A105 Stars and Galaxies
... What about Massive Stars? • Massive stars continue to generate energy by nuclear reactions until they have converted all the hydrogen and helium in their cores into iron. • Once the core is iron, no more energy can be generated • The core collapses and the star explodes ...
... What about Massive Stars? • Massive stars continue to generate energy by nuclear reactions until they have converted all the hydrogen and helium in their cores into iron. • Once the core is iron, no more energy can be generated • The core collapses and the star explodes ...
The Final Flight of Atlantis - Westchester Amateur Astronomers
... Star clusters are important because, within each cluster, member stars are probably at the same distance from the Sun, and have the same age and the same initial chemical composition. So, the study of globular clusters has now become an indispensable tool for astronomers specializing in stellar evol ...
... Star clusters are important because, within each cluster, member stars are probably at the same distance from the Sun, and have the same age and the same initial chemical composition. So, the study of globular clusters has now become an indispensable tool for astronomers specializing in stellar evol ...
ISM and star formation
... Such short-lived stars spend all their lives in the stellar nursery of their birth, so emission nebulae mark sites of ongoing star formation. Many stars of lower mass are forming too, but make few UV photons. ...
... Such short-lived stars spend all their lives in the stellar nursery of their birth, so emission nebulae mark sites of ongoing star formation. Many stars of lower mass are forming too, but make few UV photons. ...
HIGH RESOLTION SPH SIMULATIONS OF GALAXY CLUSTERS
... Spatial smoothing= 0.5 kpc Different feedback params. ...
... Spatial smoothing= 0.5 kpc Different feedback params. ...
instructor notes stellar evolution, star clusters
... Another method of determining distances to late-type stars is by means of the Wilson-Bappu effect, namely that the width of the central emission component of the Ca II K line in G and K-type stars is directly related to the absolute magnitude of the star — the broader the emission line width, denot ...
... Another method of determining distances to late-type stars is by means of the Wilson-Bappu effect, namely that the width of the central emission component of the Ca II K line in G and K-type stars is directly related to the absolute magnitude of the star — the broader the emission line width, denot ...
instructor notes stellar evolution, star clusters
... Another method of determining distances to late-type stars is by means of the Wilson-Bappu effect, namely that the width of the central emission component of the Ca II K line in G and K-type stars is directly related to the absolute magnitude of the star — the broader the emission line width, denot ...
... Another method of determining distances to late-type stars is by means of the Wilson-Bappu effect, namely that the width of the central emission component of the Ca II K line in G and K-type stars is directly related to the absolute magnitude of the star — the broader the emission line width, denot ...
The Milky Way Galaxy
... Dust is generated in the late stages of low and high mass stars, when carbon and silicon is dredged up from the cores and ejected in stellar winds, planetary nebulae, and possibly supernova remnants. The blocking of visible light by dust is called dust extinction. ...
... Dust is generated in the late stages of low and high mass stars, when carbon and silicon is dredged up from the cores and ejected in stellar winds, planetary nebulae, and possibly supernova remnants. The blocking of visible light by dust is called dust extinction. ...
Abstract book
... rapid dynamical evolution once the cores collapsed. To this aim, we have analyzed the population of dense cores in the Pipe cold molecular cloud, based on the catalogue tailored by Román-Zuñiga and collaborators. Mass-Core Function (MCF) and Density-Core Function (DCF) can be very well represented b ...
... rapid dynamical evolution once the cores collapsed. To this aim, we have analyzed the population of dense cores in the Pipe cold molecular cloud, based on the catalogue tailored by Román-Zuñiga and collaborators. Mass-Core Function (MCF) and Density-Core Function (DCF) can be very well represented b ...
AST101_lect_12
... to refill the gas tank in your car. Time remaining is the amount of fuel you have (the size of the tank) by your average usage (gallons per day). ...
... to refill the gas tank in your car. Time remaining is the amount of fuel you have (the size of the tank) by your average usage (gallons per day). ...
Test #4
... 1. The location of the center of the Galaxy is determined by observations of: a) Cepheids variables, b) Globular clusters, c) The spiral arms, d) A visually bright, massive, object around which all objects in the Galaxy move. 2. What two observations of an object allow for a determination of the Mil ...
... 1. The location of the center of the Galaxy is determined by observations of: a) Cepheids variables, b) Globular clusters, c) The spiral arms, d) A visually bright, massive, object around which all objects in the Galaxy move. 2. What two observations of an object allow for a determination of the Mil ...
Distance
... parameters are more accurate than for single star • (b) All stars are of the same age. Star clusters are the only objects that enable direct age estimate, study of the galactic evolution and the star-formation history • (c) All stars have nearly the same chemical composition, and the differences in ...
