The First Stars - Amazon Web Services
... see no relic stars totally lacking in heavier elements such as iron, as would be the case if there was a component of low mass objects in the first generation of stars. We infer that during their short but brilliant lives, aided by large numbers of star-forming dwarf galaxies, also teeming with mass ...
... see no relic stars totally lacking in heavier elements such as iron, as would be the case if there was a component of low mass objects in the first generation of stars. We infer that during their short but brilliant lives, aided by large numbers of star-forming dwarf galaxies, also teeming with mass ...
Lecture (Powerpoint)
... the mass of the Sun, or ~80 Jupiter masses) never ``turn on'' Central temperatures never get hot enough for nuclear burning to begin in earnest Nuclear burning is what powers the star through its life Star sits around as a brown dwarf – too big and hot to be a planet, too small and cold to be a real ...
... the mass of the Sun, or ~80 Jupiter masses) never ``turn on'' Central temperatures never get hot enough for nuclear burning to begin in earnest Nuclear burning is what powers the star through its life Star sits around as a brown dwarf – too big and hot to be a planet, too small and cold to be a real ...
Lab 8: Stellar Classification and the H
... luminosity class (ex. a I indicates a supergiant, a III a giant star, and a V a main sequence star). In this new system, our Sun (a typical main-sequence star) becomes a G2V. Spectral type allows astronomers to know not only the temperature of the star, but also its luminosity and color. These prope ...
... luminosity class (ex. a I indicates a supergiant, a III a giant star, and a V a main sequence star). In this new system, our Sun (a typical main-sequence star) becomes a G2V. Spectral type allows astronomers to know not only the temperature of the star, but also its luminosity and color. These prope ...
Galaxies and the Universe bb
... • Around the galactic nucleus • Outermost stars move the slowest • Sun rotates around the galactic nucleus once about every 200 million years ...
... • Around the galactic nucleus • Outermost stars move the slowest • Sun rotates around the galactic nucleus once about every 200 million years ...
Published by the Association Pro ISSI No. 37, May 2016
... Stars are born during the collapse of giant nebulae that are large interstellar clouds of dust, hydrogen, helium and other ionized gases, (Fig. 2) . These clouds are really huge, they may measure several light years across. They are not stable in the long run; rather, internal turbulences cause knot ...
... Stars are born during the collapse of giant nebulae that are large interstellar clouds of dust, hydrogen, helium and other ionized gases, (Fig. 2) . These clouds are really huge, they may measure several light years across. They are not stable in the long run; rather, internal turbulences cause knot ...
Oct - Seattle Astronomical Society
... boom. Clouds of interstellar gas within the two galaxies press against one another and collapse to form stars, dozens to hundreds at a time. This isn’t the first time astronomers have witnessed a galaxy producing so many stars. “There are some other extreme starburst ...
... boom. Clouds of interstellar gas within the two galaxies press against one another and collapse to form stars, dozens to hundreds at a time. This isn’t the first time astronomers have witnessed a galaxy producing so many stars. “There are some other extreme starburst ...
Interacting Galaxies
... can lead to spectacular mergers and spawn vast amounts of new star formation. Astronomers estimate that in the nearby universe, 1 out of every 20 gas-rich disk galaxies, like our Milky Way galaxy, is in the act of colliding. Galaxy mergers were much more common in the past, however, when the expandi ...
... can lead to spectacular mergers and spawn vast amounts of new star formation. Astronomers estimate that in the nearby universe, 1 out of every 20 gas-rich disk galaxies, like our Milky Way galaxy, is in the act of colliding. Galaxy mergers were much more common in the past, however, when the expandi ...
File - YEAR 11 EBSS PHYSICS DETAILED STUDIES
... star. After some careful observation, a relationship was established between mass an luminosity. L is proportional to m3, so a star twice as heavy as the sun will be eight times as bright. ...
... star. After some careful observation, a relationship was established between mass an luminosity. L is proportional to m3, so a star twice as heavy as the sun will be eight times as bright. ...
