Observations of V838 Mon light echo
... 1/10000 solar masses. When the ejected gas expands, its density decreases rapidly, it passes into the optically thin state and gets ionized by the hard radiation of the hot dwarf surface. On the contrary, if hydrogen explosion or energy release of another nature happens in the center of a star, the ...
... 1/10000 solar masses. When the ejected gas expands, its density decreases rapidly, it passes into the optically thin state and gets ionized by the hard radiation of the hot dwarf surface. On the contrary, if hydrogen explosion or energy release of another nature happens in the center of a star, the ...
Chapter 1 Introduction
... tend to show little or no hydrogen, and are therefore classed as Type Ib (containing helium lines) or Type Ic (containing no helium lines). e mass of the ejecta in these supernovae is small (and may be almost non-existent in the case of ultra-stripped Type Ic supernovae), and therefore so is the tot ...
... tend to show little or no hydrogen, and are therefore classed as Type Ib (containing helium lines) or Type Ic (containing no helium lines). e mass of the ejecta in these supernovae is small (and may be almost non-existent in the case of ultra-stripped Type Ic supernovae), and therefore so is the tot ...
Explores Angular Size - Chandra X
... how big something is in kilometers, instead of how big it appears to be in angular measure. To get this information, all we need to know is how far away the object is from us. The moon is 324,000 kilometers away, and Venus is about 40 million kilometers away from Earth at its closest distance. The f ...
... how big something is in kilometers, instead of how big it appears to be in angular measure. To get this information, all we need to know is how far away the object is from us. The moon is 324,000 kilometers away, and Venus is about 40 million kilometers away from Earth at its closest distance. The f ...
hr diagrams of star clusters
... Star clusters are groups of stars which, astronomers believe, were born together at roughly the same time from the same cloud of interstellar gas. HR diagrams are particularly useful for studying the characteristics of such clusters. The stars in a cluster have a range of stellar masses, from very m ...
... Star clusters are groups of stars which, astronomers believe, were born together at roughly the same time from the same cloud of interstellar gas. HR diagrams are particularly useful for studying the characteristics of such clusters. The stars in a cluster have a range of stellar masses, from very m ...
HR DIAGRAMS OF STAR CLUSTERS
... Star clusters are groups of stars which, astronomers believe, were born together at roughly the same time from the same cloud of interstellar gas. HR diagrams are particularly useful for studying the characteristics of such clusters. The stars in a cluster have a range of stellar masses, from very m ...
... Star clusters are groups of stars which, astronomers believe, were born together at roughly the same time from the same cloud of interstellar gas. HR diagrams are particularly useful for studying the characteristics of such clusters. The stars in a cluster have a range of stellar masses, from very m ...
THE PERIOD OF ROTATION OF THE SUN
... Star clusters are groups of stars which, astronomers believe, were born together at roughly the same time from the same cloud of interstellar gas. HR diagrams are particularly useful for studying the characteristics of such clusters. The stars in a cluster have a range of stellar masses, from very m ...
... Star clusters are groups of stars which, astronomers believe, were born together at roughly the same time from the same cloud of interstellar gas. HR diagrams are particularly useful for studying the characteristics of such clusters. The stars in a cluster have a range of stellar masses, from very m ...
D109-08x
... but bluer than NGC 1569, is the extreme V-R color. It is virtually impossible for galaxy stellar populations to have V-R colors this blue unless there is almost a complete absence of a red giant branch. Thus, globally, this object appears to be very young. Further V and I CCD imaging obtained in 198 ...
... but bluer than NGC 1569, is the extreme V-R color. It is virtually impossible for galaxy stellar populations to have V-R colors this blue unless there is almost a complete absence of a red giant branch. Thus, globally, this object appears to be very young. Further V and I CCD imaging obtained in 198 ...
The Milky Way Galaxy
... • It takes the Solar System about 225–250 million years to complete one orbit of the galaxy (a galactic year),[33] so it is thought to have ...
... • It takes the Solar System about 225–250 million years to complete one orbit of the galaxy (a galactic year),[33] so it is thought to have ...
lecture25
... Dust is generated in the late stages of low and high mass stars, when carbon and silicon is dredged up from the cores and ejected in stellar winds, planetary nebulae, and possibly supernova remnants. The blocking of visible light by dust is called dust extinction. ...
