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Cornell - AS 535
  • 20 Pages homework2
    Homework2

    School: Arizona

    %!PS-Adobe-2.0 %Creator: dvips(k) 5.86 Copyright 1999 Radical Eye Software %Title: homework.dvi %Pages: 3 %PageOrder: Ascend %BoundingBox: 0 0 596 842 %EndComments %DVIPSWebPage: (www.radicaleye.com) %DVIPSCommandLine: dvips homework -o homework.ps %

  • 31 Pages chiliplanets
    Chiliplanets

    School: Arizona

    KI Na-D Burgasser et al. 2001 M Dwarfs L Dwarfs T Dwarfs Jupiter Spitzer/IRAC Photometry of T Dwarfs OGLE-TR-56b Burrows et al. 2004 The Evolution and Measurement of EGPs: Remote Sensing of Extrasolar Planets (T. Guillot) (T. Guillot) Is

  • 3 Pages lecture17
    Lecture17

    School: Arizona

    Gamma Ray Bursts Shamelessly stolen from Chris Fryers summer school lectures GRBs The Historical Perspective 1967: Discovery Vela Satellites 1972-1991: Golden Age for Theorists - no constraints and a world of proposals 1991: Constraining the th

  • 3 Pages lecture14
    Lecture14

    School: Arizona

    Prelim Review <1.2 M 9 8 7 6 5 10 4 3 2 1 <1.2 M 1. Hayashi track - fully convective cooler surface temp. requires supersonic convection. Ends with burning of 2H 10 5 43 9 8 7 6 1 2 2. Star becomes radiative from core outward, becoming mor

  • 31 Pages lecture1
    Lecture1

    School: Arizona

    Astronomy 535 Stellar Structure Evolution Course Philosophy Crush them, crush them all! -Professor John Feldmeier Course Philosophy Contextual stellar evolution What we see stars doing The stellar structure that makes stars look that way The phy

  • 17 Pages lecture14
    Lecture14

    School: Arizona

    Prelim Review <1.2 M 9 8 7 6 5 10 43 2 1 <1.2 M 1. Hayashi track - fully convective cooler surface temp. requires supersonic convection. Ends with burning of 2H 10 5 43 9 8 7 6 1 2 Star becomes radiative from core outward, becoming more c

  • 7 Pages lecture9
    Lecture9

    School: Arizona

    H Exhaustion After core H exhaustion core must contract and heat before He burning can begin Shell around contracting core heated to H burning T H Exhaustion Convective core - H depleted out to r = rconvective core T much lower where H still present

  • 12 Pages lecture8
    Lecture8

    School: Arizona

    Population III Common name for the first generation of stars Implies zero metallicity, where zero is the big bang abundance of elements 12C of ~10-12 May include extremely massive objects > 150 M Low z physics issues must be handled carefully Conse

  • 23 Pages lecture3
    Lecture3

    School: Arizona

    Energy Transport in Stars Energy produced in or near centers of stars How fast energy gets out of the star determines radius luminosity effective temperature temperature structure large scale internal fluid motions Energy can be carried by radiative

  • 15 Pages lecture2
    Lecture2

    School: Arizona

    Hydrodynamics Notation: Lagrangian derivative d = +v dt t Continuity equation dr H =r v dt r + (r v ) = 0 t Mass conservation: Time rate of change of mass density must balance mass flux into/out of a volume, hence the divergence of v in the Euleri

  • 15 Pages lecture16
    Lecture16

    School: Arizona

    Supernovae continued -rich Freezeout Freezeout - nuclear reactions halted before coming to equilibrium or steady state configuration by temperature & density evolution -rich freezeout occurs in material shocked to NSE temperatures. Expansion cause

  • 26 Pages lecture11
    Lecture11

    School: Arizona

    Nuclear Reactions Nuclear Reactions Binding Energies The mass law below represents the masses of thousands of nuclei with a few parameters B=(Z(mp+me)+(A-Z)mn - M(A,Z)c2 Mass Excess M= 9.31.478MeV (M(A,Z)-A) ; M in AMU Q value - energy released

  • 15 Pages lecture12
    Lecture12

    School: Arizona

    Evolved Massive Stars Wolf-Rayet Stars Classification WNL - weak H, strong He, NIII,IV WN2-9 - He, N III,IV,V earliest types have highest excitation WC4-9 - He, C II,III,IV, O III,IV,V WO1-4 - C III,IV O IV,V,VI WN most common, WO least Wolf-