Announcements - Lick Observatory
... Galaxy, but for the vast majority, the separation of the stars is large enough that one star doesn’t affect the evolution of the other(s). ...
... Galaxy, but for the vast majority, the separation of the stars is large enough that one star doesn’t affect the evolution of the other(s). ...
Supermassive Black Holes in Inactive Galaxies Encyclopedia of Astronomy & Astrophysics eaa.iop.org
... M31 is the highest-luminosity galaxy in the LOCAL GROUP. At a distance of 0.77 Mpc, it is the nearest giant galaxy outside our own. It can therefore be studied in unusual detail. M31 contains the nearest example of a nuclear star cluster embedded in a normal bulge. When examined with HST, the nucleu ...
... M31 is the highest-luminosity galaxy in the LOCAL GROUP. At a distance of 0.77 Mpc, it is the nearest giant galaxy outside our own. It can therefore be studied in unusual detail. M31 contains the nearest example of a nuclear star cluster embedded in a normal bulge. When examined with HST, the nucleu ...
Slide 1
... End of H He burning in the core of MS star Red Giant phase with inert He-core and outer H-burning shell; star expands and cools, but is brighter Climbs up the RG branch until He-flash in the core Core expands and cools; H-burning decreases; outer layers contract; luminosity decreases but temperatu ...
... End of H He burning in the core of MS star Red Giant phase with inert He-core and outer H-burning shell; star expands and cools, but is brighter Climbs up the RG branch until He-flash in the core Core expands and cools; H-burning decreases; outer layers contract; luminosity decreases but temperatu ...
A Star is
... • Apparent magnitude: brightness of a star as seen from the Earth. • Absolute magnitude: brightness a star would have at a distance of 32.6 light-years from Earth ...
... • Apparent magnitude: brightness of a star as seen from the Earth. • Absolute magnitude: brightness a star would have at a distance of 32.6 light-years from Earth ...
Mass and composition determine most of the properties of a star
... across the street, which light would appear brighter? You cannot tell by looking in the sky how bright a star truly is. The farther away the star is, the less bright it will appear. ...
... across the street, which light would appear brighter? You cannot tell by looking in the sky how bright a star truly is. The farther away the star is, the less bright it will appear. ...
Introduction
... A galaxy is a self-gravitating system composed of an interstellar medium, stars, and dark matter. It’s difficult to overstate the role of gravity in galaxies. While the electromagnetic force has the same r 2 dependence as gravity, charge cancellation insures that large-scale electromagnetic forces a ...
... A galaxy is a self-gravitating system composed of an interstellar medium, stars, and dark matter. It’s difficult to overstate the role of gravity in galaxies. While the electromagnetic force has the same r 2 dependence as gravity, charge cancellation insures that large-scale electromagnetic forces a ...
ON THE FORMATION OF MASSIVE STELLAR CLUSTERS
... Richtler 2000 and Larsen 1999). This star-forming activity in which masses similar to the total gas content found in galactic giant molecular clouds (massive elongated structures that extend over 100 pc in length) are turned into stars, all in a very small volume (∼ few pc) much smaller than the typ ...
... Richtler 2000 and Larsen 1999). This star-forming activity in which masses similar to the total gas content found in galactic giant molecular clouds (massive elongated structures that extend over 100 pc in length) are turned into stars, all in a very small volume (∼ few pc) much smaller than the typ ...
StarCharacteristics
... across the street, which light would appear brighter? You cannot tell by looking in the sky how bright a star truly is. The farther away the star is, the less bright it will appear. ...
... across the street, which light would appear brighter? You cannot tell by looking in the sky how bright a star truly is. The farther away the star is, the less bright it will appear. ...
Stellar Evolution
... It can be seen from this H–R diagram that stars more massive than the Sun follow very different paths when leaving the main sequence: ...
... It can be seen from this H–R diagram that stars more massive than the Sun follow very different paths when leaving the main sequence: ...
solar.gmu.edu
... •A quasar’s luminosity can be calculated from its apparent brightness and the distance using the inverse-square law •Even though small, the luminosity of a quasar (1038 to 1042 Watts) can be very larger, i.e., several thousand times more than the entire Milly Way Galaxies (1037). •A quasar has emiss ...
