... Chemical evolution models and analysis of the color magnitude diagram of the Hipparcos dataset indicate the Milky Way has been forming stars at a nearly constant, yet slowly declining, rate of 1–3 M⊙ yr−1 over the past several gigayears (Hernandez et al. 2000; Chiappini et al. 2001, 2003; Fuchs et a ...
... Chemical evolution models and analysis of the color magnitude diagram of the Hipparcos dataset indicate the Milky Way has been forming stars at a nearly constant, yet slowly declining, rate of 1–3 M⊙ yr−1 over the past several gigayears (Hernandez et al. 2000; Chiappini et al. 2001, 2003; Fuchs et a ...
Star Formation
... • Supernova blast waves near clouds can initiate star formation (happened for our own sun, from SNe produced radioactive daughter products in meteorites) • Collapse raises density, core cannot radiate away heat gravitational collapse heat fast enough, and temp rises, until H fusion begins at 10 mill ...
... • Supernova blast waves near clouds can initiate star formation (happened for our own sun, from SNe produced radioactive daughter products in meteorites) • Collapse raises density, core cannot radiate away heat gravitational collapse heat fast enough, and temp rises, until H fusion begins at 10 mill ...
Formation of the Solar System Chapter 8
... The idea that the solar system was born from the collapse of a cloud of dust and gas for proposed by Immanuel Kant (1755) and by Pierre Simon Laplace 40 years later. During the first part of the 20th century, some proposed that the solar system was the result of a near collision of the Sun with anot ...
... The idea that the solar system was born from the collapse of a cloud of dust and gas for proposed by Immanuel Kant (1755) and by Pierre Simon Laplace 40 years later. During the first part of the 20th century, some proposed that the solar system was the result of a near collision of the Sun with anot ...
Cosmology Handouts
... Rainbows reveal that white light is a combination of all the colours. In 1666, Isaac Newton showed that white light could be separated into its component colours using glass prisms. Soon scientists were using this new tool to analyze the light coming from several different light sources. Some scient ...
... Rainbows reveal that white light is a combination of all the colours. In 1666, Isaac Newton showed that white light could be separated into its component colours using glass prisms. Soon scientists were using this new tool to analyze the light coming from several different light sources. Some scient ...
Star formation in galaxies over the last 10 billion
... massive galaxies formed bulk of stars quickly and early, less massive galaxies formed on longer timescales (“Downsizing”) ...
... massive galaxies formed bulk of stars quickly and early, less massive galaxies formed on longer timescales (“Downsizing”) ...
Star Formation in Disks: Spiral Arms, Turbulence, and Triggering
... triggering. Energy types include thermal, magnetic, turbulent, cosmic ray, and rotational. The first four are all comparable and equal to several tenths of an eV cm−3 . Rotational energy is much denser, several hundred eV cm−3 . Of the first four, only supersonic turbulence has been associated with st ...
... triggering. Energy types include thermal, magnetic, turbulent, cosmic ray, and rotational. The first four are all comparable and equal to several tenths of an eV cm−3 . Rotational energy is much denser, several hundred eV cm−3 . Of the first four, only supersonic turbulence has been associated with st ...
HST Key Project to Measure the Hubble Constant from
... in size (get brighter as they grow larger, dim as they shrink) Can’t achieve balance of power welling up from core and power radiating from surface ...
... in size (get brighter as they grow larger, dim as they shrink) Can’t achieve balance of power welling up from core and power radiating from surface ...
Discussion Session A: “Evidence”
... A) Starburst galaxies B) Normal star-‐forming galaxies C) Quiescent galaxies D) Massive galaxies E) Green valley/transi8on galaxies F) All equally likely ...
... A) Starburst galaxies B) Normal star-‐forming galaxies C) Quiescent galaxies D) Massive galaxies E) Green valley/transi8on galaxies F) All equally likely ...
Document
... • High-mass protostars become stars relatively quickly. – They contract quickly due to stronger gravity. – Core becomes hot enough for fusion at a lower density. – High-mass stars are less dense. ...
... • High-mass protostars become stars relatively quickly. – They contract quickly due to stronger gravity. – Core becomes hot enough for fusion at a lower density. – High-mass stars are less dense. ...
Nebulae
... glowing clouds of gas • They are found near hot, luminous stars of spectral types O and B • They are powered by ultraviolet light that they absorb from nearby hot stars • They are composed of ...
... glowing clouds of gas • They are found near hot, luminous stars of spectral types O and B • They are powered by ultraviolet light that they absorb from nearby hot stars • They are composed of ...
The Reflector: January 2010 - Peterborough Astronomical Association
... star birthing area in Sagittarius to two double stars in Cygnus, a million stars in a ball in Hercules, and finally to the final stages of star life in M57 and M27, all in one night. It’s quite a story and you’ll meet a red giant star—Antares—along the way. Planet buffs will also be able to take in ...
... star birthing area in Sagittarius to two double stars in Cygnus, a million stars in a ball in Hercules, and finally to the final stages of star life in M57 and M27, all in one night. It’s quite a story and you’ll meet a red giant star—Antares—along the way. Planet buffs will also be able to take in ...
Galaxies and the Universe
... • Proxima Centauri has a parallax of 0.77 arcseconds. So it is 1/0.77= 1.3 parsecs away. • Sense of scale: – If you make a model where the distance between the Earth and the Sun (1 AU) is an inch, then one light-year is a mile. One parsec is 3.26 miles. – The size of our galaxy, the Milky Way, is ab ...
... • Proxima Centauri has a parallax of 0.77 arcseconds. So it is 1/0.77= 1.3 parsecs away. • Sense of scale: – If you make a model where the distance between the Earth and the Sun (1 AU) is an inch, then one light-year is a mile. One parsec is 3.26 miles. – The size of our galaxy, the Milky Way, is ab ...
Link again
... galaxy and we see a lot of stars and dust and gas when we look toward the disk. We see little dust and few stars when we look away form the disk. The colors of the stars tell us their temperatures. Reddish stars are relatively cool (about 3000 degrees C.). Bluish stars are hot (10,000 degrees C.). O ...
... galaxy and we see a lot of stars and dust and gas when we look toward the disk. We see little dust and few stars when we look away form the disk. The colors of the stars tell us their temperatures. Reddish stars are relatively cool (about 3000 degrees C.). Bluish stars are hot (10,000 degrees C.). O ...
Astronomy
... galaxy and we see a lot of stars and dust and gas when we look toward the disk. We see little dust and few stars when we look away form the disk. The colors of the stars tell us their temperatures. Reddish stars are relatively cool (about 3000 degrees C.). Bluish stars are hot (10,000 degrees C.). O ...
... galaxy and we see a lot of stars and dust and gas when we look toward the disk. We see little dust and few stars when we look away form the disk. The colors of the stars tell us their temperatures. Reddish stars are relatively cool (about 3000 degrees C.). Bluish stars are hot (10,000 degrees C.). O ...
The distribution of the ISM in the Milky Way A three
... emission from the Galaxy by fitting exponential dust distributions to the COBE/DIRBE maps. In this study, the authors find that the best fit could be achieved by assuming that the dust distribution is more extended than that of the stars, namely that the scalelength of the dust is 1.5 times that of ...
... emission from the Galaxy by fitting exponential dust distributions to the COBE/DIRBE maps. In this study, the authors find that the best fit could be achieved by assuming that the dust distribution is more extended than that of the stars, namely that the scalelength of the dust is 1.5 times that of ...