  • 20 Pages lecture10
    Lecture10

    School: Arizona

    The Red Giant Branch The Red Giant Branch Lshell drives expansion Lshell driven by Mcore - as |, |T| increase outside contracting core shell narrows, also Lcore from contraction increases Tshell Lshell large, rshell small so convection necessary

  • 26 Pages lecture11
    Lecture11

    School: Arizona

    Nuclear Reactions Nuclear Reactions Binding Energies The mass law below represents the masses of thousands of nuclei with a few parameters B=(Z(mp+me)+(A-Z)mn - M(A,Z)c2 Mass Excess M= 9.31.478MeV (M(A,Z)-A) ; M in AMU Q value - energy released

  • 25 Pages lecture13
    Lecture13

    School: Arizona

    Late Burning Stages Late Burning Stages fuel 1H 4He 12C 20Ne 16O 28Si 56Ni q(erg g-1) 5-8e18 7e17 5e17 1.1e17 5e17 0-3e17 -8e18 T/109 0.01 0.2 0.8 1.5 2 3.5 6-10 Late Burning Stages fuel 1H 4He 12C 20Ne 16O 28Si 56Ni q(erg g-1) 5-8e18 7e17 5e17 1.1

  • 23 Pages lecture15
    Lecture15

    School: Arizona

    Core Collapse Supernovae Core Collapse 0. cooling gives a small core & large mantle calculations without it have overly large Fe cores. Get a Chandrasekhar mass Fe core 1. Bad: binding energy of Fe peak nuclei very small or negative - no energy gen

  • 3 Pages lecture9
    Lecture9

    School: Arizona

    H Exhaustion After core H exhaustion core must contract and heat before He burning can begin Shell around contracting core heated to H burning T H Exhaustion Convective core - H depleted out to r = rconvective core T much lower where H still present

  • 34 Pages lecture7
    Lecture7

    School: Arizona

    The Main Sequence Projects Evolve from initial model to establishment of H burning shell after core H exhaustion At minimum do z=0, z=0.1solar, z=solar, z=2solar for z=2solar use hetoz = 2.0 and 3.0 (see genex) Note features in the HR diagram a

  • 3 Pages 535.syllabus
    535.syllabus

    School: Arizona

    DRAFT ASTR 535 Stellar Evolution http:/chandra.as.arizona.edu/~dave/535/ David Arnett darnett@as.arizona.edu Office 330 Jim Liebert jliebert@as.arizona.edu Office 336 Patrick Young payoung@as.arizona.edu Office T102 (in the trailer) Homework: There w

  • 3 Pages lecture2
    Lecture2

    School: Arizona

    Hydrodynamics Notation: Lagrangian derivative d" = +v#$ dt "t Continuity equation d" ! = "# $ v dt &" % + # $ ( "v ) = 0 &t Mass conservation: Time rate of change of mass density must balance mass flux into/out of a volume, hence the divergence of

  • 15 Pages lecture12
    Lecture12

    School: Arizona

    Evolved Massive Stars Wolf-Rayet Stars Classification WNL - weak H, strong He, NIII,IV WN2-9 - He, N III,IV,V earliest types have highest excitation WC4-9 - He, C II,III,IV, O III,IV,V WO1-4 - C III,IV O IV,V,VI WN most common, WO least Wolf

  • 3 Pages lecture8
    Lecture8

    School: Arizona

    Population III Common name for the first generation of stars Implies zero metallicity, where zero is the big bang abundance of elements 12C of ~10-12 May include extremely massive objects > 150 M Low z physics issues must be handled carefully Conse

  • 3 Pages lecture3
    Lecture3

    School: Arizona

    Energy Transport in Stars Energy produced in or near centers of stars How fast energy gets out of the star determines radius luminosity effective temperature temperature structure large scale internal fluid motions Energy can be carried by radiative

  • 3 Pages lecture16
    Lecture16

    School: Arizona

    Supernovae continued -rich Freezeout Freezeout - nuclear reactions halted before coming to equilibrium or steady state configuration by temperature & density evolution -rich freezeout occurs in material shocked to NSE temperatures. Expansion causes

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