Lecture10
... not too hot and not too cold, many hydrogen atoms have their electron in the n = 2 orbit: hence strong absorption ...
... not too hot and not too cold, many hydrogen atoms have their electron in the n = 2 orbit: hence strong absorption ...
Lecture 22 - Seattle Central
... What are the main stages in a high mass star’s life? What happens in the core of a high mass star at the end of its life? Why does fusion stop at Iron in high mass stars? Where do elements heavier than Iron come from? What are the two possibilities when the electron degeneracy pressure in a high mas ...
... What are the main stages in a high mass star’s life? What happens in the core of a high mass star at the end of its life? Why does fusion stop at Iron in high mass stars? Where do elements heavier than Iron come from? What are the two possibilities when the electron degeneracy pressure in a high mas ...
Document
... Modified from: http://cas.sdss.org/dr5/en/proj/teachers/basic/spectraltypes/lesson.asp When astronomers look through their telescopes, they see billions of stars. What can they learn fromThe goal of this problem set is for you to understand that astronomers classify stars on the basis of two differe ...
... Modified from: http://cas.sdss.org/dr5/en/proj/teachers/basic/spectraltypes/lesson.asp When astronomers look through their telescopes, they see billions of stars. What can they learn fromThe goal of this problem set is for you to understand that astronomers classify stars on the basis of two differe ...
Chapter 1 - A Modern View of the Universe
... Comet A relatively small and primarily icy object which orbits a star. ...
... Comet A relatively small and primarily icy object which orbits a star. ...
Be Stars
... Finally, there are Be stars that show a prominent emission spectrum of hydrogen this is because they have a rapid rate of rotation, with an equatorial rotation velocity of about 200km/s, which in relation to the suns rotation of about 2 km/s is very fast ...
... Finally, there are Be stars that show a prominent emission spectrum of hydrogen this is because they have a rapid rate of rotation, with an equatorial rotation velocity of about 200km/s, which in relation to the suns rotation of about 2 km/s is very fast ...
ILÍDIO LOPES ()
... There are several mechanisms driving the oscillations in stars. Two of the most important are the κ-mechanism (related with changes in opacity) and the stochastic driving. The κ-mechanism acts like an heat engine, converting thermal into mechanical energy. The stochastic driving is the main mechanis ...
... There are several mechanisms driving the oscillations in stars. Two of the most important are the κ-mechanism (related with changes in opacity) and the stochastic driving. The κ-mechanism acts like an heat engine, converting thermal into mechanical energy. The stochastic driving is the main mechanis ...
Pallavicini - IASF Milano
... Why observing stellar clusters in X-rays • Open clusters constitute homogeneous samples of stars with approximately the same age, distance and chemical composition ...
... Why observing stellar clusters in X-rays • Open clusters constitute homogeneous samples of stars with approximately the same age, distance and chemical composition ...
Our Star - the Sun
... detected and analyzed, even though the system may be so distant or the two stars so close together that the two star images cannot be resolved A spectrum binary appears to be a single star but has a spectrum with the absorption lines for two distinctly different spectral types A spectroscopic binary ...
... detected and analyzed, even though the system may be so distant or the two stars so close together that the two star images cannot be resolved A spectrum binary appears to be a single star but has a spectrum with the absorption lines for two distinctly different spectral types A spectroscopic binary ...
Lecture 18
... • The free-fall time was ~105 years, and the clouds must span 0.01-100 solar masses, with smaller masses being much more common • The contracting cloud forms a disk, with a central condensation called a protostar. ...
... • The free-fall time was ~105 years, and the clouds must span 0.01-100 solar masses, with smaller masses being much more common • The contracting cloud forms a disk, with a central condensation called a protostar. ...
monkeyball_lifecycleofastar
... atoms which gives it the Bright red color. When this happens in billions Of years if there are still Humans, all life will be fried. ...
... atoms which gives it the Bright red color. When this happens in billions Of years if there are still Humans, all life will be fried. ...
Stars: from Adolescence to Old Age
... As the helium is quickly used up in the fusion into carbon and oxygen, gravity will once more take over The situation is analogous to the end of the main sequence 4 August 2005 ...
... As the helium is quickly used up in the fusion into carbon and oxygen, gravity will once more take over The situation is analogous to the end of the main sequence 4 August 2005 ...
More about the game plan:
... • Orbital velocity of stars different than pattern speed • Stars, gas bunch up at position of spiral arms • Causes higher grav. potential • Unclear if self-sustaining or forced. ...
... • Orbital velocity of stars different than pattern speed • Stars, gas bunch up at position of spiral arms • Causes higher grav. potential • Unclear if self-sustaining or forced. ...
SOLUTIONS TO PROBLEM SET # 3
... would be within a Hubble distance of us? Dividing this number of atoms by the volume of space within a Hubble distance of us, show how many hydrogen atoms there would be, on average, per cubic meter of the visible universe. The number of stars within a Hubble distance of us is Nstar = 3.33 × 1022 . ...
