The Milky Way Galaxy
... Herschel didn’t know about different kinds of stars, he thought they were all the same (like the sun) and therefore all the same luminosity. Using this assumption, he could just simply compute the distance from the brightness. Brightness = Luminosity/(distance)2 ...
... Herschel didn’t know about different kinds of stars, he thought they were all the same (like the sun) and therefore all the same luminosity. Using this assumption, he could just simply compute the distance from the brightness. Brightness = Luminosity/(distance)2 ...
Geochemistry & Lab
... + asteroids + comets +others ▪ Star + star + .. Galaxy < Galaxy group < Universe A star may be the elementary constituent of ...
... + asteroids + comets +others ▪ Star + star + .. Galaxy < Galaxy group < Universe A star may be the elementary constituent of ...
The Milky Way – A Classic Galaxy
... How old is the Milky Way? • Globular clusters again are the clue… • As we saw, we can age date any star cluster… • The main sequence is a mass sequence; higher mass stars live shorter lives. • We use stellar evolution models and take advantage of the fact that all stars in a cluster are born at the ...
... How old is the Milky Way? • Globular clusters again are the clue… • As we saw, we can age date any star cluster… • The main sequence is a mass sequence; higher mass stars live shorter lives. • We use stellar evolution models and take advantage of the fact that all stars in a cluster are born at the ...
Measuring the Stars
... • 1990: A few hundred stellar parallaxes measured by now, out to about 100 lightyears. Atmospheric blurring makes further measurements from earth’s surface virtually impossible. • 1990’s: “Hipparcos” satellite, launched by European Space Agency, measures more than 100,000 parallaxes, out to more tha ...
... • 1990: A few hundred stellar parallaxes measured by now, out to about 100 lightyears. Atmospheric blurring makes further measurements from earth’s surface virtually impossible. • 1990’s: “Hipparcos” satellite, launched by European Space Agency, measures more than 100,000 parallaxes, out to more tha ...
The Life Cycle of Stars
... mass to other stars like Sirius, and Proxima Centauri. Based on its mass, will our sun be around for a while? Realize that once our Sun starts to run out of hydrogen fuel and has exhausted its ability to fuse other elements like carbon and oxygen, it will become a red giant and expand in size to env ...
... mass to other stars like Sirius, and Proxima Centauri. Based on its mass, will our sun be around for a while? Realize that once our Sun starts to run out of hydrogen fuel and has exhausted its ability to fuse other elements like carbon and oxygen, it will become a red giant and expand in size to env ...
galaxies
... • has about 200 billion stars, and lots of gas and dust • is a barred-spiral (we think) • about 100,000 light-years wide • our Sun is halfway to the edge, revolving at half a million miles per hour around the center of the Galaxy • takes our Solar System about 200 million years to revolve once aroun ...
... • has about 200 billion stars, and lots of gas and dust • is a barred-spiral (we think) • about 100,000 light-years wide • our Sun is halfway to the edge, revolving at half a million miles per hour around the center of the Galaxy • takes our Solar System about 200 million years to revolve once aroun ...
AN INTRODUCTION TO ASTRONOMY Dr. Uri Griv Department of Physics, Ben-Gurion University
... Tel.: 08-6428226 Email: [email protected] ...
... Tel.: 08-6428226 Email: [email protected] ...
Chapter 15 (Star Lives)
... B. only their temperatures. C. heliocentric parallax and density. D. measuring the sizes of eclipsing binary systems. 20. Once you know about the H-R diagram, you can determine a star's luminosity if you: A. know its “type” and measure its temperature. B. know its distance and mass. C. know its size ...
... B. only their temperatures. C. heliocentric parallax and density. D. measuring the sizes of eclipsing binary systems. 20. Once you know about the H-R diagram, you can determine a star's luminosity if you: A. know its “type” and measure its temperature. B. know its distance and mass. C. know its size ...
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. ...
Death of Stars
... - a sparse interstellar medium Stars form in dense clouds of this medium Gravity of denser parts of the cloud starts to attract surrounding material Increased rotation of core may lead to fragmentation that forms clusters and, later, planets Restricted movement across magnetic fields causes a disc t ...
... - a sparse interstellar medium Stars form in dense clouds of this medium Gravity of denser parts of the cloud starts to attract surrounding material Increased rotation of core may lead to fragmentation that forms clusters and, later, planets Restricted movement across magnetic fields causes a disc t ...
