Powerpoint
... a) those heavier than iron, because of supernovae b) iron, formed just before massive stars explode c) odd-numbered nuclei, built with hydrogen fusion d) even-numbered nuclei, built with helium fusion ...
... a) those heavier than iron, because of supernovae b) iron, formed just before massive stars explode c) odd-numbered nuclei, built with hydrogen fusion d) even-numbered nuclei, built with helium fusion ...
Lecture 17 - Yale University
... The Snowplow Phase Initially the shell is pushed forward by the pressure of the hot gas behind the shock. However, cooling continues to a point where the interior pressure becomes negligble. From that point on, the ambient gas is swept up by the inertia of the moving shell. The evolution is now gove ...
... The Snowplow Phase Initially the shell is pushed forward by the pressure of the hot gas behind the shock. However, cooling continues to a point where the interior pressure becomes negligble. From that point on, the ambient gas is swept up by the inertia of the moving shell. The evolution is now gove ...
Galactic Science - Caltech Optical Observatories
... NGAO: Planet detection sensitivity • Very high contrast in near-IR enables imaging of Jovianmass planets around low-mass stars and brown dwarfs. • This can only be done by NGAO. The stars are too optically faint for ExAO ...
... NGAO: Planet detection sensitivity • Very high contrast in near-IR enables imaging of Jovianmass planets around low-mass stars and brown dwarfs. • This can only be done by NGAO. The stars are too optically faint for ExAO ...
Binocular Universe: Summer`s Swan Song
... but he did spot a small clump of starlight a little less than 2° south-southeast of Sadr. Noting its position, he added it as the 29th entry in his famous catalog. Though not one of Messier’s best, M29 is visible through small, hand-supported binoculars as a tiny, rectangular patch of light, with pe ...
... but he did spot a small clump of starlight a little less than 2° south-southeast of Sadr. Noting its position, he added it as the 29th entry in his famous catalog. Though not one of Messier’s best, M29 is visible through small, hand-supported binoculars as a tiny, rectangular patch of light, with pe ...
Populations of Galaxies and their Formation at z < 7
... 3. Galaxies at high redshifts are peculiar and are likely undergoing mergers. The transition from mergers to normal Hubble types occurs at about z~1.5. Calculations show that this picture is consistent with LBGs forming into modern Hubble types. 4. The source(s) of reionization are still unknown. Th ...
... 3. Galaxies at high redshifts are peculiar and are likely undergoing mergers. The transition from mergers to normal Hubble types occurs at about z~1.5. Calculations show that this picture is consistent with LBGs forming into modern Hubble types. 4. The source(s) of reionization are still unknown. Th ...
class 1,F10
... We are on a planet, orbiting a star, in a galaxy (which is a member of the Local Group of galaxies in the Local Supercluster) • How did we come to be? • How can we know what the universe was like in the past? • Can we see the entire universe? ...
... We are on a planet, orbiting a star, in a galaxy (which is a member of the Local Group of galaxies in the Local Supercluster) • How did we come to be? • How can we know what the universe was like in the past? • Can we see the entire universe? ...
Orbital Instabilities in Triaxial Mass Distributions and
... effects are neither dominant nor negligible: Closest approaches of order 1000 AU Disks truncated dynamically to 300 AU Disks truncated via radiation to 40 AU Lifetimes have environmental upper limit Planetary orbits are moderately altered Only a few planetary ejections per cluster These effects must ...
... effects are neither dominant nor negligible: Closest approaches of order 1000 AU Disks truncated dynamically to 300 AU Disks truncated via radiation to 40 AU Lifetimes have environmental upper limit Planetary orbits are moderately altered Only a few planetary ejections per cluster These effects must ...
class 1,S11
... We are on a planet, orbiting a star, in a galaxy (which is a member of the Local Group of galaxies in the Local Supercluster) • How did we come to be? • How can we know what the universe was like in the past? • Can we see the entire universe? ...
... We are on a planet, orbiting a star, in a galaxy (which is a member of the Local Group of galaxies in the Local Supercluster) • How did we come to be? • How can we know what the universe was like in the past? • Can we see the entire universe? ...
From Simulation to Visualization: Astrophysics Goes
... Simulation Details Time Evolution Calculate forces, heating, other changes Update position, velocity, etc. with new values Repeat Data Output Write file of positions, velocities, etc Series of files covering simulation time ...
... Simulation Details Time Evolution Calculate forces, heating, other changes Update position, velocity, etc. with new values Repeat Data Output Write file of positions, velocities, etc Series of files covering simulation time ...
