Lecture 12: Age, Metalicity, and Observations Abundance
... SFR(M " yr #1 ) = 7.9 $10#42 L(H% )(ergs#1 ) = 1.08 $10#53 Q(H o )(s#1 ) Q(H o ) is the ionising photon luminosity constants are derived from evol. synthesis models (e.g., Kennicutt 1982) ...
... SFR(M " yr #1 ) = 7.9 $10#42 L(H% )(ergs#1 ) = 1.08 $10#53 Q(H o )(s#1 ) Q(H o ) is the ionising photon luminosity constants are derived from evol. synthesis models (e.g., Kennicutt 1982) ...
The Milky Way
... Distant galaxies are moving away from our Milky Way, with a recession velocity, vr, proportional to their distance d: ...
... Distant galaxies are moving away from our Milky Way, with a recession velocity, vr, proportional to their distance d: ...
Stability and formation of the fractal
... Stability of the molecular disk Usual homogeneous disk: the Toomre criterion Collaboration between the pressure at small-scale and the rotation at large-scale Small-scale: Jeans criterion λJ = σ tff = σ/(2π Gρ)1/2 in 2D (disk) Σ = h ρ and h = σ2 / ( 2π G Σ ) ==> λJ = σ2 / ( 2π G Σ ) = h Large-scale ...
... Stability of the molecular disk Usual homogeneous disk: the Toomre criterion Collaboration between the pressure at small-scale and the rotation at large-scale Small-scale: Jeans criterion λJ = σ tff = σ/(2π Gρ)1/2 in 2D (disk) Σ = h ρ and h = σ2 / ( 2π G Σ ) ==> λJ = σ2 / ( 2π G Σ ) = h Large-scale ...
PPT - Cornell University
... • Protogalaxies acquire angular momentum through tidal torques with nearest neighbors during the linear regime [Stromberg 1934; Hoyle 1949] • As self-gravity decouples the protogalaxy from the Hubble flow, [l/(d l/d t)] becomes v.large and the growth of l ceases ...
... • Protogalaxies acquire angular momentum through tidal torques with nearest neighbors during the linear regime [Stromberg 1934; Hoyle 1949] • As self-gravity decouples the protogalaxy from the Hubble flow, [l/(d l/d t)] becomes v.large and the growth of l ceases ...
Future Directions for Astronomy at MSU The lab The rest
... • Find through long-term monitoring of radial velocity variations ...
... • Find through long-term monitoring of radial velocity variations ...
22 October: The Formation of Stars
... there are young stars. • When we see massive main sequence stars (spectral class O), we know they are young. • With fairly simple observations, we can find groups of O and B stars (OB associations) ...
... there are young stars. • When we see massive main sequence stars (spectral class O), we know they are young. • With fairly simple observations, we can find groups of O and B stars (OB associations) ...
Problem 4 : a. (20 points)
... From Table A4-1, the nearest star to us is 1.31 pc, so the local density of stars is something less than one per cubic parsec. This is consistent with one of our past studio exercises (on interstellar reddening) where we were told that the local density of stars is something like 0.1 per cubic parse ...
... From Table A4-1, the nearest star to us is 1.31 pc, so the local density of stars is something less than one per cubic parsec. This is consistent with one of our past studio exercises (on interstellar reddening) where we were told that the local density of stars is something like 0.1 per cubic parse ...
The Universe and Galaxies - West Jefferson Local Schools
... 2. ________ (fig. 26-16, pg. 832) most ________ type of galaxy - spherical and ________ shaped NO spiral arms, little dust and gas - generally have ________ stars (reddish in color) - Range of sizes a. ________ - trillions of stars, millions of light years in diameter b. ________ - millions of s ...
... 2. ________ (fig. 26-16, pg. 832) most ________ type of galaxy - spherical and ________ shaped NO spiral arms, little dust and gas - generally have ________ stars (reddish in color) - Range of sizes a. ________ - trillions of stars, millions of light years in diameter b. ________ - millions of s ...
The Universe and Galaxies - West Jefferson Local Schools
... 2. ________ (fig. 26-16, pg. 832) most ________ type of galaxy - spherical and ________ shaped NO spiral arms, little dust and gas - generally have ________ stars (reddish in color) - Range of sizes a. ________ - trillions of stars, millions of light years in diameter b. ________ - millions of ...
