Measuring the masses of clusters
... and sin' = %/Dd ~ ' Note that &, ', (, and % are vectors, so must be added vectorially. Not important for the point-source case, but is important when modeling complex systems (like a cluster!) ...
... and sin' = %/Dd ~ ' Note that &, ', (, and % are vectors, so must be added vectorially. Not important for the point-source case, but is important when modeling complex systems (like a cluster!) ...
Document
... 31. A surface explosion on a white dwarf, caused by falling matter from the atmosphere of its binary companion, creates what kind of object? a) Nova., b) Type-I supernova., c) Type-II supernova., d) Contact binary. 32. An iron core cannot support a star because: a) Iron has poor nuclear binding ener ...
... 31. A surface explosion on a white dwarf, caused by falling matter from the atmosphere of its binary companion, creates what kind of object? a) Nova., b) Type-I supernova., c) Type-II supernova., d) Contact binary. 32. An iron core cannot support a star because: a) Iron has poor nuclear binding ener ...
Astronomy HOMEWORK Chapter 12 - 9th Edition 1. Consider a star
... smoothly as mass decreases. So: the first stars to turn into Red Giants (and pass rapidly through other stages) are the high-mass ones. So “How:” the turnoff point is determined (L and T ). These values are correlated with a lifetime, and that’s the age of the cluster. 16. Why do astronomers believe ...
... smoothly as mass decreases. So: the first stars to turn into Red Giants (and pass rapidly through other stages) are the high-mass ones. So “How:” the turnoff point is determined (L and T ). These values are correlated with a lifetime, and that’s the age of the cluster. 16. Why do astronomers believe ...
18 are exactly the same ones as for galactic star clusters of early
... suggesting a gravitational con traction time of about 30 million years. Finally, there is the curious vertical branch at B—V=-\-l-l; some of these stars probably belong to the field, but one may ask whether some correspond to a very much older generation of stars. This observation seems to support ...
... suggesting a gravitational con traction time of about 30 million years. Finally, there is the curious vertical branch at B—V=-\-l-l; some of these stars probably belong to the field, but one may ask whether some correspond to a very much older generation of stars. This observation seems to support ...
Diapositiva 1
... Stars, Dust and Nebula in NGC 6559 Machine with which the photo has been taken: Hawaiian Starlight Telescope Explanation: When stars form, pandemonium reigns. A textbook case is the star forming region NGC 6559. Visible above are red glowing emission nebulas of hydrogen, blue reflection nebulas of ...
... Stars, Dust and Nebula in NGC 6559 Machine with which the photo has been taken: Hawaiian Starlight Telescope Explanation: When stars form, pandemonium reigns. A textbook case is the star forming region NGC 6559. Visible above are red glowing emission nebulas of hydrogen, blue reflection nebulas of ...
observingnebulaeclusters-1
... show several protoplanetary disks or "proplyds" and finally a single dark disk surrounding a central star. ...
... show several protoplanetary disks or "proplyds" and finally a single dark disk surrounding a central star. ...
Today`s Powerpoint
... D: Metals spontaneously decay to lighter elements during the 10 billion year age of the globular cluster. ...
... D: Metals spontaneously decay to lighter elements during the 10 billion year age of the globular cluster. ...
Evan_Skillman_1
... those that have finished fusing H to He in their cores are no longer on the main sequence. • All stars become larger and redder after exhausting their core hydrogen: giants and supergiants. • Most stars end up small and white after fusion has ceased: white dwarfs. ...
... those that have finished fusing H to He in their cores are no longer on the main sequence. • All stars become larger and redder after exhausting their core hydrogen: giants and supergiants. • Most stars end up small and white after fusion has ceased: white dwarfs. ...
Ch. 19 (Starbirth)
... • The protostar continues to collapse; when the core is dense and hot enough, fusion begins • The star still continues to collapse until the inward force of gravity is balanced by the outward pressure from the core. The star is now on the main sequence. • More massive stars follow the same process, ...
... • The protostar continues to collapse; when the core is dense and hot enough, fusion begins • The star still continues to collapse until the inward force of gravity is balanced by the outward pressure from the core. The star is now on the main sequence. • More massive stars follow the same process, ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... • Very massive stars found in these clusters ...
... • Very massive stars found in these clusters ...
Astronomy 104: Homework Set 5 Due: Monday, March 16, 2015
... Keeping in mind that the Bulge of our Galaxy has a power-law slope of about −4 and the Halo has a power-law slope of about −3, which density profile from the table, number 1 or number 2, is most likely from the galaxy’s bulge population, and which is most likely from its halo? d) At what radius from ...
... Keeping in mind that the Bulge of our Galaxy has a power-law slope of about −4 and the Halo has a power-law slope of about −3, which density profile from the table, number 1 or number 2, is most likely from the galaxy’s bulge population, and which is most likely from its halo? d) At what radius from ...
Document
... Our Milky Way I. Select bright objects that you can see throughout the Milky Way and trace their directions and distances II. Observe objects at wavelengths other than visible (to eliminate problems caused by dust, gas, other galactic bodies, etc), and catalogue their directions and distances ...
... Our Milky Way I. Select bright objects that you can see throughout the Milky Way and trace their directions and distances II. Observe objects at wavelengths other than visible (to eliminate problems caused by dust, gas, other galactic bodies, etc), and catalogue their directions and distances ...