... Dust is generated in the late stages of low and high mass stars, when carbon and silicon is dredged up from the cores and ejected in stellar winds, planetary nebulae, and possibly supernova remnants. The blocking of visible light by dust is called dust extinction. ...
B - Department of Physics and Astronomy
... C. *They are burning helium into carbon and oxygen in their cores D. They are burning helium into carbon and oxygen in a shell around their cores 4. In the process of helium shell fusion in low-mass stars near the end of their lives, the stars moves upward and to the right on the asymptotic giant b ...
... C. *They are burning helium into carbon and oxygen in their cores D. They are burning helium into carbon and oxygen in a shell around their cores 4. In the process of helium shell fusion in low-mass stars near the end of their lives, the stars moves upward and to the right on the asymptotic giant b ...
Correct answers shown in boldface. Be sure to write your name and
... b. they did not have photographic plates to detect very faint stars c. their telescopes were too small to see the whole system d. they needed infrared detectors e. they did not realize how interstellar dust cut off their view 33. When clumps of gas first collapse into young stars, their arrival on t ...
... b. they did not have photographic plates to detect very faint stars c. their telescopes were too small to see the whole system d. they needed infrared detectors e. they did not realize how interstellar dust cut off their view 33. When clumps of gas first collapse into young stars, their arrival on t ...
preliminary version - University of Exeter
... Cep OB3b imply an evolutionary sequence in which stars are initially disc-locked at 8-day periods (the ONC) are released at ~ 1 Myr and gradually spin up, to 2 day periods at ~4 Myr (Cep OB3b). A neat evolutionary sequence is spoiled by IC 348, however. Like the ONC, the high mass stars in IC 348 ar ...
... Cep OB3b imply an evolutionary sequence in which stars are initially disc-locked at 8-day periods (the ONC) are released at ~ 1 Myr and gradually spin up, to 2 day periods at ~4 Myr (Cep OB3b). A neat evolutionary sequence is spoiled by IC 348, however. Like the ONC, the high mass stars in IC 348 ar ...
Presentation - University of Idaho
... The Schonberg-Chandrasekhar Limit Helium has 4 times more mass than Hydrogen ...
... The Schonberg-Chandrasekhar Limit Helium has 4 times more mass than Hydrogen ...
Post main sequence evolution
... Where can we find it? Molecular Clouds Once we have enough material, it actually needs to collapse (gravity will take care of that) into a star. Stars are always born in clusters, where the majority of stars are low-mass stars. To determine the proportion of low-mass stars relative to highmass stars ...
... Where can we find it? Molecular Clouds Once we have enough material, it actually needs to collapse (gravity will take care of that) into a star. Stars are always born in clusters, where the majority of stars are low-mass stars. To determine the proportion of low-mass stars relative to highmass stars ...
Project 4: The HR diagram. Open clusters
... Exercise 2: Sirius is about twice as massive as the Sun. How much brighter is it with respect to the Sun? In the HR diagram, where will you find the least massive stars? and the most massive stars? If I double the mass of a main sequence star, the luminosity increases by a factor 2 3.5 ~ 11.3. ...
... Exercise 2: Sirius is about twice as massive as the Sun. How much brighter is it with respect to the Sun? In the HR diagram, where will you find the least massive stars? and the most massive stars? If I double the mass of a main sequence star, the luminosity increases by a factor 2 3.5 ~ 11.3. ...
All_Stars
... The Pleiades star cluster, a grouping of hundreds of stars all born at roughly the same time and at the same distance from Earth. ...
... The Pleiades star cluster, a grouping of hundreds of stars all born at roughly the same time and at the same distance from Earth. ...
charts_set_8
... Higher mass stars fuse heavier elements. Result is "onion" structure with many shells of fusion-produced elements. Heaviest element made is iron. Strong winds. ...
... Higher mass stars fuse heavier elements. Result is "onion" structure with many shells of fusion-produced elements. Heaviest element made is iron. Strong winds. ...
