Introduction - Willmann-Bell
... Argo Navis. What can we say about this sprawling and incredibly bountiful constellation? Dennis has deemed it our masterpiece, and truth be told, there was no shortage of celestial marvels to chronicle and illustrate. We think it safe to say (as much as modesty allows) that our review of the uncanny ...
... Argo Navis. What can we say about this sprawling and incredibly bountiful constellation? Dennis has deemed it our masterpiece, and truth be told, there was no shortage of celestial marvels to chronicle and illustrate. We think it safe to say (as much as modesty allows) that our review of the uncanny ...
Distant galaxies and quasars The ages of things Light
... estimate the total rate of star formation in the Universe (regardless which galaxies it is taking place in ... This, like the quasar evolution, shows a dramatic peak at earlier times ... but somewhat later than the quasars ...
... estimate the total rate of star formation in the Universe (regardless which galaxies it is taking place in ... This, like the quasar evolution, shows a dramatic peak at earlier times ... but somewhat later than the quasars ...
Galactic astronomy - Sierra College Astronomy Home Page
... – Dust reradiates the absorbed energy in the infrared; – The most conspicuous type of bright emission nebula are HII regions. ...
... – Dust reradiates the absorbed energy in the infrared; – The most conspicuous type of bright emission nebula are HII regions. ...
Today`s Powerpoint
... Finally, fusion starts, stopping collapse: a star! Star reaches Main Sequence at end of Hayashi Track ...
... Finally, fusion starts, stopping collapse: a star! Star reaches Main Sequence at end of Hayashi Track ...
1_Introduction
... Proper motion = how fast a star is moving relative to background objects in arcseconds per year. Barnard’s Star ...
... Proper motion = how fast a star is moving relative to background objects in arcseconds per year. Barnard’s Star ...
The Milky Way: Home to Star Clusters
... was the original extent of the galaxy, and that this was created first, from the primordial gas that eventually collapsed in on itself, also demonstrated by the old stars contained within the globular clusters. This matter condensed to create the central bulge, which ultimately began to rotate, crea ...
... was the original extent of the galaxy, and that this was created first, from the primordial gas that eventually collapsed in on itself, also demonstrated by the old stars contained within the globular clusters. This matter condensed to create the central bulge, which ultimately began to rotate, crea ...
The Mass Assembly of Galaxies
... The Center of our Galaxy There is a cluster of B stars in the central 1’’ of the galaxy, the so-called S-cluster. These high proper motion stars - in particular star S2 - show that Sgr A* is a black-hole of 3-4 million solar masses. Large numbers of young stars, in particular O supergiants and WR s ...
... The Center of our Galaxy There is a cluster of B stars in the central 1’’ of the galaxy, the so-called S-cluster. These high proper motion stars - in particular star S2 - show that Sgr A* is a black-hole of 3-4 million solar masses. Large numbers of young stars, in particular O supergiants and WR s ...
The Milky Way Galaxy
... found on the edges of the galaxy. • Harlow Shapley found the distance to these clusters and he plotted their positions. • For them to fit, the Milky Way must be around 30 kpc across. (Shapley miscalcuated to around 40 kpc. ...
... found on the edges of the galaxy. • Harlow Shapley found the distance to these clusters and he plotted their positions. • For them to fit, the Milky Way must be around 30 kpc across. (Shapley miscalcuated to around 40 kpc. ...
Document
... • What are the two major types of star cluster? • Why are star clusters useful for studying stellar evolution? • How do we measure the age of a star cluster? ...
... • What are the two major types of star cluster? • Why are star clusters useful for studying stellar evolution? • How do we measure the age of a star cluster? ...
Chapter 19 Star Formation
... begins. The protostar has become a star. The star continues to contract and increase in temperature until it is in equilibrium: Internal pressure force outward, balancing the inward force of gravity, at every layer of the star’s interior. This is stage 7: The star has reached the Main Sequence and w ...
... begins. The protostar has become a star. The star continues to contract and increase in temperature until it is in equilibrium: Internal pressure force outward, balancing the inward force of gravity, at every layer of the star’s interior. This is stage 7: The star has reached the Main Sequence and w ...
Chapter 19 Star Formation
... begins. The protostar has become a star. The star continues to contract and increase in temperature until it is in equilibrium: Internal pressure force outward, balancing the inward force of gravity, at every layer of the star’s interior. This is stage 7: The star has reached the Main Sequence and w ...
... begins. The protostar has become a star. The star continues to contract and increase in temperature until it is in equilibrium: Internal pressure force outward, balancing the inward force of gravity, at every layer of the star’s interior. This is stage 7: The star has reached the Main Sequence and w ...
Astronomy 102, Spring 2003 Solutions to Review Problems
... certainly the stars formed together, as it is very unlikely that they would have come across each other and captured each other into a binary system. If the two stars formed together, then they must be the same age . If they’re the same age, and one is still on the main sequence while the other has ...
... certainly the stars formed together, as it is very unlikely that they would have come across each other and captured each other into a binary system. If the two stars formed together, then they must be the same age . If they’re the same age, and one is still on the main sequence while the other has ...
