20 pm - Starmap
... Using binoculars, preferably with a tripod, will considerably enhance your star gazing experience. Many deep sky objects like galaxies and clusters will be within reach. Jupiter satellites and Saturn’s rings will also be visible. A spectacular experience for beginners in astronomy... ...
... Using binoculars, preferably with a tripod, will considerably enhance your star gazing experience. Many deep sky objects like galaxies and clusters will be within reach. Jupiter satellites and Saturn’s rings will also be visible. A spectacular experience for beginners in astronomy... ...
Interpreting the HR diagram of stellar clusters
... In fact, it seems that stars are usually born in big groups, as members of a cluster of stars. All the stars in the cluster form at about the same time. So, if we look at a cluster, we see a bunch of stars which are all roughly the same age. However, the stars do not all have the same mass: most ten ...
... In fact, it seems that stars are usually born in big groups, as members of a cluster of stars. All the stars in the cluster form at about the same time. So, if we look at a cluster, we see a bunch of stars which are all roughly the same age. However, the stars do not all have the same mass: most ten ...
Announcements Evolution of High-Mass Stars: Red Supergiants
... The Halo has very little gas, and no new stars are forming there. The halo of the galaxy is populated by old stars. (Population II stars) ...
... The Halo has very little gas, and no new stars are forming there. The halo of the galaxy is populated by old stars. (Population II stars) ...
Document
... center (rather heliocentric) •Tried to estimate Rayleigh scattering due to ISM gas but determined it to be insignificant (because most obscuration is due to ISM dust absorption which has a smaller dependence) ...
... center (rather heliocentric) •Tried to estimate Rayleigh scattering due to ISM gas but determined it to be insignificant (because most obscuration is due to ISM dust absorption which has a smaller dependence) ...
Slide 1
... accretion disk indicating BH or WH in center--a quadrillion solar masses!) The Pisces-Cetus Complex: may include 400 rich (and lots of poor) clusters. Brent Tully. Is the Universe homogeneous? God's Bubble Bath: Galaxy superclusters seem to from in bubble structures and filaments with Voids 100-500 ...
... accretion disk indicating BH or WH in center--a quadrillion solar masses!) The Pisces-Cetus Complex: may include 400 rich (and lots of poor) clusters. Brent Tully. Is the Universe homogeneous? God's Bubble Bath: Galaxy superclusters seem to from in bubble structures and filaments with Voids 100-500 ...
The Milky Way`s Restless Swarms of Stars
... the final stage of analysis by a team including kinetic energy. That forces the Shara and astronomer Rex Saffer at Villanova binary stars into a tighter orbit University in Pennsylvania. around each other, a process Getting at the core called binary “burning.” In Another cluster mystery lies at the ...
... the final stage of analysis by a team including kinetic energy. That forces the Shara and astronomer Rex Saffer at Villanova binary stars into a tighter orbit University in Pennsylvania. around each other, a process Getting at the core called binary “burning.” In Another cluster mystery lies at the ...
Document
... The structure is hard to determine because: 1) We are inside 2) Distance measurements are difficult 3) Our view towards the center is obscured by gas and dust ...
... The structure is hard to determine because: 1) We are inside 2) Distance measurements are difficult 3) Our view towards the center is obscured by gas and dust ...
Integrative Studies 410 Our Place in the Universe
... – While the parent star is destroyed, a tiny ultracompressed remnant may remain – a neutron ...
... – While the parent star is destroyed, a tiny ultracompressed remnant may remain – a neutron ...
Deep Space Objects
... galaxies, devouring nearby Suns in their star-dense nuclei and adding those stars’ mass to their own. As far as we can see, galaxies themselves are the main building blocks of our universe. Galaxies can be a fraction the size of our Milky Way, or dozens or more times larger. They can be shaped like ...
... galaxies, devouring nearby Suns in their star-dense nuclei and adding those stars’ mass to their own. As far as we can see, galaxies themselves are the main building blocks of our universe. Galaxies can be a fraction the size of our Milky Way, or dozens or more times larger. They can be shaped like ...
Summary Of the Structure of the Milky Way
... Way. These clusters are more luminous than open clusters because they typically contain 500,000 stars many of which are red giants. Also, they are not (generally) buried in the dust of the Milky Way's disk, but are seen in the dust-free halo above and below the disk. The distribution of globular clu ...
... Way. These clusters are more luminous than open clusters because they typically contain 500,000 stars many of which are red giants. Also, they are not (generally) buried in the dust of the Milky Way's disk, but are seen in the dust-free halo above and below the disk. The distribution of globular clu ...
Document
... stars, with a fairly large cluster core radius. The black hole certainly would have an effect on the density of stars near it, but only at a radius well inside 1% of the globular cluster core radius and only affecting a few tens of stars or so ...
... stars, with a fairly large cluster core radius. The black hole certainly would have an effect on the density of stars near it, but only at a radius well inside 1% of the globular cluster core radius and only affecting a few tens of stars or so ...
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 ...
The Milky Way Galaxy
... • Henrietta Leavitt discovered that the period of Cepheid variable stars depends on their absolute magnitudes. • If we know the magnitudes, we can determine distances: D = 10(Mapp - Mabs +5)/5 • You can also read the distance off the graph! ...
... • Henrietta Leavitt discovered that the period of Cepheid variable stars depends on their absolute magnitudes. • If we know the magnitudes, we can determine distances: D = 10(Mapp - Mabs +5)/5 • You can also read the distance off the graph! ...
