Star Formation in the Galactic Center
... ‘normal’ (Nayakshin et al (2005) star formation at several parsecs away from GC in a massive cluster that then spirals in. This would avoid the need for excessive gas density in order to form stars. Cluster would orbit through background stars, decay through friction, and settle in center cont ...
... ‘normal’ (Nayakshin et al (2005) star formation at several parsecs away from GC in a massive cluster that then spirals in. This would avoid the need for excessive gas density in order to form stars. Cluster would orbit through background stars, decay through friction, and settle in center cont ...
talk.wyse - Johns Hopkins University
... In ΛCDM the first scales to form are small, and galaxies like the Milky Way evolve through merging and assimilation of smaller systems. Highest resolution N-body simulations (gravity only) show persistent small-scale substructure, with many more darkmatter subhaloes surviving to the present-day than ...
... In ΛCDM the first scales to form are small, and galaxies like the Milky Way evolve through merging and assimilation of smaller systems. Highest resolution N-body simulations (gravity only) show persistent small-scale substructure, with many more darkmatter subhaloes surviving to the present-day than ...
observing the universe
... A galaxy is an assembly of between a billion (109) and a hundred billion (1011) stars. There is often a large amount of dust and gas intermingled, all held together by gravity. The Sun and Earth are in the Milky Way Galaxy. Galaxies have many different characteristics, but the easiest way to classif ...
... A galaxy is an assembly of between a billion (109) and a hundred billion (1011) stars. There is often a large amount of dust and gas intermingled, all held together by gravity. The Sun and Earth are in the Milky Way Galaxy. Galaxies have many different characteristics, but the easiest way to classif ...
Stellar Evolution Game (PDF: 112k)
... 1. Teach students to read an HR diagram. Students will need to use this information to answer the questions during the game. 2. Students will also need to be knowledgeable about basic stellar evolution pathways for stars based on their masses. 3. Copy a set of the game cards on matching colored pape ...
... 1. Teach students to read an HR diagram. Students will need to use this information to answer the questions during the game. 2. Students will also need to be knowledgeable about basic stellar evolution pathways for stars based on their masses. 3. Copy a set of the game cards on matching colored pape ...
Carolina Kehrig
... Observations versus HeII-ionizing fluxes from radiation-driven wind models for the most massive, hottest O stars at the metallicity of IZw18 and below (Kudritzki 2002): the number of such stars needed to explain Q(HeII)obs implies a cluster mass ~ 10 - 20 x Mstar of the NW knot of IZw18 These models ...
... Observations versus HeII-ionizing fluxes from radiation-driven wind models for the most massive, hottest O stars at the metallicity of IZw18 and below (Kudritzki 2002): the number of such stars needed to explain Q(HeII)obs implies a cluster mass ~ 10 - 20 x Mstar of the NW knot of IZw18 These models ...
– 1 – 1. Historical Notes for Ay 123 1.1.
... achieved in physics laboratories on the Earth, and hence by studying the properties of stars we probe regimes of physical parameters that cannot be reached any other way. The opposite extreme is often reached in the interstellar medium, same idea. Temperature T(ISM) ∼ 3 − 10K, T(Sun, center) ∼ 20 × ...
... achieved in physics laboratories on the Earth, and hence by studying the properties of stars we probe regimes of physical parameters that cannot be reached any other way. The opposite extreme is often reached in the interstellar medium, same idea. Temperature T(ISM) ∼ 3 − 10K, T(Sun, center) ∼ 20 × ...
Lecture 24, The local group
... One possibility is that about 10% of halos that are small now (Vc < 30 km/s) were much larger at z > 2, but suffer tidal stripping in the hierarchical merging process. The MW dSph formed in such objects with M > 109 M , so were able to build up some stellar mass and survive reionization despit ...
... One possibility is that about 10% of halos that are small now (Vc < 30 km/s) were much larger at z > 2, but suffer tidal stripping in the hierarchical merging process. The MW dSph formed in such objects with M > 109 M , so were able to build up some stellar mass and survive reionization despit ...
A Hero`s Little Horse: Discovery of a Dissolving Star Cluster in
... We report the discovery of an ultra-faint stellar system in the constellation of Pegasus. This concentration of stars was detected by applying our overdensity detection algorithm to the SDSS-DR10 and confirmed with deeper photometry from the Dark Energy Camera at the 4-m Blanco telescope. The best-f ...
