Lecture Ten - The Sun Amongst the Stars Part II
... So why are there so many M dwarfs? Does the star formation process strongly favor the production of such stars? Or is there some other process at work ‘removing’ hotter and more luminous stars from the populations we observe? The answer requires us to know how stars change over time, and therefore t ...
... So why are there so many M dwarfs? Does the star formation process strongly favor the production of such stars? Or is there some other process at work ‘removing’ hotter and more luminous stars from the populations we observe? The answer requires us to know how stars change over time, and therefore t ...
HW #8 Answers (Due 10/21)
... rapidly and therefore die while still nearby the region in which they formed. They die as supernova explosions which send out shock waves that run into the molecular cloud from which they formed. This helps to compress the cloud and set off new star formation. This is also a selfsustaining process. ...
... rapidly and therefore die while still nearby the region in which they formed. They die as supernova explosions which send out shock waves that run into the molecular cloud from which they formed. This helps to compress the cloud and set off new star formation. This is also a selfsustaining process. ...
Galaxies - Wallkill Valley Regional High School
... - Range from dwarf to giant galaxies based on number of stars ...
... - Range from dwarf to giant galaxies based on number of stars ...
the printable Observing Olympics Object Info Sheet in pdf
... NGC6572 – A very bright 8.1 magnitude Planetary Nebula, located in Ophiuchus and discovered in 1825 by Friedrich George Wilhelm Von Struve. Visually at low power it will appear as a colored star but higher magnification will reveal its disk. It has a very high surface brightness and some observers r ...
... NGC6572 – A very bright 8.1 magnitude Planetary Nebula, located in Ophiuchus and discovered in 1825 by Friedrich George Wilhelm Von Struve. Visually at low power it will appear as a colored star but higher magnification will reveal its disk. It has a very high surface brightness and some observers r ...
AS1001:Extra-Galactic Astronomy Stars and Gas in Galaxies
... • Stars are born from gas in high-density regions. • Compressing gas (e.g. in collisions, or spiral arms) triggers gravitational collapse to form stars. – Ellipticals: very little gas ...
... • Stars are born from gas in high-density regions. • Compressing gas (e.g. in collisions, or spiral arms) triggers gravitational collapse to form stars. – Ellipticals: very little gas ...
Age Estimates of Globular Clusters in the Milky Way
... are thought to have coalesced early on from small-scale density fluctuations in the primordial gas cloud, which itself later coherently collapsed, dissipating its energy and settling into the disk of our Milky Way Galaxy. As a result, these objects populate a roughly spherical halo in our galaxy toda ...
... are thought to have coalesced early on from small-scale density fluctuations in the primordial gas cloud, which itself later coherently collapsed, dissipating its energy and settling into the disk of our Milky Way Galaxy. As a result, these objects populate a roughly spherical halo in our galaxy toda ...
Star Clusters - Caltech Astronomy
... globular clusters are the stellar associations, loose, unbound groups of stars with particular spectral properties. Associations are normally observed as widespread regions with an excess density of spectral type O and B stars (‘OB ASSOCIATIONS’) or T TAURI STARS (‘T associations’). In principle, th ...
... globular clusters are the stellar associations, loose, unbound groups of stars with particular spectral properties. Associations are normally observed as widespread regions with an excess density of spectral type O and B stars (‘OB ASSOCIATIONS’) or T TAURI STARS (‘T associations’). In principle, th ...
The Origin of the Milky Way
... a huge disk, and a galactic halo surrounding both. • The diameter of the disk is 30kpc (100,000 light years). • The thickness of the disk is only 300pc (1000 light years) on average. • The total detectable mass is 200 billion solar masses. ...
... a huge disk, and a galactic halo surrounding both. • The diameter of the disk is 30kpc (100,000 light years). • The thickness of the disk is only 300pc (1000 light years) on average. • The total detectable mass is 200 billion solar masses. ...
3.1 Introduction
... 0 to 9. Thus we have spectral classes O9 and B0, the former being just hotter than the latter. Division between subclasses can be finer, e.g. class O9.5. O and B stars are sometimes referred to as ‘early-type’, while K and M are ‘late-type’. The Sun has spectral class G2. More recently the classific ...