Ages of Star Clusters - Indiana University Astronomy
... Attached are Hertzsprung-Russell (HR) diagrams for six star clusters in the Milky Way. The clusters range in age from less than 20 million years (2x107 years) to 5 billion years (5x109 years). Today we will investigate the properties of star clusters, and determine their distances and ages. The HR d ...
... Attached are Hertzsprung-Russell (HR) diagrams for six star clusters in the Milky Way. The clusters range in age from less than 20 million years (2x107 years) to 5 billion years (5x109 years). Today we will investigate the properties of star clusters, and determine their distances and ages. The HR d ...
Summary: Nuclear burning in stars
... • Gas, stars closer to center orbit in less time than those farther from center. • Î automatic stretching of any feature into a trailing spiral. • But arms should rapidly wind up and disappear ...
... • Gas, stars closer to center orbit in less time than those farther from center. • Î automatic stretching of any feature into a trailing spiral. • But arms should rapidly wind up and disappear ...
2010_02_04 LP08 Our Galactic Home
... Heliocentric parallax (Earth’s ORBIT as baseline) Moving clusters (Pleiades) H-R Diagram R R Lyrae variable stars (M=0.5) Cepheid variable stars Brightest supergiants (M=-8) “Normal” novae Globular clusters (brightest at M=-10) H II Regions (doesn’t work perfectly) Planetary nebulae Hydrogen clouds ...
... Heliocentric parallax (Earth’s ORBIT as baseline) Moving clusters (Pleiades) H-R Diagram R R Lyrae variable stars (M=0.5) Cepheid variable stars Brightest supergiants (M=-8) “Normal” novae Globular clusters (brightest at M=-10) H II Regions (doesn’t work perfectly) Planetary nebulae Hydrogen clouds ...
1 Astronomical Measurements and Quantities 2 Astronomical Objects
... Distance Ladder: The Hubble low (V=HD) and the expansion of the Universe. The Baade-Wesselink method. A brief overview of different methods treated through the course to go from very nearby objects to very distant ones. [K],[BM] Galaxy Clusters: Morphological classification. Main properties. Cluster ...
... Distance Ladder: The Hubble low (V=HD) and the expansion of the Universe. The Baade-Wesselink method. A brief overview of different methods treated through the course to go from very nearby objects to very distant ones. [K],[BM] Galaxy Clusters: Morphological classification. Main properties. Cluster ...
Unit 1
... D. Stopping of time in the vicinity of the black hole as the black hole travels through space-time ...
... D. Stopping of time in the vicinity of the black hole as the black hole travels through space-time ...
Where do Stars Form ?
... cooler & fainter longer MS lifetimes High Mass Stars: hotter & brighter shorter MS lifetimes ...
... cooler & fainter longer MS lifetimes High Mass Stars: hotter & brighter shorter MS lifetimes ...
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 ...
Project 5: Globular cluster
... 1. Globular Clusters A globular cluster is a spherical collection of stars that are very tightly bound to each other by gravity. Globular clusters orbit around the Milky Way galaxy core like satellites. The number of stars in a globular cluster varies from a few thousand up to a m ...
... 1. Globular Clusters A globular cluster is a spherical collection of stars that are very tightly bound to each other by gravity. Globular clusters orbit around the Milky Way galaxy core like satellites. The number of stars in a globular cluster varies from a few thousand up to a m ...
More on Cluster HR diagrams - University of Texas Astronomy
... this is stellar evolution theory). Eventually (after only a few hours or less), the huge energy input does cause the pressure to increase enough so that the core expands, making itself non-degenerate; it settles into a new equilibrium between pressure and gravity converting He into C ⇒ called “horiz ...
... this is stellar evolution theory). Eventually (after only a few hours or less), the huge energy input does cause the pressure to increase enough so that the core expands, making itself non-degenerate; it settles into a new equilibrium between pressure and gravity converting He into C ⇒ called “horiz ...
Globular cluster
A globular cluster is a spherical collection of stars that orbits a galactic core as a satellite. Globular clusters are very tightly bound by gravity, which gives them their spherical shapes and relatively high stellar densities toward their centers. The name of this category of star cluster is derived from the Latin globulus—a small sphere. A globular cluster is sometimes known more simply as a globular.Globular clusters, which are found in the halo of a galaxy, contain considerably more stars and are much older than the less dense galactic, or open clusters, which are found in the disk. Globular clusters are fairly common; there are about 150 to 158 currently known globular clusters in the Milky Way, with perhaps 10 to 20 more still undiscovered. These globular clusters orbit the Galaxy at radii of 40 kiloparsecs (130,000 light-years) or more. Larger galaxies can have more: Andromeda, for instance, may have as many as 500. Some giant elliptical galaxies, particularly those at the centers of galaxy clusters, such as M87, have as many as 13,000 globular clusters.Every galaxy of sufficient mass in the Local Group has an associated group of globular clusters, and almost every large galaxy surveyed has been found to possess a system of globular clusters. The Sagittarius Dwarf galaxy and the disputed Canis Major Dwarf galaxy appear to be in the process of donating their associated globular clusters (such as Palomar 12) to the Milky Way. This demonstrates how many of this galaxy's globular clusters might have been acquired in the past.Although it appears that globular clusters contain some of the first stars to be produced in the galaxy, their origins and their role in galactic evolution are still unclear. It does appear clear that globular clusters are significantly different from dwarf elliptical galaxies and were formed as part of the star formation of the parent galaxy rather than as a separate galaxy. However, recent conjectures by astronomers suggest that globular clusters and dwarf spheroidals may not be clearly separate and distinct types of objects.