Weighing a Galaxy15 Nov 11/15/2010
... 2. Under influence of the gravity of the sun, a planet moves a given distance. If the time is short, the mass of the sun is greater. Write an equivalent statement for the galaxy NGC 3672. Mass ...
... 2. Under influence of the gravity of the sun, a planet moves a given distance. If the time is short, the mass of the sun is greater. Write an equivalent statement for the galaxy NGC 3672. Mass ...
Powerpoint Presentation (large file)
... 4. How can a neutron star supply energy to a surrounding nebula? 5. What are conditions like inside a neutron star? 6. How are some neutron stars able to spin several hundred times per second? 7. Why do some pulsars emit fantastic amounts of X rays? 8. Are X-ray bursters and novae similar to superno ...
... 4. How can a neutron star supply energy to a surrounding nebula? 5. What are conditions like inside a neutron star? 6. How are some neutron stars able to spin several hundred times per second? 7. Why do some pulsars emit fantastic amounts of X rays? 8. Are X-ray bursters and novae similar to superno ...
Driving downsizing with galaxy groups
... • Gas around satellite galaxies may be shock-heated, tidally- or rampressure stripped • Stripping the cold, dense gas in the disk requires high velocities and ICM densities • The hot halo can perhaps be stripped more easily (Larson, Tinsley & Caldwell 1980) ...
... • Gas around satellite galaxies may be shock-heated, tidally- or rampressure stripped • Stripping the cold, dense gas in the disk requires high velocities and ICM densities • The hot halo can perhaps be stripped more easily (Larson, Tinsley & Caldwell 1980) ...
The Autumn Night Sky
... There is something special within the constellation of Perseus that is worth looking for. It is a star called Algol which, every 68 hours, dims for several hours and brightens again. This can be witnessed with the naked eye so no telescope is required. Due to this behaviour Algol is sometimes referr ...
... There is something special within the constellation of Perseus that is worth looking for. It is a star called Algol which, every 68 hours, dims for several hours and brightens again. This can be witnessed with the naked eye so no telescope is required. Due to this behaviour Algol is sometimes referr ...
Gamma Ray Bursts - University of Arizona
... false by observations • Supranovae predict that the SN outburst occurs BEFORE GRB – also disproved by observations (hard to explain long-duration bursts in any ...
... false by observations • Supranovae predict that the SN outburst occurs BEFORE GRB – also disproved by observations (hard to explain long-duration bursts in any ...
this article
... tremendous rates that they wither into white dwarfs rather than explode as ∙ increases over time as an AGB supernovae. Generally, the mass-loss rate, M, star evolves, and ends in an episode of extremely high mass loss, the superwind (SW) phase (Iben and Renzini 1983; Bowen 1988; Bowen and Willson 19 ...
... tremendous rates that they wither into white dwarfs rather than explode as ∙ increases over time as an AGB supernovae. Generally, the mass-loss rate, M, star evolves, and ends in an episode of extremely high mass loss, the superwind (SW) phase (Iben and Renzini 1983; Bowen 1988; Bowen and Willson 19 ...
File
... From here on earth it is difficult to fathom the huge distances that exist between the stars and planets. The circumference of the earth (38,500 km) may seem like a long way to us but is an insignificant distance in space. The nearest celestial object to earth, the moon, is approximately 400, 000 km ...
... From here on earth it is difficult to fathom the huge distances that exist between the stars and planets. The circumference of the earth (38,500 km) may seem like a long way to us but is an insignificant distance in space. The nearest celestial object to earth, the moon, is approximately 400, 000 km ...
AST 207 7 Homew
... L on Deneb b. Here you will w find out wh hat it means tto live near a ggiant like Denneb. Recall thhat the lu uminosity of a star , where T is its temperaature and R iss its radius. Abs. mag. Diistance (pc) Appp. Mag. A ...
... L on Deneb b. Here you will w find out wh hat it means tto live near a ggiant like Denneb. Recall thhat the lu uminosity of a star , where T is its temperaature and R iss its radius. Abs. mag. Diistance (pc) Appp. Mag. A ...
Astronomy 114 – Summary of Important Concepts #2 1 Stars: key
... (hydrogen nuclei) and becomes significant at temperatures of around 10 million K. The p-p chain of reactions ultimately forms 4 He from 4 H. The atomic weights do not exactly match because the more exact weight of the proton is 1.0078 (in atomic mass units) and four of them add to 4.0312, while the ...
... (hydrogen nuclei) and becomes significant at temperatures of around 10 million K. The p-p chain of reactions ultimately forms 4 He from 4 H. The atomic weights do not exactly match because the more exact weight of the proton is 1.0078 (in atomic mass units) and four of them add to 4.0312, while the ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.