Synthetic color-magnitude diagrams: the ingredients
... at time t = 0, no metals were present; hence Z(0) = 0. – The galaxy did not contain any stars at the time of its birth, so that all baryonic matter was in the form of gas. – In addition, we consider the galaxy as a closed system out of which no matter can escape or be added later on by processes o ...
... at time t = 0, no metals were present; hence Z(0) = 0. – The galaxy did not contain any stars at the time of its birth, so that all baryonic matter was in the form of gas. – In addition, we consider the galaxy as a closed system out of which no matter can escape or be added later on by processes o ...
pptx
... of old stars, seen in infra-red light which penetrates the dust slowly rotating, high in heavy elements (with wide spread) ...
... of old stars, seen in infra-red light which penetrates the dust slowly rotating, high in heavy elements (with wide spread) ...
The Milky Way - University of North Texas
... b. Objects below this mass can only form in HI clouds. c. Objects below this mass are not hot enough to fuse normal hydrogen. d. They form too slowly and hot stars nearby clear the gas and dust quickly. e. Our telescopes do not have enough light gathering power to detect dim objects. ...
... b. Objects below this mass can only form in HI clouds. c. Objects below this mass are not hot enough to fuse normal hydrogen. d. They form too slowly and hot stars nearby clear the gas and dust quickly. e. Our telescopes do not have enough light gathering power to detect dim objects. ...
1/2016
... Description: Delta Cephei is the prototype of the Cepheid class of variable stars. With a change in visual magnitude of 3.5 to 4.4, delta Cephei’s entire range of variability can be observed with the unaided eye. Its period of 5.366 days makes it an attractive candidate for anyone anxious to obtain ...
... Description: Delta Cephei is the prototype of the Cepheid class of variable stars. With a change in visual magnitude of 3.5 to 4.4, delta Cephei’s entire range of variability can be observed with the unaided eye. Its period of 5.366 days makes it an attractive candidate for anyone anxious to obtain ...
REACH FOR THE STARS MLK 2009
... What causes a sun like star to suddenly contract in diameter? ___________________________________ How many times will a blue giant orbit the center of the Milky Way during its life? ________________ Where are globular clusters typically found in a galaxy? ___________________ Approximately what % of ...
... What causes a sun like star to suddenly contract in diameter? ___________________________________ How many times will a blue giant orbit the center of the Milky Way during its life? ________________ Where are globular clusters typically found in a galaxy? ___________________ Approximately what % of ...
Astronomers Find Extremely Large Planet
... birthplace for most of the stars in our galaxy. “It’s surprising that these new disks are so large, given that they are found in dense clusters of young stars,” Lada says. “Naively, you would think that the gravitational interactions between such stars would tend to disrupt extremely large disks, si ...
... birthplace for most of the stars in our galaxy. “It’s surprising that these new disks are so large, given that they are found in dense clusters of young stars,” Lada says. “Naively, you would think that the gravitational interactions between such stars would tend to disrupt extremely large disks, si ...
12 The Milky Way - Journigan-wiki
... from interstellar gas caught between the spiral arms of galaxies. The strong gravitational fields compress the gas creating stars that are gravitationally bound together. These clusters eventually break apart. Approximately 20,000 star clusters are believed to exist in the Milky Way. Our own Sun may ...
... from interstellar gas caught between the spiral arms of galaxies. The strong gravitational fields compress the gas creating stars that are gravitationally bound together. These clusters eventually break apart. Approximately 20,000 star clusters are believed to exist in the Milky Way. Our own Sun may ...
1 Pau Amaro Seoane - modest 15-s
... the Universe. With typical masses of 107 to 108 solar masses and half-mass radii between 10 to 100 pc they are more than a factor 1000 denser than dwarf galaxies of the same mass. They also show evidence for elevated mass-to-light ratios, which could be due to the presence of massive black holes or ...
... the Universe. With typical masses of 107 to 108 solar masses and half-mass radii between 10 to 100 pc they are more than a factor 1000 denser than dwarf galaxies of the same mass. They also show evidence for elevated mass-to-light ratios, which could be due to the presence of massive black holes 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.