Document
... gotten on earth (about 10-11 Torr or mm of mercury) there is still plenty of gas and dust called interstellar medium. About 99% of this medium is gas and the rest is dust.As to the composition of this dust “The dust is made of thin, highly flattened flakes or needles of graphite (carbon) and silicat ...
... gotten on earth (about 10-11 Torr or mm of mercury) there is still plenty of gas and dust called interstellar medium. About 99% of this medium is gas and the rest is dust.As to the composition of this dust “The dust is made of thin, highly flattened flakes or needles of graphite (carbon) and silicat ...
2. A giant hand took one of the planets discovered
... 2. A giant hand took one of the planets discovered around other stars and put it in the solar system at the same distance from the sun as from its star. The mass of the planet is approximately that of Jupiter and the orbit is approximately that of Earth. These are the “hot Jupiters”, as big as Jupit ...
... 2. A giant hand took one of the planets discovered around other stars and put it in the solar system at the same distance from the sun as from its star. The mass of the planet is approximately that of Jupiter and the orbit is approximately that of Earth. These are the “hot Jupiters”, as big as Jupit ...
HR Diagram
... 8. Compare your results for NGC with data given at end of writeup. If way off check for errors. 9. Go through the step 6 procedure again using M45 (younger cluster) 10. Go thought step 7 procedure again using M45. 11. Go through procedure again using M67 (older cluster). 12. Compute the distances in ...
... 8. Compare your results for NGC with data given at end of writeup. If way off check for errors. 9. Go through the step 6 procedure again using M45 (younger cluster) 10. Go thought step 7 procedure again using M45. 11. Go through procedure again using M67 (older cluster). 12. Compute the distances in ...
File - greenscapes4you
... luminosity, but still much brighter than main sequence stars of same spectral type. The hot, white, small radius stars near the lower left are called white dwarfs. Giants and Supergiants are stars nearing the ends of their lives because they have already exhausted their core hydrogen. Surprisingly, ...
... luminosity, but still much brighter than main sequence stars of same spectral type. The hot, white, small radius stars near the lower left are called white dwarfs. Giants and Supergiants are stars nearing the ends of their lives because they have already exhausted their core hydrogen. Surprisingly, ...
Today`s Powerpoint
... Finally, fusion starts, stopping collapse: a star! Star reaches Main Sequence at end of Hayashi Track ...
... Finally, fusion starts, stopping collapse: a star! Star reaches Main Sequence at end of Hayashi Track ...
PPT - Yale University
... rotation periods) because disks are fragile and cannot sustain a large torque. Most disks probably do not last this long before being disrupted by violent interactions in a realistic system of forming stars because . . . ...
... rotation periods) because disks are fragile and cannot sustain a large torque. Most disks probably do not last this long before being disrupted by violent interactions in a realistic system of forming stars because . . . ...
Answer to question 1 - Northwestern University
... B. Red giants, globular clusters, brightest galaxy in a cluster ...
... B. Red giants, globular clusters, brightest galaxy in a cluster ...
Announcements Evolution of High-Mass Stars: Red Supergiants
... • Pop. II: Older, bulge and halo stars, with lower percentage of heavy elements • Heavy elements (metals): anything that isn’t H, He, or Li ...
... • Pop. II: Older, bulge and halo stars, with lower percentage of heavy elements • Heavy elements (metals): anything that isn’t H, He, or Li ...
Slide 1 - Personal.psu.edu
... 19.3 Stars of Other Masses This H-R diagram shows the evolution of stars somewhat more and somewhat less massive than the Sun. The shape of the paths is similar, but they wind up in different places on the Main ...
... 19.3 Stars of Other Masses This H-R diagram shows the evolution of stars somewhat more and somewhat less massive than the Sun. The shape of the paths is similar, but they wind up in different places on the Main ...
Stars and constellations
... Sometimes the nuclear furnace that powers a star gets out of control. When this happens the star blows up. Now a star is a huge thing and so when it blows up you get a huge explosion. In fact it makes the star so bright that you can sometimes see it in daylight. This is what happened in 1054 when th ...
... Sometimes the nuclear furnace that powers a star gets out of control. When this happens the star blows up. Now a star is a huge thing and so when it blows up you get a huge explosion. In fact it makes the star so bright that you can sometimes see it in daylight. This is what happened in 1054 when th ...
HW7-3
... (260)RQ 2: (a) Why is there a lower end to the main sequence? (b) Why is there an upper end? (a) Stars less than 0.08M☉ (8% of M☉) are not hot enough in their cores to run fusion. These are brown dwarfs. (b) Very massive stars have so much fusion that the outward forces overwhelm gravity and they ar ...
... (260)RQ 2: (a) Why is there a lower end to the main sequence? (b) Why is there an upper end? (a) Stars less than 0.08M☉ (8% of M☉) are not hot enough in their cores to run fusion. These are brown dwarfs. (b) Very massive stars have so much fusion that the outward forces overwhelm gravity and they ar ...
Triggered Star Formation by Massive Stars in Star
... Wen-Ping Chen & Hsu-Tai Lee NCU/Astronomy BATC Workshop 2005.08.11 Weihai NGC6823 by BATC ...
... Wen-Ping Chen & Hsu-Tai Lee NCU/Astronomy BATC Workshop 2005.08.11 Weihai NGC6823 by BATC ...
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.