Homework #9 - Solutions - Department of Physics and Astronomy
... in the Pleiades star cluster The Pleiades star cluster is a young open star cluster located in the spiral arms, thus we would expect population I stars. d) in intergalactic space (beyond the halo) We would expect to see only old extreme population II stars (and possibly population III stars which ar ...
... in the Pleiades star cluster The Pleiades star cluster is a young open star cluster located in the spiral arms, thus we would expect population I stars. d) in intergalactic space (beyond the halo) We would expect to see only old extreme population II stars (and possibly population III stars which ar ...
Death of Stars
... fusion of four Hydrogen nuclei to form a He nucleus and conversion of mass to energy The energy appears as K.E of the particles formed, high energy gamma rays and neutrinos The temperature of the star’s core ...
... fusion of four Hydrogen nuclei to form a He nucleus and conversion of mass to energy The energy appears as K.E of the particles formed, high energy gamma rays and neutrinos The temperature of the star’s core ...
Starry Night¨ Times - October 2008
... they're not connected in any way: M46 hangs in space about 5,000 lightyears distant, while M47 is closer at 1,700 lightyears. Of special interest is the planetary nebula that seems to be embedded near M46's center. Although the nebula is probably not actually part of the cluster (it simply lies alon ...
... they're not connected in any way: M46 hangs in space about 5,000 lightyears distant, while M47 is closer at 1,700 lightyears. Of special interest is the planetary nebula that seems to be embedded near M46's center. Although the nebula is probably not actually part of the cluster (it simply lies alon ...
September Evening Skies
... separation, are ζ UMa, δ Lyr, α Cap, ο Cyg, ε Lyr, ν Dra, ζ Lyr, β Cyg. ...
... separation, are ζ UMa, δ Lyr, α Cap, ο Cyg, ε Lyr, ν Dra, ζ Lyr, β Cyg. ...
Integrative Studies 410 Our Place in the Universe
... • Classic example: Great Hercules Cluster (M13) • Spherical clusters • may contain millions of stars • Old stars • Great tool to study stellar life cycle ...
... • Classic example: Great Hercules Cluster (M13) • Spherical clusters • may contain millions of stars • Old stars • Great tool to study stellar life cycle ...
Handout from Allaire Star Party
... closest stars? Imagine now that the Sun is shrunk even further, to the size of an orange. The nearest star to the Sun, Alpha Centauri (actually a three star system), would be another orange about a thousand miles away – the distance from New York to St. Louis. We live in a collection of about 200 bi ...
... closest stars? Imagine now that the Sun is shrunk even further, to the size of an orange. The nearest star to the Sun, Alpha Centauri (actually a three star system), would be another orange about a thousand miles away – the distance from New York to St. Louis. We live in a collection of about 200 bi ...
22 October: The Formation of Stars
... • Now, how to stars form? What do they form from? Space seems to be empty. Where does the material come from? ...
... • Now, how to stars form? What do they form from? Space seems to be empty. Where does the material come from? ...
The Milky Way – A Classic Galaxy
... • Could see the brightest individual stars. Among them, variables of the right color and light variation to show them as Cepheids • Therefore, this was not a nearby nebula around a new star, it was an entire galaxy. • Herschel’s map then could be seen as a map of our own Milky Way Galaxy ...
... • Could see the brightest individual stars. Among them, variables of the right color and light variation to show them as Cepheids • Therefore, this was not a nearby nebula around a new star, it was an entire galaxy. • Herschel’s map then could be seen as a map of our own Milky Way Galaxy ...
Document
... • What causes the mass to keep on increasing? • Don’t see anything there. Thus “dark” matter. ...
... • What causes the mass to keep on increasing? • Don’t see anything there. Thus “dark” matter. ...
Milky Way
... • What causes the mass to keep on increasing? • Don’t see anything there. Thus “dark” matter. ...
... • What causes the mass to keep on increasing? • Don’t see anything there. Thus “dark” matter. ...
SSG Coordinators will be at the Cronan Ranch observing site at 5
... galaxy is tilted about 30 to our line of sight. With about 300 billion stars spread across a 130,000 light year disk, this is an object worth spending some time with. Of interest is that M31 is approaching us at about 185 miles per second. In about 5 billion years the two galaxies will collide and ...
... galaxy is tilted about 30 to our line of sight. With about 300 billion stars spread across a 130,000 light year disk, this is an object worth spending some time with. Of interest is that M31 is approaching us at about 185 miles per second. In about 5 billion years the two galaxies will collide and ...
every star in the cluster.
... This is just one relatively brief stage on the way to stellar demise. The globular cluster in the figure just above has a lot of red giants, continually forming from evolving stars near the turnoff. But there were originally many stars that were even more massive, that became red giants for a time, ...