... We report the discovery of an ultra-faint stellar system in the constellation of Pegasus. This concentration of stars was detected by applying our overdensity detection algorithm to the SDSS-DR10 and confirmed with deeper photometry from the Dark Energy Camera at the 4-m Blanco telescope. The best-f ...
Components of the Milky Way
... Gas in the Milky Way exists in different phases: • Molecular gas (T = 10 - 100 K) • Atomic hydrogen (neutral gas, called H I) • Ionized gas (called H II) Most of the gas is in atomic form, but stars form out of the ...
... Gas in the Milky Way exists in different phases: • Molecular gas (T = 10 - 100 K) • Atomic hydrogen (neutral gas, called H I) • Ionized gas (called H II) Most of the gas is in atomic form, but stars form out of the ...
ASTR-1020: Astronomy II Course Lecture Notes - Faculty
... e) Population I star Cepheids (called Type I or classical Cepheids) have a slightly different period-luminosity relationship than the Population II star cepheids (called Type II Cepheids or W Virginis stars). 3. Lower mass versions of Cepheids exist called RR Lyrae type variables, which change in br ...
... e) Population I star Cepheids (called Type I or classical Cepheids) have a slightly different period-luminosity relationship than the Population II star cepheids (called Type II Cepheids or W Virginis stars). 3. Lower mass versions of Cepheids exist called RR Lyrae type variables, which change in br ...
Core-collapse supernovae and their massive progenitors
... of the collapse of an 11 M⊙ star and followed accretion onto the proto-neutron star beyond 500 ms after the bounce (figure 4). An acoustic oscillation arises at 200 ms and the power generated by the oscillating core is enough to drive the explosion. This mechanism was not identified previously as mo ...
... of the collapse of an 11 M⊙ star and followed accretion onto the proto-neutron star beyond 500 ms after the bounce (figure 4). An acoustic oscillation arises at 200 ms and the power generated by the oscillating core is enough to drive the explosion. This mechanism was not identified previously as mo ...
Acting Out the Life Cycle of Stars - University of Texas Astronomy
... As a class, we’re going to act out the life cycle of stars. Each of you will represent a small clump of gas, mostly made of hydrogen (since that’s by far the most abundant element in the Universe). a. We all start in random motion, wandering around aimlessly, mostly ignoring all other clumps of gas. ...
... As a class, we’re going to act out the life cycle of stars. Each of you will represent a small clump of gas, mostly made of hydrogen (since that’s by far the most abundant element in the Universe). a. We all start in random motion, wandering around aimlessly, mostly ignoring all other clumps of gas. ...
Quasars: Back to the Infant Universe
... Active supermassive black holes (AGN) in the centers of nearby galaxies… ...
... Active supermassive black holes (AGN) in the centers of nearby galaxies… ...
OGU - What`s Out Tonight?
... galaxies, there is little gas and dust to form new stars. A second type of galaxy is the spiral, which resembles its name. The galaxy that we live in, the Milky Way Galaxy, is a spiral. Spirals are flatter looking, like a dish. They have round bulged centers out of which curved arms radiate. Spirals ...
... galaxies, there is little gas and dust to form new stars. A second type of galaxy is the spiral, which resembles its name. The galaxy that we live in, the Milky Way Galaxy, is a spiral. Spirals are flatter looking, like a dish. They have round bulged centers out of which curved arms radiate. Spirals ...
journey to the stars - American Museum of Natural History
... But not just the Sun. Like most stars, the Sun formed in a tightly packed group of stars called a cluster. The brightest young stars in the Sun’s cluster lit and heated this pocket within its birth cloud. If we speed up time, we can see the intense light of these bright stars driving the cloud away ...
... But not just the Sun. Like most stars, the Sun formed in a tightly packed group of stars called a cluster. The brightest young stars in the Sun’s cluster lit and heated this pocket within its birth cloud. If we speed up time, we can see the intense light of these bright stars driving the cloud away ...
$doc.title
... Starburst can drive winds of enriched gas (e.g., from supernova ejecta) out to the intergalactic medium. This gas can then be accreted again by galaxies. In a disk galaxy, the winds are generally bipolar outflows ...
... Starburst can drive winds of enriched gas (e.g., from supernova ejecta) out to the intergalactic medium. This gas can then be accreted again by galaxies. In a disk galaxy, the winds are generally bipolar outflows ...