... 0 to 9. Thus we have spectral classes O9 and B0, the former being just hotter than the latter. Division between subclasses can be finer, e.g. class O9.5. O and B stars are sometimes referred to as ‘early-type’, while K and M are ‘late-type’. The Sun has spectral class G2. More recently the classific ...
IAUS 298: Setting the Scene for Gaia and LAMOST, The current and
... (ASKAP, GAMES). In particular, we’ll be able to study in much more detail the connection (gas) between the disk and the halo, l-v diagrams for Galactic structure, absorption, rotation curve Star formation and giant molecular clouds, and the role of spiral arms (Dobbs): Simulations of the formation o ...
... (ASKAP, GAMES). In particular, we’ll be able to study in much more detail the connection (gas) between the disk and the halo, l-v diagrams for Galactic structure, absorption, rotation curve Star formation and giant molecular clouds, and the role of spiral arms (Dobbs): Simulations of the formation o ...
Final review - Physics and Astronomy
... Main Sequence stars fuse H to He in core. Lifetime depends on mass of H available and rate of fusion. Mass of H in core depends on mass of star. Fusion rate is related to luminosity ...
... Main Sequence stars fuse H to He in core. Lifetime depends on mass of H available and rate of fusion. Mass of H in core depends on mass of star. Fusion rate is related to luminosity ...
Lecture Eight (Powerpoint format) - Flash
... Giant Molecular clouds -- very dense and cold (by ISM standards) -hundreds of thousands of molecules per cubic centimeter, tens of degrees. Location of all known star formation. Coronal phase -- very hot (millions of degrees), heated by powerful blasts from supernovae. Diffuse, not concentrated ...
... Giant Molecular clouds -- very dense and cold (by ISM standards) -hundreds of thousands of molecules per cubic centimeter, tens of degrees. Location of all known star formation. Coronal phase -- very hot (millions of degrees), heated by powerful blasts from supernovae. Diffuse, not concentrated ...
Stars: from Adolescence to Old Age
... The higher the temperature inside a star, the faster it uses up its hydrogen fuel Although massive stars have more fuel, they burn it so quickly that their lifetimes are much shorter than those of low-mass stars This also explains why the most massive main-sequence stars are the most luminous 4 Augu ...
... The higher the temperature inside a star, the faster it uses up its hydrogen fuel Although massive stars have more fuel, they burn it so quickly that their lifetimes are much shorter than those of low-mass stars This also explains why the most massive main-sequence stars are the most luminous 4 Augu ...
ppt document - FacStaff Home Page for CBU
... Do galaxies cluster together like stars do? When we look around, we do indeed see that galaxies appear in clusters, and appear to orbit one another by their mutual gravity. The Milky Way is one of about 40 or so galaxies that form the Local Group. Andromeda (another spiralB galaxy about 2 million li ...
... Do galaxies cluster together like stars do? When we look around, we do indeed see that galaxies appear in clusters, and appear to orbit one another by their mutual gravity. The Milky Way is one of about 40 or so galaxies that form the Local Group. Andromeda (another spiralB galaxy about 2 million li ...
Hertzsprung-Russell Diagram—key to understanding properties of stars. 26 Sept
... constellation and a globular cluster (taken 100 years later)? ...
... constellation and a globular cluster (taken 100 years later)? ...
BASIC PROPERTIES of STARS - 2
... Venus is about 105,000,000 km from the Sun. (1) What is approximate time to get the return signal from Venus when it is at its closest to Earth? C = 3 x 105 km/s (A 150; B 200; C 300; D 400 seconds) (2) What is the approximate time to get a return signal from Venus when Venus is at its most distant ...
... Venus is about 105,000,000 km from the Sun. (1) What is approximate time to get the return signal from Venus when it is at its closest to Earth? C = 3 x 105 km/s (A 150; B 200; C 300; D 400 seconds) (2) What is the approximate time to get a return signal from Venus when Venus is at its most distant ...
Summary: Modes of Star Formation
... There has been much interest in reconstructing the history of star formation in our Galaxy and others from their stellar age distributions, and new results were presented here for the star formation history of our Galaxy, the Magellanic Clouds, and several other Local Group dwarfs. The non-uniform a ...