Chapter14- Our Galaxy - SFA Physics and Astronomy
... Cool clouds of molecular gas from out of hydrogen and other elements. ...
... Cool clouds of molecular gas from out of hydrogen and other elements. ...
The Milky Way * A Classic Galaxy
... • Find layers at age 1.5Myrs and another at 2.3 Myrs ago, • This indicates two SN blasts at these times, and roughly 300 light yrs away from the abundances. • Agrees with Local Bubble size and expansion ...
... • Find layers at age 1.5Myrs and another at 2.3 Myrs ago, • This indicates two SN blasts at these times, and roughly 300 light yrs away from the abundances. • Agrees with Local Bubble size and expansion ...
PHY 150
... leaves the main sequence to when it becomes a white dwarf. Approximately how much mass will the Sun have when it becomes a white dwarf? Where will the rest of the mass ...
... leaves the main sequence to when it becomes a white dwarf. Approximately how much mass will the Sun have when it becomes a white dwarf? Where will the rest of the mass ...
Week 11 Concept Summary
... 2. Interstellar Medium: This is the gas and dust that floats freely about the galaxy. It is what blocks visible light and only allows us to see nearby stars in the plane of the galaxy, though radio and infrared light can get through it easily. Stars collapse and form from the ISM, build up more heav ...
... 2. Interstellar Medium: This is the gas and dust that floats freely about the galaxy. It is what blocks visible light and only allows us to see nearby stars in the plane of the galaxy, though radio and infrared light can get through it easily. Stars collapse and form from the ISM, build up more heav ...
1. a) Astronomers use the parallax method to measure
... distance to stars in other galaxies. In particular, we use the standard candle method to measure the distances to Cepheid variable stars in other galaxies. What is special about Cepheid variable stars that makes them useful for this purpose? We can figure out their luminosities from their periods of ...
... distance to stars in other galaxies. In particular, we use the standard candle method to measure the distances to Cepheid variable stars in other galaxies. What is special about Cepheid variable stars that makes them useful for this purpose? We can figure out their luminosities from their periods of ...
Night Sky Course Stars and Star Clusters within the
... about 15 light years. The cluster is only about 500 light years away – farther than the Pleiades. The bright orange stars are the ones that have had time to evolve into red giants. (Given the estimates of mass for those stars still remaining on the main sequence, we can use our models of stellar evo ...
... about 15 light years. The cluster is only about 500 light years away – farther than the Pleiades. The bright orange stars are the ones that have had time to evolve into red giants. (Given the estimates of mass for those stars still remaining on the main sequence, we can use our models of stellar evo ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... Brown dwarfs (and planets): estimated lower stellar mass limit is 0.08 M (or 80MJup). Lower mass objects have core T too low to ignite H. Red dwarfs: stars whose main-sequence lifetime exceeds the present age of the Universe (estimated as 1-2x1010 yr). Models yield an upper mass limit of stars that ...
... Brown dwarfs (and planets): estimated lower stellar mass limit is 0.08 M (or 80MJup). Lower mass objects have core T too low to ignite H. Red dwarfs: stars whose main-sequence lifetime exceeds the present age of the Universe (estimated as 1-2x1010 yr). Models yield an upper mass limit of stars that ...
Stellar evolution
... - First occurs in a runaway process: "the helium flash". Energy from fusion goes into re-expanding and cooling the core. This slows fusion, so star gets dimmer again. - Then stable He -> C burning. Still have H -> He shell burning surrounding it. ...
... - First occurs in a runaway process: "the helium flash". Energy from fusion goes into re-expanding and cooling the core. This slows fusion, so star gets dimmer again. - Then stable He -> C burning. Still have H -> He shell burning surrounding it. ...
STAR FORMATION (Ch. 19)
... stars, starting with the Bok globules (dark clouds) and giant gaseous pillars (emission nebulae), followed by circumstellar disks, and progressing to evolved massive stars in the young starburst cluster.To the upper right of center is the evolved blue supergiant called Sher 25. The star has a unique ...
... stars, starting with the Bok globules (dark clouds) and giant gaseous pillars (emission nebulae), followed by circumstellar disks, and progressing to evolved massive stars in the young starburst cluster.To the upper right of center is the evolved blue supergiant called Sher 25. The star has a unique ...
characteristics of stars
... the disk. In the central bulge, the stars are so numerous that they appear very close even though they are separated by large distance. Most of the stars outside the bulge are arranged in long ____________, called _________ which curve around the bulge. The entire Milky Way rotates around this bulge ...
... the disk. In the central bulge, the stars are so numerous that they appear very close even though they are separated by large distance. Most of the stars outside the bulge are arranged in long ____________, called _________ which curve around the bulge. The entire Milky Way rotates around this bulge ...
proposed october viewing list
... M11 Known as the Wild Duck cluster, this open cluster in the constellation Scutum, (SKEW-tum) is seen best with the 4” refractor at low magnification. It contains more than 2900 stars and is estimated to be about 250 million years old. M11 is receding from us at a speed of 27 km/s. M17 The Omega, or ...
... M11 Known as the Wild Duck cluster, this open cluster in the constellation Scutum, (SKEW-tum) is seen best with the 4” refractor at low magnification. It contains more than 2900 stars and is estimated to be about 250 million years old. M11 is receding from us at a speed of 27 km/s. M17 The Omega, or ...
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.