Our galaxy is the centre of the universe
... redshifts as being caused mainly by velocities. Figure 4 shows more recent data on the redshift-distance relation out to much greater distances.7 Deviations from the trend line would be caused not by expansion, but by other phenomena, such as the Doppler effect. For example, galaxy M31 in Andromeda ...
... redshifts as being caused mainly by velocities. Figure 4 shows more recent data on the redshift-distance relation out to much greater distances.7 Deviations from the trend line would be caused not by expansion, but by other phenomena, such as the Doppler effect. For example, galaxy M31 in Andromeda ...
Surveying the Stars
... •Apparent positions of the nearest stars shift by only about an arcsecond as Earth orbits the Sun, and the shift is smaller for more distant stars. •These very small angles explain why the Greeks were unable to detect parallax with their naked eyes. •This inability helped delay the acceptance of the ...
... •Apparent positions of the nearest stars shift by only about an arcsecond as Earth orbits the Sun, and the shift is smaller for more distant stars. •These very small angles explain why the Greeks were unable to detect parallax with their naked eyes. •This inability helped delay the acceptance of the ...
pdf of paper
... the most abW1dant dements formed in stars. The many collisions of protons with helium atoms do not give rise to significant fusion products. Lithiwn, beryllium and boron-the nuclei of which are smaller than those of carbon-are a million times less ablUldant than carbon. Thus, abundances of elements ...
... the most abW1dant dements formed in stars. The many collisions of protons with helium atoms do not give rise to significant fusion products. Lithiwn, beryllium and boron-the nuclei of which are smaller than those of carbon-are a million times less ablUldant than carbon. Thus, abundances of elements ...
Transcript - Chandra X
... are more diverse and complicated than this diagram would lead you to believe. For instance, there are many more stellar classes than OBAFGKM; however for simplicity’s sake, only the classes that contain a large majority are shown. Absolute magnitude – the intrinsic brightness of stars – is similar ...
... are more diverse and complicated than this diagram would lead you to believe. For instance, there are many more stellar classes than OBAFGKM; however for simplicity’s sake, only the classes that contain a large majority are shown. Absolute magnitude – the intrinsic brightness of stars – is similar ...
Lesson Plan - ScienceA2Z.com
... The idea is that elliptical galaxy or spiral galaxy will form, depending upon when star formation occurs in the galaxy formation process. Because stars are small and they are far apart, they don't collide in the formation process. This allows the stars to maintain "roughly" their initial shape and t ...
... The idea is that elliptical galaxy or spiral galaxy will form, depending upon when star formation occurs in the galaxy formation process. Because stars are small and they are far apart, they don't collide in the formation process. This allows the stars to maintain "roughly" their initial shape and t ...
Ch17_lecture
... Galaxy Clusters • In general, all clusters need dark matter to explain galactic motions and the confinement of hot intergalactic gas within cluster • Near clusters appear to have their members fairly smoothly spread out, while far away clusters (and hence younger clusters) are more ragged looking – ...
... Galaxy Clusters • In general, all clusters need dark matter to explain galactic motions and the confinement of hot intergalactic gas within cluster • Near clusters appear to have their members fairly smoothly spread out, while far away clusters (and hence younger clusters) are more ragged looking – ...
Chapter 17 Galaxies Galaxies Early Observations
... Galaxy Distances • Galaxy distances are too far to employ the parallax technique • The method of “standard candles” is used • The standard candles are usually Cepheid variables, supergiant stars, planetary nebulas, supernovas, etc. ...
... Galaxy Distances • Galaxy distances are too far to employ the parallax technique • The method of “standard candles” is used • The standard candles are usually Cepheid variables, supergiant stars, planetary nebulas, supernovas, etc. ...
Our galaxy is the centre of the universe, `quantized` red shifts show
... thinking of the redshifts as being caused mainly by velocities. Figure 4 shows more recent data on the redshift-distance relation out to much greater distances.7 Deviations from the trend line would be caused not by expansion, but by other phenomena, such as the Doppler effect. For example, galaxy M ...
... thinking of the redshifts as being caused mainly by velocities. Figure 4 shows more recent data on the redshift-distance relation out to much greater distances.7 Deviations from the trend line would be caused not by expansion, but by other phenomena, such as the Doppler effect. For example, galaxy M ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.