... would be within a Hubble distance of us? Dividing this number of atoms by the volume of space within a Hubble distance of us, show how many hydrogen atoms there would be, on average, per cubic meter of the visible universe. The number of stars within a Hubble distance of us is Nstar = 3.33 × 1022 . ...
Constellation Part II readingConstellation Part II reading(es)
... Why Do Most Stars and Constellations Move? The stars are distant objects. Their distances vary, but they are all very far away. Excluding our Sun, the nearest star, Proxima Centauri, is more than 4 light years away. As Earth spins on its axis, we, as Earth-bound observers, spin past this background ...
... Why Do Most Stars and Constellations Move? The stars are distant objects. Their distances vary, but they are all very far away. Excluding our Sun, the nearest star, Proxima Centauri, is more than 4 light years away. As Earth spins on its axis, we, as Earth-bound observers, spin past this background ...
Fossil Galaxies
... least luminous, most dark-matter-dominated, and least chemically evolved galaxies known. These systems are thought to be some of the tiniest, oldest, and most pristine galaxies in the universe. The Sloan survey uncovered more than a dozen of these galaxies in the Milky Way’s neighborhood while scann ...
... least luminous, most dark-matter-dominated, and least chemically evolved galaxies known. These systems are thought to be some of the tiniest, oldest, and most pristine galaxies in the universe. The Sloan survey uncovered more than a dozen of these galaxies in the Milky Way’s neighborhood while scann ...
Groups of Stars
... Spherical shape Generally older stars Surround the galaxy • Out of galaxy plane ...
... Spherical shape Generally older stars Surround the galaxy • Out of galaxy plane ...
About SDSS - Astro Projects
... the number of stars you can see rises to about 10,000, and with a 15 cm telescope more than two million can be seen. The bigger the telescope, the more light it gathers, so the fainter the stars and other objects that it can see. ...
... the number of stars you can see rises to about 10,000, and with a 15 cm telescope more than two million can be seen. The bigger the telescope, the more light it gathers, so the fainter the stars and other objects that it can see. ...
Word
... Sword are distinctive patterns to look for; the shoulder star Betelgeuse is a very bright red star while the bright blue star Rigel is in the hunter’s knee. (We’ll talk about the colors of stars later.) Also, take a look nearly overhead and you should be able to see the Pleiades star cluster. (You m ...
... Sword are distinctive patterns to look for; the shoulder star Betelgeuse is a very bright red star while the bright blue star Rigel is in the hunter’s knee. (We’ll talk about the colors of stars later.) Also, take a look nearly overhead and you should be able to see the Pleiades star cluster. (You m ...
Stellar Evolution Before…..During……and After…. The Main
... • The length of time a star spends fusing hydrogen into helium is called its main sequence lifetime ...
... • The length of time a star spends fusing hydrogen into helium is called its main sequence lifetime ...
Sample Midterm - IUPUI Physics
... 1) A) For a brief period after the Hydrogen in a core of a star is all fused to Helium where does the energy that a star needs to survive come from (before it starts to fuse Helium) and how does that affect the size and temperature of the surface of the star? B) What is the process by which Helium ( ...
... 1) A) For a brief period after the Hydrogen in a core of a star is all fused to Helium where does the energy that a star needs to survive come from (before it starts to fuse Helium) and how does that affect the size and temperature of the surface of the star? B) What is the process by which Helium ( ...
Lecture 13
... • These stars have finished fusing H to He in their cores are no longer on the main sequence. • They may be fusing He to Carbon in their core or fusing H to He in shell outside the core … but there is no H to He fusion in the core. • All stars become larger and redder after exhausting their core hyd ...
... • These stars have finished fusing H to He in their cores are no longer on the main sequence. • They may be fusing He to Carbon in their core or fusing H to He in shell outside the core … but there is no H to He fusion in the core. • All stars become larger and redder after exhausting their core hyd ...
Document
... surface temperature. For example, a Sun-like star with a surface temperature of 6000K is yellow. Taking images of stars in a few wide-spectrum bands and taking the ratio of intensities thus can be a very CHEAP way of characterizing them. ...
... surface temperature. For example, a Sun-like star with a surface temperature of 6000K is yellow. Taking images of stars in a few wide-spectrum bands and taking the ratio of intensities thus can be a very CHEAP way of characterizing them. ...
Chapter16
... exponents such as those in the mass-luminosity relation (Figure 16.21). A reminder of the meaning of non-integer exponents might be a good idea. Even if they have trouble with the concept, however, they should be able to use most calculators to do problems involving the use of non-integer exponents. ...
... exponents such as those in the mass-luminosity relation (Figure 16.21). A reminder of the meaning of non-integer exponents might be a good idea. Even if they have trouble with the concept, however, they should be able to use most calculators to do problems involving the use of non-integer exponents. ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.