... parameters are more accurate than for single star • (b) All stars are of the same age. Star clusters are the only objects that enable direct age estimate, study of the galactic evolution and the star-formation history • (c) All stars have nearly the same chemical composition, and the differences in ...
Слайд 1 - Tuorla Observatory
... parameters are more accurate than for single star • (b) All stars are of the same age. Star clusters are the only objects that enable direct age estimate, study of the galactic evolution and the star-formation history • (c) All stars have nearly the same chemical composition, and the differences in ...
... parameters are more accurate than for single star • (b) All stars are of the same age. Star clusters are the only objects that enable direct age estimate, study of the galactic evolution and the star-formation history • (c) All stars have nearly the same chemical composition, and the differences in ...
Manual - TUM
... index ; that is, the difference in magnitudes of a star in two different filters (e.g. B-V or V-R). It is the observational equivalent of a Hertzsprung-Russell diagram (HRD) 1 . On a HRD, absolute magnitude or luminosity is plotted increasing up the vertical axis and spectral type or temperature (re ...
... index ; that is, the difference in magnitudes of a star in two different filters (e.g. B-V or V-R). It is the observational equivalent of a Hertzsprung-Russell diagram (HRD) 1 . On a HRD, absolute magnitude or luminosity is plotted increasing up the vertical axis and spectral type or temperature (re ...
Magnetic Fields in the ICM and IGM from Active Galaxies
... 1. Diffused Radio Emission: Distribution and strength of cosmic magnetic fields, seeding from first stars, dwarf galaxies, AGN feedbacks, or (turbulent) dynamo. 2. Differential FRM of jet pc-kpc scale: is there current? 3. Clusters as magnetic field laboratories: Structure formation, AGNs, heating, ...
... 1. Diffused Radio Emission: Distribution and strength of cosmic magnetic fields, seeding from first stars, dwarf galaxies, AGN feedbacks, or (turbulent) dynamo. 2. Differential FRM of jet pc-kpc scale: is there current? 3. Clusters as magnetic field laboratories: Structure formation, AGNs, heating, ...
Chapter 5 Galaxies and Star Systems
... systems, star clusters, dust, and gas bound together by gravity. There are billions of galaxies in the universe. The largest galaxies have more than a trillion stars! Astronomers classify most galaxies into the following types: spiral, elliptical, and irregular. Spiral galaxies are those that appear ...
... systems, star clusters, dust, and gas bound together by gravity. There are billions of galaxies in the universe. The largest galaxies have more than a trillion stars! Astronomers classify most galaxies into the following types: spiral, elliptical, and irregular. Spiral galaxies are those that appear ...
PH607 – Galaxies
... The Milky Way: course begins by considering the largescale structure of our own Galaxy. The Local Group: We then go on to consider how the Milky Way fits in with what we see in other galaxies, and what the morphologies of these systems tell us about their ...
... The Milky Way: course begins by considering the largescale structure of our own Galaxy. The Local Group: We then go on to consider how the Milky Way fits in with what we see in other galaxies, and what the morphologies of these systems tell us about their ...
July - astra
... cury, Venus, Mars, Jupiter and Saturn. Venus is extremely bright Open clusters reside in our Milky Way Galaxy. Our Sun is no and hugs close to the Sun, so you see it for a short time in the longer in its group. west after sunset or in the east before sunrise. Jupiter can be out Globular Clusters loo ...
... cury, Venus, Mars, Jupiter and Saturn. Venus is extremely bright Open clusters reside in our Milky Way Galaxy. Our Sun is no and hugs close to the Sun, so you see it for a short time in the longer in its group. west after sunset or in the east before sunrise. Jupiter can be out Globular Clusters loo ...
charts_set_9
... - contains young and old stars, gas, dust. Has spiral structure - vertical thickness roughly 100 pc - 2 kpc (depending on component. Most gas and dust in thinner layer, most stars in thicker layer) ...
... - contains young and old stars, gas, dust. Has spiral structure - vertical thickness roughly 100 pc - 2 kpc (depending on component. Most gas and dust in thinner layer, most stars in thicker layer) ...
Activity: Stellar Evolution Scavenger Hunt - Chandra X
... These clusters are among the brightest, densest, and closest of those containing moderately massive stars. Intervening dust from the Milky Way's disk slightly obscures our view, dimming the pair's overall brightness by about a factor of five. The two clusters (known as NGC 884 and NGC 869) are strik ...
... These clusters are among the brightest, densest, and closest of those containing moderately massive stars. Intervening dust from the Milky Way's disk slightly obscures our view, dimming the pair's overall brightness by about a factor of five. The two clusters (known as NGC 884 and NGC 869) are strik ...