File
... Supergiants are the largest and brightest stars in the galaxy. Red supergiants are larger than blue ones, but less hot. When a large star runs out of hydrogen to fuse, it expands to become a red giant. When it reaches the stage of burning helium to carbon, it expands and become a red supergiant. Thr ...
... Supergiants are the largest and brightest stars in the galaxy. Red supergiants are larger than blue ones, but less hot. When a large star runs out of hydrogen to fuse, it expands to become a red giant. When it reaches the stage of burning helium to carbon, it expands and become a red supergiant. Thr ...
Stellar Evolution
... When all the hydrogen is consumed, the core no longer has outward pressure supporting it, and will contract The core will grow hotter, the heat is radiated outward and expands the surface As the surface expands, it cools down, producing its reddish color The core will eventually reach a temperature ...
... When all the hydrogen is consumed, the core no longer has outward pressure supporting it, and will contract The core will grow hotter, the heat is radiated outward and expands the surface As the surface expands, it cools down, producing its reddish color The core will eventually reach a temperature ...
Final Review Questions. 1. Compare the atmospheric scale height of
... n = 1017 cm−3 ? 25. Go back to Worksheet #10 and do it again! Make sure to explain why a solar MS star evolves the way it does off the MS. Is the mass of the star constant during this evolution? 26. Derive the mass-radius relationship for white dwarfs in the non-relativistic limit. 27. Why do object ...
... n = 1017 cm−3 ? 25. Go back to Worksheet #10 and do it again! Make sure to explain why a solar MS star evolves the way it does off the MS. Is the mass of the star constant during this evolution? 26. Derive the mass-radius relationship for white dwarfs in the non-relativistic limit. 27. Why do object ...
Dead Stars - University of Iowa Astrophysics
... scattered throughout space are a galaxy’s memory of its past glory. Because no fusion occurs in their interiors, white dwarfs simply cool off at an essentially constant radius as they slowly deplete their supply of thermal energy”…Carroll and Ostlie, “Modern Astrophysics” ...
... scattered throughout space are a galaxy’s memory of its past glory. Because no fusion occurs in their interiors, white dwarfs simply cool off at an essentially constant radius as they slowly deplete their supply of thermal energy”…Carroll and Ostlie, “Modern Astrophysics” ...
SHELL H II REGIONS IN NGC 6334
... • That is, if we know a, the semimajor axis of the orbit, and P, the orbital period, we can find m+M, the sum of the masses of the two stars. But, how can we study very young stars that form inside clouds with high obscuration and that cannot be studied with the usual optical and infrared techniques ...
... • That is, if we know a, the semimajor axis of the orbit, and P, the orbital period, we can find m+M, the sum of the masses of the two stars. But, how can we study very young stars that form inside clouds with high obscuration and that cannot be studied with the usual optical and infrared techniques ...
Components of Universe
... Galaxies contain more than just stars. The irregular-looking blobs are either hot (pink) or cold (dark) interstellar clouds ...
... Galaxies contain more than just stars. The irregular-looking blobs are either hot (pink) or cold (dark) interstellar clouds ...
PPT - Mr.E Science
... Nebula – a huge gas cloud made up mainly of Hydrogen that collapse down on itself and compresses the gas down into a Protostar Star is “born” when the protostar has contracting tight enough for Hydrogen to fuse into Helium, this releases the light and energy we normally associate with a “normal” sta ...
... Nebula – a huge gas cloud made up mainly of Hydrogen that collapse down on itself and compresses the gas down into a Protostar Star is “born” when the protostar has contracting tight enough for Hydrogen to fuse into Helium, this releases the light and energy we normally associate with a “normal” sta ...
Worksheet: Stars and the HR Diagram
... Background: The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were al the same distance away. Rather than speak of the br ...
... Background: The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were al the same distance away. Rather than speak of the br ...
Stars: Their Life and Afterlife
... Superbubbles are large cavities of hot, low-density plasma that are created by the collective effects of a large number of massive stars. We saw earlier in the lecture series that stars tend to form in clusters as a giant molecular cloud contracts. This means that they not only tend to form close to ...
... Superbubbles are large cavities of hot, low-density plasma that are created by the collective effects of a large number of massive stars. We saw earlier in the lecture series that stars tend to form in clusters as a giant molecular cloud contracts. This means that they not only tend to form close to ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.