... 2. ________ (fig. 26-16, pg. 832) most ________ type of galaxy - spherical and ________ shaped NO spiral arms, little dust and gas - generally have ________ stars (reddish in color) - Range of sizes a. ________ - trillions of stars, millions of light years in diameter b. ________ - millions of ...
Universe of Learning Science Briefing: Our Home, the Milky Way
... Going from 2d to 3d : Turning Pictures into a Galactic Map There are no rulers that can be observed in our Galaxy. But there are types of stars called Red Clump Giants for which we know the intrinsic brightness. They are also fairly common and bright and can be used to trace the structure of the Ga ...
... Going from 2d to 3d : Turning Pictures into a Galactic Map There are no rulers that can be observed in our Galaxy. But there are types of stars called Red Clump Giants for which we know the intrinsic brightness. They are also fairly common and bright and can be used to trace the structure of the Ga ...
Coming Home - Marcia Bartusiak
... he enigmatic infrared objects do not resemble individual stars; one looks like it might be a particularly dense and energetic cluster of stars. Whatever they are, their combined power could account for much of the hubbub in the galactic cen ter. If so, then there is no need for a supermassive black ...
... he enigmatic infrared objects do not resemble individual stars; one looks like it might be a particularly dense and energetic cluster of stars. Whatever they are, their combined power could account for much of the hubbub in the galactic cen ter. If so, then there is no need for a supermassive black ...
The Pulsar “Lighthouse”
... • Degenerate pressure of neutrons can support stars only up to 3M • For M > 3M: Further collapse Î black hole • Mass is so concentrated that light cannot escape. • One way to think about it: – vescape = 2GM/R becomes greater than speed of light. – So photons can’t escape. • Black holes now known o ...
... • Degenerate pressure of neutrons can support stars only up to 3M • For M > 3M: Further collapse Î black hole • Mass is so concentrated that light cannot escape. • One way to think about it: – vescape = 2GM/R becomes greater than speed of light. – So photons can’t escape. • Black holes now known o ...
The Sun and Stardust
... How are other elements made? Massive stars burn their hydrogen (and helium and carbon-nitrogen-oxygen) very quickly. At the end of their life heavier (metals) are formed such as vanadium, chromium, manganese, iron, cobalt, and nickel etc. Then massive stars (about ten times more massive than the Su ...
... How are other elements made? Massive stars burn their hydrogen (and helium and carbon-nitrogen-oxygen) very quickly. At the end of their life heavier (metals) are formed such as vanadium, chromium, manganese, iron, cobalt, and nickel etc. Then massive stars (about ten times more massive than the Su ...
Living alongside Monsters: Matter around Central Massive Black Holes Q. Daniel Wang
... Great Observatory Survey of the GC ...
... Great Observatory Survey of the GC ...
Unit Review Answers - click here
... together. The outer planets are much farther away from the Sun (outer part of the solar system) and have gaseous compositions, so they should be classified together. 17. large, mainly gas composition; have lots of moons, rings systems; cold temperatures. 18. Pluto is neither gas giant nor a terrestr ...
... together. The outer planets are much farther away from the Sun (outer part of the solar system) and have gaseous compositions, so they should be classified together. 17. large, mainly gas composition; have lots of moons, rings systems; cold temperatures. 18. Pluto is neither gas giant nor a terrestr ...
lecture27
... can exceed one billion solar masses. Observations of the rapid variability of active galactic nuclei tells us that their energy output comes from quite a small region, while Doppler shifts of orbiting gas clouds tell us that the central region contains an enormous amount of mass. The only known way ...
... can exceed one billion solar masses. Observations of the rapid variability of active galactic nuclei tells us that their energy output comes from quite a small region, while Doppler shifts of orbiting gas clouds tell us that the central region contains an enormous amount of mass. The only known way ...
スライド 1 - Astrophyics Lab. in Kagoshima University
... What is currently hot topics in (radio) astronomy? • New type of radio sources (e.g. fast radio bursts) • Newly found phase of star formation and stellar evolution • Newly discovered gas dynamics • New characteristics of a black hole, a high-envergy object, and interstellar medium • Innovative resea ...