... •A quasar’s luminosity can be calculated from its apparent brightness and the distance using the inverse-square law •Even though small, the luminosity of a quasar (1038 to 1042 Watts) can be very larger, i.e., several thousand times more than the entire Milly Way Galaxies (1037). •A quasar has emiss ...
Document
... • The length of time a star spends fusing hydrogen into helium is called its main sequence lifetime. – Stars spend most of their lives on the main sequence. – Lifetime depends on the star’s mass and luminosity. • More luminous stars burn their energy more rapidly than less luminous stars.. • High-ma ...
... • The length of time a star spends fusing hydrogen into helium is called its main sequence lifetime. – Stars spend most of their lives on the main sequence. – Lifetime depends on the star’s mass and luminosity. • More luminous stars burn their energy more rapidly than less luminous stars.. • High-ma ...
Stellar Evolution Guiding Questions Stars Evolve
... 2. What kind of matter exists in the spaces between the stars? 3. What steps are involved in forming a star like the Sun? 4. When a star forms, why does it end up with only a fraction of the available matter? 5. What do star clusters tell us about the formation of stars? 6. Where in the Galaxy does ...
... 2. What kind of matter exists in the spaces between the stars? 3. What steps are involved in forming a star like the Sun? 4. When a star forms, why does it end up with only a fraction of the available matter? 5. What do star clusters tell us about the formation of stars? 6. Where in the Galaxy does ...
Galaxy Evolution
... All measurements are within r500. Overplotted are the best-fit relations for the Vikhlinin et al. (2006) sample gas mass fractions and for our stellar mass fractions. The WMAP 1 ! confidence region for the universal baryon fraction from Spergel et al. (2006) is shown for comparison, and the right-ha ...
... All measurements are within r500. Overplotted are the best-fit relations for the Vikhlinin et al. (2006) sample gas mass fractions and for our stellar mass fractions. The WMAP 1 ! confidence region for the universal baryon fraction from Spergel et al. (2006) is shown for comparison, and the right-ha ...
Transcript - Chandra X
... the red giant stage as it evolves through the Mira instability strip on the H-R diagram. Plotting the pulsations of Mira variable stars – which are basically changes in brightness – over time results in a plot called a light curve which shows the unique behavior of Mira variables. The light curve sh ...
... the red giant stage as it evolves through the Mira instability strip on the H-R diagram. Plotting the pulsations of Mira variable stars – which are basically changes in brightness – over time results in a plot called a light curve which shows the unique behavior of Mira variables. The light curve sh ...
Serpens
Serpens (""the Serpent"", Greek Ὄφις) is a constellation of the northern hemisphere. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical Union. It is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent's Head) to the west and Serpens Cauda (Serpent's Tail) to the east. Between these two halves lies the constellation of Ophiuchus, the ""Serpent-Bearer"". In figurative representations, the body of the serpent is represented as passing behind Ophiuchus between Mu Serpentis in Serpens Caput and Nu Serpentis in Serpens Cauda.The brightest star in Serpens is the red giant star Alpha Serpentis, or Unukalhai, in Serpens Caput, with an apparent magnitude of 2.63. Also located in Serpens Caput are the naked-eye globular cluster Messier 5 and the naked-eye variables R Serpentis and Tau4 Serpentis. Notable extragalactic objects include Seyfert's Sextet, one of the densest galaxy clusters known; Arp 220, the prototypical ultraluminous infrared galaxy; and Hoag's Object, the most famous of the very rare class of galaxies known as ring galaxies.Part of the Milky Way's galactic plane passes through Serpens Cauda, which is therefore rich in galactic deep-sky objects, such as the Eagle Nebula (IC 4703) and its associated star cluster Messier 16. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. Other striking objects include the Red Square Nebula, one of the few objects in astronomy to take on a square shape; and Westerhout 40, a massive nearby star-forming region consisting of a molecular cloud and an H II region.