Microsoft Word 97
... 1) The Nuclear Bulge – Our galaxy has the general shape of a pancake with a bulge at its center that contains millions of stars, primarily old ones. This nuclear bulge has the galactic nucleus at its center. The nucleus itself if only about 10 light-years across. 2) The Disk – The part of the pancak ...
... 1) The Nuclear Bulge – Our galaxy has the general shape of a pancake with a bulge at its center that contains millions of stars, primarily old ones. This nuclear bulge has the galactic nucleus at its center. The nucleus itself if only about 10 light-years across. 2) The Disk – The part of the pancak ...
Determination of kinetic energies of stars using Hipparcos data *
... has resulted in kind of a U-turn of the astronomical community towards stellar kinematics. This is not surprising, in view of the fact that the previous peak of the amount of works devoted to stellar kinematics was in 1930s when the General Catalogue by B. Boss became available (Boss, B. 1937). The ...
... has resulted in kind of a U-turn of the astronomical community towards stellar kinematics. This is not surprising, in view of the fact that the previous peak of the amount of works devoted to stellar kinematics was in 1930s when the General Catalogue by B. Boss became available (Boss, B. 1937). The ...
17_LectureOutline
... Once many stars are plotted on an H–R diagram, a pattern begins to form. These are the 80 closest stars to us; note the dashed lines of constant radius. The darkened curve is called the main sequence, as this is where most stars are. Also indicated is the white dwarf region; these stars are hot but ...
... Once many stars are plotted on an H–R diagram, a pattern begins to form. These are the 80 closest stars to us; note the dashed lines of constant radius. The darkened curve is called the main sequence, as this is where most stars are. Also indicated is the white dwarf region; these stars are hot but ...
Star Sizes - Fort Lewis College
... • Distances to several thousand stars are known this way. • The Hipparcos satellite extends the distance to ~200 pc, so distances to nearly one million stars can be measured with parallax. ...
... • Distances to several thousand stars are known this way. • The Hipparcos satellite extends the distance to ~200 pc, so distances to nearly one million stars can be measured with parallax. ...
Document
... Abundances of Stars: Lithium Abundance variations can also be caused by evolutionary changes in the stellar composition. An example is Lithium Lithium is destroyed at temperatures of T ≈ 2 x 106 K. The convection zone of the star brings Li to the deeper, hotter layers of the star where it is destro ...
... Abundances of Stars: Lithium Abundance variations can also be caused by evolutionary changes in the stellar composition. An example is Lithium Lithium is destroyed at temperatures of T ≈ 2 x 106 K. The convection zone of the star brings Li to the deeper, hotter layers of the star where it is destro ...
Chapter 19 Stars Galaxies and the Universe
... When telescopes were developed, scientists discovered this system had flaws. They could see more stars with the telescope than with the naked eye. They could also see the differences in brightness more clearly. The old system for classifying brightness was too general to include the dimmest stars th ...
... When telescopes were developed, scientists discovered this system had flaws. They could see more stars with the telescope than with the naked eye. They could also see the differences in brightness more clearly. The old system for classifying brightness was too general to include the dimmest stars th ...
Is Draco II one of the faintest dwarf galaxies? First study from Keck
... of stars 2 and 10, which must have very similar stellar parameters as they are confirmed Dra II member stars with almost identical colours and magnitudes ((0.53,18.87) and (0.55,18.98)), implies that these two member stars have significantly different metallicities (a 4.5σ difference in the equivale ...
... of stars 2 and 10, which must have very similar stellar parameters as they are confirmed Dra II member stars with almost identical colours and magnitudes ((0.53,18.87) and (0.55,18.98)), implies that these two member stars have significantly different metallicities (a 4.5σ difference in the equivale ...
Nebulae.The Lagoon and Dumbbell Nebulae
... The Dumbbell Nebula, also known as M27 or NGC 6853, is the first ever found planetary nebula. It is located in the Vulpecula constellation. The nebula is a remnant of a dying star which is approximately 2 times smaller than the Sun. The star is hot and blue with temperature of 85000K (Most of these ...
... The Dumbbell Nebula, also known as M27 or NGC 6853, is the first ever found planetary nebula. It is located in the Vulpecula constellation. The nebula is a remnant of a dying star which is approximately 2 times smaller than the Sun. The star is hot and blue with temperature of 85000K (Most of these ...
Teacher`s Guide - Cornell Science Inquiry Partnerships
... Astronomy, Earth Science Audience This activity is aimed at a high school audience, but it could easily be modified for use with middle school students. Time Required The essential activities can be covered in 40 minutes, or the entire project can be stretched to 4 hours or even much longer. (In the ...
... Astronomy, Earth Science Audience This activity is aimed at a high school audience, but it could easily be modified for use with middle school students. Time Required The essential activities can be covered in 40 minutes, or the entire project can be stretched to 4 hours or even much longer. (In the ...
Review 3 (11-18-10)
... • Neutron Stars: even denser, about mass of Sun in size of Orlando. Neutrons stop further collapse. M between 1.4 and 3 solar masses. Some neutron stars can be detected as pulsars • Black Holes: M more than 3 solar masses. Nothing stops the collapse and produces an object so compact that escape velo ...
... • Neutron Stars: even denser, about mass of Sun in size of Orlando. Neutrons stop further collapse. M between 1.4 and 3 solar masses. Some neutron stars can be detected as pulsars • Black Holes: M more than 3 solar masses. Nothing stops the collapse and produces an object so compact that escape velo ...
Galaxies Galaxies M81
... Clusters of Galaxies Rather than occurring individually in space, galaxies are grouped in clusters ranging in size from a few dozens to thousands of galaxies. The Coma Cluster, shown at right, is 300 million light years from the Milky Way and contains more than 1,000 (and possibly as many as 10,000 ...