Chapter 13
... 1. Stars are born in the cold (20K), giant molecular clouds (GMCs) found in the Galaxy. Astronomers estimate that our Galaxy contains 5,000 GMCs. 2. The average density of a GMC is about 200 molecules/cm3; a typical cloud may be 50 pc across and contain as much as a million solar masses of material. ...
... 1. Stars are born in the cold (20K), giant molecular clouds (GMCs) found in the Galaxy. Astronomers estimate that our Galaxy contains 5,000 GMCs. 2. The average density of a GMC is about 200 molecules/cm3; a typical cloud may be 50 pc across and contain as much as a million solar masses of material. ...
Chapter 14 The Milky Way Galaxy
... • RR Lyrae stars all have about the same luminosity; knowing their apparent magnitude allows us to calculate the distance. • Cepheids have a luminosity that is strongly correlated with the period of their oscillations; once the period is measured, the luminosity is known and we can proceed as above. ...
... • RR Lyrae stars all have about the same luminosity; knowing their apparent magnitude allows us to calculate the distance. • Cepheids have a luminosity that is strongly correlated with the period of their oscillations; once the period is measured, the luminosity is known and we can proceed as above. ...
Globular Clusters
... cluster of stars stretching far from the bright core. This is another big one. Unfortunately 47 Tuc does not easily resolve into stars with smaller scopes. The Pavo glob and M22 are a bit easier. NGC 362 is near 47 tuc, at the Achernar end of the SMC, on the 47 Tuc side. It's half the size, twice th ...
... cluster of stars stretching far from the bright core. This is another big one. Unfortunately 47 Tuc does not easily resolve into stars with smaller scopes. The Pavo glob and M22 are a bit easier. NGC 362 is near 47 tuc, at the Achernar end of the SMC, on the 47 Tuc side. It's half the size, twice th ...
Physics - Content by Unit
... time less than an orbital period, most of the mass points would collapse to a bar-shaped, dense concentration close to the center of the galaxy with only a few mass points at larger radii. This looked nothing like the elegant spiral or elliptical shapes we are used to seeing. However, if they added ...
... time less than an orbital period, most of the mass points would collapse to a bar-shaped, dense concentration close to the center of the galaxy with only a few mass points at larger radii. This looked nothing like the elegant spiral or elliptical shapes we are used to seeing. However, if they added ...
Space astrometry 2: Scientific results from Hipparcos
... • resonance due to rotating bar: Hercules stream (Dehnen 1998) • other moving groups: • Castor: 0.2 Gyr (Barrado y Navascues 1998, Montes et al 2001) • Ursa Major: 0.3 Gyr (Eggen 1998, Chupina et al 2001, King et al 2003) • HR 1614: 2-6 Gyr (Eggen 1998, Feltzing & Holmberg 2000) ...
... • resonance due to rotating bar: Hercules stream (Dehnen 1998) • other moving groups: • Castor: 0.2 Gyr (Barrado y Navascues 1998, Montes et al 2001) • Ursa Major: 0.3 Gyr (Eggen 1998, Chupina et al 2001, King et al 2003) • HR 1614: 2-6 Gyr (Eggen 1998, Feltzing & Holmberg 2000) ...
Open cluster
An open cluster, also known as galactic cluster, is a group of up to a few thousand stars that were formed from the same giant molecular cloud and have roughly the same age. More than 1,100 open clusters have been discovered within the Milky Way Galaxy, and many more are thought to exist. They are loosely bound by mutual gravitational attraction and become disrupted by close encounters with other clusters and clouds of gas as they orbit the galactic center, resulting in a migration to the main body of the galaxy as well as a loss of cluster members through internal close encounters. Open clusters generally survive for a few hundred million years, with the most massive ones surviving for a few billion years. In contrast, the more massive globular clusters of stars exert a stronger gravitational attraction on their members, and can survive for longer. Open clusters have been found only in spiral and irregular galaxies, in which active star formation is occurring.Young open clusters may still be contained within the molecular cloud from which they formed, illuminating it to create an H II region. Over time, radiation pressure from the cluster will disperse the molecular cloud. Typically, about 10% of the mass of a gas cloud will coalesce into stars before radiation pressure drives the rest of the gas away.Open clusters are key objects in the study of stellar evolution. Because the cluster members are of similar age and chemical composition, their properties (such as distance, age, metallicity and extinction) are more easily determined than they are for isolated stars. A number of open clusters, such as the Pleiades, Hyades or the Alpha Persei Cluster are visible with the naked eye. Some others, such as the Double Cluster, are barely perceptible without instruments, while many more can be seen using binoculars or telescopes. The Wild Duck Cluster, M11, is an example.