... This is just one relatively brief stage on the way to stellar demise. The globular cluster in the figure just above has a lot of red giants, continually forming from evolving stars near the turnoff. But there were originally many stars that were even more massive, that became red giants for a time, ...
8 clusters stellar evo
... What we found in star clusters: Small stars live longer Very massive stars live hard and die young Old stars leave the main sequence to become red giants. ...
... What we found in star clusters: Small stars live longer Very massive stars live hard and die young Old stars leave the main sequence to become red giants. ...
Ages of Star Clusters - Indiana University Astronomy
... sequence sooner. In a cluster in which all the stars formed at the same time, the stars “peel off” the main sequence from the top, leaving only progressively less and less massive stars remaining on the main sequence as time goes by. The main sequence turnoff is the point on the main sequence for wh ...
... sequence sooner. In a cluster in which all the stars formed at the same time, the stars “peel off” the main sequence from the top, leaving only progressively less and less massive stars remaining on the main sequence as time goes by. The main sequence turnoff is the point on the main sequence for wh ...
Spectral Class and Colour index
... Spectral Class and Colour index As we have seen the colour of a star is related to its temperature as a consequence of Wien’s law. λmaxT = constant The spectral class (OBAFGKM) of a main sequence star is also a direct result of its temperature. One (relatively crude) way of determining the temperatu ...
... Spectral Class and Colour index As we have seen the colour of a star is related to its temperature as a consequence of Wien’s law. λmaxT = constant The spectral class (OBAFGKM) of a main sequence star is also a direct result of its temperature. One (relatively crude) way of determining the temperatu ...
Lecture 10: The Milky Way
... This gives us the absolute luminosities of low-mass stars, and using binary systems we can calibrate our models to true masses and radii (see earlier). The trouble is that within 100pc we have no massive stars and only 4 giants – how do we calibrate these? To get distances to objects further away we ...
... This gives us the absolute luminosities of low-mass stars, and using binary systems we can calibrate our models to true masses and radii (see earlier). The trouble is that within 100pc we have no massive stars and only 4 giants – how do we calibrate these? To get distances to objects further away we ...
Pallavicini - IASF Milano
... On the basis of ROSAT observations a much lower detection rate of cluster sources was reported for Praesepe than for the Hyades (Randich & Schmitt 1995) suggesting that a cluster of a given age may not be representative of all clusters with the same age. Age 600 Myr, metallicity about solar Combined ...
... On the basis of ROSAT observations a much lower detection rate of cluster sources was reported for Praesepe than for the Hyades (Randich & Schmitt 1995) suggesting that a cluster of a given age may not be representative of all clusters with the same age. Age 600 Myr, metallicity about solar Combined ...
The Ursa Major Moving Cluster, Collinder 285
... escaped due to mutual encounters, tidal forces of the Milky Way, or encounters with large interstellar clouds and other clusters. Now as they have left the cluster, their orbits around the Milky Way Galaxy's center is still similar to that of the cluster so that they have a common motion. All these ...
... escaped due to mutual encounters, tidal forces of the Milky Way, or encounters with large interstellar clouds and other clusters. Now as they have left the cluster, their orbits around the Milky Way Galaxy's center is still similar to that of the cluster so that they have a common motion. All these ...
Early Spring Observing – Millstone News Night Sky
... The Beehive contains a larger star population than most other nearby clusters. Under dark skies the Beehive Cluster looks like a nebulous object to the naked eye; thus it has been known since ancient times. We often find it, rather than the constellation it is found in (Cancer). From Wikipedia: The ...
... The Beehive contains a larger star population than most other nearby clusters. Under dark skies the Beehive Cluster looks like a nebulous object to the naked eye; thus it has been known since ancient times. We often find it, rather than the constellation it is found in (Cancer). From Wikipedia: The ...
Galaxy clusters - University of Iowa Astrophysics
... • From this, the amount of X-ray emitting gas can be calculated to be 2×1014 M • The mass of X-ray emitting gas is greater than the mass in all the stars in all the galaxies in the cluster and about 10% of the total mass. ...
... • From this, the amount of X-ray emitting gas can be calculated to be 2×1014 M • The mass of X-ray emitting gas is greater than the mass in all the stars in all the galaxies in the cluster and about 10% of the total mass. ...
Galaxy clusters - University of Iowa Astrophysics
... • From this, the amount of X-ray emitting gas can be calculated to be 2×1014 M • The mass of X-ray emitting gas is greater than the mass in all the stars in all the galaxies in the cluster and about 10% of the total mass. ...
... • From this, the amount of X-ray emitting gas can be calculated to be 2×1014 M • The mass of X-ray emitting gas is greater than the mass in all the stars in all the galaxies in the cluster and about 10% of the total mass. ...
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.