... Clusters of Galaxies Rather than occurring individually in space, galaxies are grouped in clusters ranging in size from a few dozens to thousands of galaxies. The Coma Cluster, shown at right, is 300 million light years from the Milky Way and contains more than 1,000 (and possibly as many as 10,000 ...
Our Local Group of Galaxies
... How complete is the list of Milky Way dSph companions? • These results raise all sorts of questions: - is the ~constant (dark matter) mass a characteristic of galaxy formation, or does it say something about dark matter physics? (standard ΛCDM theory has no preferred mass scale) - see Strigari et ...
... How complete is the list of Milky Way dSph companions? • These results raise all sorts of questions: - is the ~constant (dark matter) mass a characteristic of galaxy formation, or does it say something about dark matter physics? (standard ΛCDM theory has no preferred mass scale) - see Strigari et ...
Variable Stars – II. Pulsating stars
... It’s not quite as simple as that. If the zone is too deep in the star, it cannot drive against the overlying layers and if the zone is too high, it has essentially nothing above it to drive. Placement of the zone is thus fairly critical in determining whether pulsation occurs – and explains why ther ...
... It’s not quite as simple as that. If the zone is too deep in the star, it cannot drive against the overlying layers and if the zone is too high, it has essentially nothing above it to drive. Placement of the zone is thus fairly critical in determining whether pulsation occurs – and explains why ther ...
Document
... Venn & Lambert (2008) have argued that this may not be the case. Peculiar stars such as post AGB stars and l Boo stars have iron abundances as low as [Fe/H] ~ –5. These are thought to be due to the separation of gas and dust beyond the stellar surface followed by an accretion of the dust-depleted g ...
... Venn & Lambert (2008) have argued that this may not be the case. Peculiar stars such as post AGB stars and l Boo stars have iron abundances as low as [Fe/H] ~ –5. These are thought to be due to the separation of gas and dust beyond the stellar surface followed by an accretion of the dust-depleted g ...
The Origin, Structure, and Evolution of the Stars
... the evolutionary tracks of stars off the main-sequence and also gives the time spent as main-sequence stars for stars in different regions of the H-R diagram. Our calculations indicate that the more massive stars “burn” their fuel so rapidly they cannot last very long. Some of these bright stars mus ...
... the evolutionary tracks of stars off the main-sequence and also gives the time spent as main-sequence stars for stars in different regions of the H-R diagram. Our calculations indicate that the more massive stars “burn” their fuel so rapidly they cannot last very long. Some of these bright stars mus ...
The Star Finder Book - Starpath School of Navigation
... Under cloudy skies, the extreme value of accurate dead reckoning becomes clear very soon. But this is not the subject at hand, and improving dead reckoning procedure is easily accommodated underway without special training. The problem with cloudy skies we cover here is that of identifying unknown s ...
... Under cloudy skies, the extreme value of accurate dead reckoning becomes clear very soon. But this is not the subject at hand, and improving dead reckoning procedure is easily accommodated underway without special training. The problem with cloudy skies we cover here is that of identifying unknown s ...
Chapter14(4-7-11)
... After leaving the main sequence red giants eject their outer layers back to the interstellar medium Supernovae explode and eject their outer layers back to the interstellar medium Supernova explosions and other events can compress an interstellar cloud of gas and dust that collapses to form stars …… ...
... After leaving the main sequence red giants eject their outer layers back to the interstellar medium Supernovae explode and eject their outer layers back to the interstellar medium Supernova explosions and other events can compress an interstellar cloud of gas and dust that collapses to form stars …… ...
... 3. THE RR LYRAE STARS IN M15 In Clement’s (2002) data base of variables stars, a total of 158 variable stars are known, from which approximately 104 are RR Lyrae type stars. In this work, 33 known RR Lyrae stars, identified in Figs. 1 and 2 and listed in Table 4, have been studied. For all the stars ...
Astronomy and the Coal Age of Alabama
... The Big Dipper would have looked virtually the same to the ancient Egyptians, but 100,000 years ago it looked different. It will further lose its familiar shape in the future. Its 7 bright stars are not all at the same distance. This kind of thing can’t be extrapolated too far backward or forward i ...
... The Big Dipper would have looked virtually the same to the ancient Egyptians, but 100,000 years ago it looked different. It will further lose its familiar shape in the future. Its 7 bright stars are not all at the same distance. This kind of thing can’t be extrapolated too far backward or forward i ...
Corona Australis
Corona Australis /kɵˈroʊnə ɒˈstreɪlɨs/ or Corona Austrina /kɵˈroʊnə ɒˈstraɪnə/ is a constellation in the Southern Celestial Hemisphere. Its Latin name means ""southern crown"", and it is the southern counterpart of Corona Borealis, the northern crown. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations. The Ancient Greeks saw Corona Australis as a wreath rather than a crown and associated it with Sagittarius or Centaurus. Other cultures have likened the pattern to a turtle, ostrich nest, a tent, or even a hut belonging to a rock hyrax.Although fainter than its namesake, the oval- or horseshoe-shaped pattern of its brighter stars renders it distinctive. Alpha and Beta Coronae Australis are the two brightest stars with an apparent magnitude of around 4.1. Epsilon Coronae Australis is the brightest example of a W Ursae Majoris variable in the southern sky. Lying alongside the Milky Way, Corona Australis contains one of the closest star-forming regions to our Solar System—a dusty dark nebula known as the Corona Australis Molecular Cloud, lying about 430 light years away. Within it are stars at the earliest stages of their lifespan. The variable stars R and TY Coronae Australis light up parts of the nebula, which varies in brightness accordingly.