... What is currently hot topics in (radio) astronomy? • New type of radio sources (e.g. fast radio bursts) • Newly found phase of star formation and stellar evolution • Newly discovered gas dynamics • New characteristics of a black hole, a high-envergy object, and interstellar medium • Innovative resea ...
슬라이드 1
... - Dynamical timescale ~ 60 Myr (assuming σ ~ 200km/s) - Even for the objects at 95kpc, the dynamical timescale < 0.5 Gyr However, the observed stellar mass in these galaxies is significantly less than ~ 1011M⊙ - 1012M⊙ in a typical local cD galaxy. → The majority of the stars have yet to form. ...
... - Dynamical timescale ~ 60 Myr (assuming σ ~ 200km/s) - Even for the objects at 95kpc, the dynamical timescale < 0.5 Gyr However, the observed stellar mass in these galaxies is significantly less than ~ 1011M⊙ - 1012M⊙ in a typical local cD galaxy. → The majority of the stars have yet to form. ...
Freeman_DM2
... We have had a long controversy over the last few years about whether the rotation curves imply cusped or cored dark halos. This continues to be very illuminating Galaxies of low surface brightness are important in this debate. The normal or high surface brightness spirals have a fairly well defined ...
... We have had a long controversy over the last few years about whether the rotation curves imply cusped or cored dark halos. This continues to be very illuminating Galaxies of low surface brightness are important in this debate. The normal or high surface brightness spirals have a fairly well defined ...
Spiral arms in the milky way galaxy and cosmic rays
... The disk is characterized with stars that move in nearly circular orbits around the galactic center. The Central Bulge is characterized with stars with large random motions. Therefore its distribution is ellipsoidal. The star in the disk has a differential velocity, meaning the star nearer to the ce ...
... The disk is characterized with stars that move in nearly circular orbits around the galactic center. The Central Bulge is characterized with stars with large random motions. Therefore its distribution is ellipsoidal. The star in the disk has a differential velocity, meaning the star nearer to the ce ...
21. Solar System Formation
... gas can’t reach the center! It seems that jets — possibly driven by magnetic fields — may slow disk rotation and allow gas to flow in. ...
... gas can’t reach the center! It seems that jets — possibly driven by magnetic fields — may slow disk rotation and allow gas to flow in. ...
Monday, April 28
... Herschel’s Findings • Stars thinned out very fast at right angles to Milky Way • In the plane of the Milky Way the thinning was slower and depended upon the direction in which he looked • Flaws: – Observations made only in visible spectrum – Did not take into account absorption by interstellar gas ...
... Herschel’s Findings • Stars thinned out very fast at right angles to Milky Way • In the plane of the Milky Way the thinning was slower and depended upon the direction in which he looked • Flaws: – Observations made only in visible spectrum – Did not take into account absorption by interstellar gas ...
Slide 1
... Milky Way Galaxy • Consists of over 200 billion stars • 16,000 light years thick (central bulge) • 100,000 light years across (long end to end) • The arm that our solar system is in (Orion Arm) is about 30,000 light years long ...
... Milky Way Galaxy • Consists of over 200 billion stars • 16,000 light years thick (central bulge) • 100,000 light years across (long end to end) • The arm that our solar system is in (Orion Arm) is about 30,000 light years long ...
The Milky Way powepoint
... The farthest known quasar is about 12 billion light-years away. When we look out into space, out beyond the quasars, we are really looking back into time. Why are all galaxies moving away from us? Why should the galaxies farthest away from us move away the fastest? What’s so special about us? ...
... The farthest known quasar is about 12 billion light-years away. When we look out into space, out beyond the quasars, we are really looking back into time. Why are all galaxies moving away from us? Why should the galaxies farthest away from us move away the fastest? What’s so special about us? ...
word document - FacStaff Home Page for CBU
... In Section A we consider the organization and structure of all the stars and star clusters that are anywhere near us. This group of stars we call the Milky Way Galaxy. In Section B we find that by looking out beyond our own galaxy that there are other separate groups of stars, i.e., other galaxies. ...
... In Section A we consider the organization and structure of all the stars and star clusters that are anywhere near us. This group of stars we call the Milky Way Galaxy. In Section B we find that by looking out beyond our own galaxy that there are other separate groups of stars, i.e., other galaxies. ...