... There has been much interest in reconstructing the history of star formation in our Galaxy and others from their stellar age distributions, and new results were presented here for the star formation history of our Galaxy, the Magellanic Clouds, and several other Local Group dwarfs. The non-uniform a ...
Dark Matter - UW - Laramie, Wyoming | University of Wyoming
... bend the light from a more distant galaxy. Image of the galaxy is strongly distorted into arcs. ...
... bend the light from a more distant galaxy. Image of the galaxy is strongly distorted into arcs. ...
Astronomy of the Northern Sky—
... itself forms. The disk likely forms smaller, non-energy producing, non-glowing bodies—planets—with moons, comets and other small bodies around them. What kind of star? All depends on the mass available. More mass—> bigger star, hotter, more bluish, shorter living. The Northern Sky faces mostly away ...
... itself forms. The disk likely forms smaller, non-energy producing, non-glowing bodies—planets—with moons, comets and other small bodies around them. What kind of star? All depends on the mass available. More mass—> bigger star, hotter, more bluish, shorter living. The Northern Sky faces mostly away ...
Nuclear fusion in stars
... • If R increases by a factor of 4, r does the same by factor of 8. This means that a collapsing cloud can fragment ! into smaller collapsing clouds. • This process ends with star formation or when rotational speed becomes too high (conservation of angular momentum) • Hierarchical collapse can produc ...
... • If R increases by a factor of 4, r does the same by factor of 8. This means that a collapsing cloud can fragment ! into smaller collapsing clouds. • This process ends with star formation or when rotational speed becomes too high (conservation of angular momentum) • Hierarchical collapse can produc ...
- Amazing Space, STScI
... center of the star at 1.5 million miles per hour. At the bottom-left corner of the image is an irregularly shaped object called a dark globule. These are dark clouds of dust and gas that resist erosion by the stellar winds. New stars may be forming in their depths. Moving along the lower-left quadra ...
... center of the star at 1.5 million miles per hour. At the bottom-left corner of the image is an irregularly shaped object called a dark globule. These are dark clouds of dust and gas that resist erosion by the stellar winds. New stars may be forming in their depths. Moving along the lower-left quadra ...
the magellanic clouds newsletter - Keele University Astrophysics
... much as 30 kpc and 75 km s−1 . Furthermore, we show that the gravitational pull of the LMC and response of the Milky Way are likely to significantly affect the orbit and phase space distribution of tidal debris from the Sagittarius dwarf galaxy (Sgr). Such effects are larger than previous estimates ...
... much as 30 kpc and 75 km s−1 . Furthermore, we show that the gravitational pull of the LMC and response of the Milky Way are likely to significantly affect the orbit and phase space distribution of tidal debris from the Sagittarius dwarf galaxy (Sgr). Such effects are larger than previous estimates ...
March
... autumn evenings, easily seen by eye in a dark sky. They are two galaxies like the Milky Way but much smaller. Each is made of billions of stars. The Large Cloud contains many clusters of young luminous stars seen as patches of light in binoculars and telescopes. The LMC is about 160 000 light years ...
... autumn evenings, easily seen by eye in a dark sky. They are two galaxies like the Milky Way but much smaller. Each is made of billions of stars. The Large Cloud contains many clusters of young luminous stars seen as patches of light in binoculars and telescopes. The LMC is about 160 000 light years ...
Colour-magnitude diagram of an open cluster
... Hertzsprung-Russell diagram, which is a plot of luminosity versus temperature. In this project you will produce a colour-magnitude diagram (hereafter CMD) for an open star cluster. Open star clusters are groups of stars that were born at the same time from a single gas cloud. All stars in a cluster ...
... Hertzsprung-Russell diagram, which is a plot of luminosity versus temperature. In this project you will produce a colour-magnitude diagram (hereafter CMD) for an open star cluster. Open star clusters are groups of stars that were born at the same time from a single gas cloud. All stars in a cluster ...
Galaxy Far Far Away ppt
... the galaxy. HALO: Area surrounding galaxy that contains some scattered globular clusters. DISK: Contains most of the stars in the galaxy. ...
... the galaxy. HALO: Area surrounding galaxy that contains some scattered globular clusters. DISK: Contains most of the stars in the galaxy. ...
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.