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Exergy_analysis_CO2
Course: CH 242a, Fall 2010School: Caltech
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Caltech - CH - 242a
Fuel productivity for closed system70071072073074075076077078079080081082083084085086087088089090091092093094095096097098099010001010102010301040105010601070108010901100111011201130114011501160117011801190
Caltech - CH - 242a
alculation of fuel productivity for closed systemVariation of temperature157316731773187319732073TLTHVariation of nAr157316731773187319732073THnAr0.00380.00558.60E-030.01630.02910.04370.00350.00538.40E-030.01610.02890.04350.
Caltech - CH - 242a
Fuel productivity for closed system70071072073074075076077078079080081082083084085086087088089090091092093094095096097098099010001010102010301040105010601070108010901100111011201130114011501160117011801190
Caltech - CH - 242a
Fuel productivity for fixed pO2-values70071072073074075076077078079080081082083084085086087088089090091092093094095096097098099010001010102010301040105010601070108010901100111011201130114011501160117011801
Caltech - CH - 242a
0.00070.00060.00150.00210.00270.00370.0050.00760.01840.06210.12030.15980.19260.224811730.00150.00210.00270.00360.0050.00730.01510.04040.08540.13210.16950.20330.23920.302112730.00040.00060.00120.00170.00230.0030.0040.00
Caltech - CH - 242a
Efficiency as a function of operating temperatures0.140.120.10.080.060.04Fuel production as a function of operating temperatures0.02020000.14160014001900120018000.12100017000.1TH0.088001600600TL0.060.040.020 Fuel production
Caltech - CH - 242a
Second Law AnalysisA second law analysis of the two-stepthermo-chemical process to split water andCO2 is performed to assess its ability toconvert solar energy into chemical energyin the form of gaseous hydrogen orcarbonmonoxide.boththetherFig.
Caltech - CH - 242a
Exergy Analysis for CO2CTHTL[H2O]ipO2QsolarQreradiationQreactor,netIrrdissociationQcoolingIrrcoolingQCO2-reducerIrrCO2-reducerQFCWFCexergyabsorption30001873.15 K673.15 K0.0172 molceria/s0.1609 molH2O/molceria1.013*10-5 bar3000 W69
Caltech - CH - 242a
CTHTL[H2O]ipO2QsolarQreradiationQreactor,netIrrdissociationQcoolingIrrcoolingQhydrolysisIrrhydrolysisQFCWFCabsorptionexergy30001873,15 K673,15 K0,0164 mol/s0,1606 molH2O/molceria1,013*10-5 bar3000 W698,09 W2301,9 W2,11 W/K1959,8
Caltech - CH - 242a
Exergy Analysis for H2OCTHTL[H2O]ipO2QsolarQreradiationQreactor,netIrrdissociationQcoolingIrrcoolingQhydrolysisIrrhydrolysisQFCWFCabsorptionexergy30001873,15 K673,15 K0,0164 mol/s0,1606 molH2O/molceria1,013*10-5 bar3000 W698,09 W
Caltech - CH - 242a
Efficiency open systemVariation of temperatureTL600610620630640650660670680690700710720730740750760770780790800810820830840850860870880890900910920930940950960970980990100010101020103010401050106010701080
Caltech - GEL - 132
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Caltech - GEL - 133
Characteristics of planetary candidates observed by Kepler, II: Analysisof the first four months of dataWilliam J. Borucki0,1, David G. Koch1, Gibor Basri2, Natalie Batalha3, Timothy M. Brown5,Stephen T. Bryson1, Douglas Caldwell6, Jrgen Christensen-Da
Caltech - GEL - 133
Etc. etc. etc.NPlutinos3:22:1Nrosne ceptusingscattered KBOsclassical KBOsNSJUNPPlutoUranusNeptuneSaturnJupiterAsteroid beltMarsEarthVenusMercuryPlutoEarthSaturnJupiterAsteroid beltVenusMercuryMarsUranusNeptune?Kuiper
Caltech - GEL - 133
Ge 133 Planetary Formation & EvolutionFinal ExaminationOut: 02 December 2011Due: 09 December 20111 pmThis exam has a 4-hour limit and must be completed within a single block of time.It is totally closed book, notes, friends, neighbors, internet, dog
Caltech - GEL - 133
1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T
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The Demographics of Extrasolar Planets Beyond theSnow Line with Ground-based Microlensing SurveysarXiv:0903.0880v1 [astro-ph.EP] 4 Mar 2009White Paper for the Astro2010 PSF Science Frontier PanelB. Scott GaudiThe Ohio State Universitygaudi@astronomy
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LETTERdoi:10.1038/nature10201A low mass for Mars from Jupiters earlygas-driven migrationKevin J. Walsh1,2, Alessandro Morbidelli1, Sean N. Raymond3,4, David P. OBrien5 & Avi M. Mandell6we present a simple scenario that reflects one plausible history
Caltech - GEL - 133
c ESO 2011Astronomy & Astrophysics manuscript no. HARPSstatSeptember 13, 2011The HARPS search for southern extra-solar planetsXXXIV. Occurrence, mass distribution and orbital properties of super-Earths andNeptune-mass planetsM. Mayor1 , M. Marmier1
Caltech - GEL - 133
Draft version August 20, 2009APreprint typeset using L TEX style emulateapj v. 10/09/06INTERNATIONAL YEAR OF ASTRONOMY INVITED REVIEW ON EXOPLANETSJohn Asher Johnson1arXiv:0903.3059v1 [astro-ph.EP] 17 Mar 2009Draft version August 20, 2009ABSTRACTJ
Caltech - GEL - 133
Lecture 1 What can the solar system tell us about theformation & evolution of planetary systems?Lets consider:1. The sun.2. The major planets.3. Small bodies, including the Kuiper Beltand laboratory samples.What is the composition of the sun? Are o
Caltech - GEL - 133
Lecture 1 What can the solar system tell us about theformation & evolution of planetary systems?Lets consider:1. The sun.2. The major planets.3. Small bodies, including the Kuiper Beltand laboratory samples.What is the composition of the sun? Are o
Caltech - GEL - 133
Extrasolar planet detection:Methods and limitsGe/Ay133How do you find a planet? Look for it? Hard (as well see)!Only planet imagedis very young andfar from its star.Are such objectscommon or rare?Duquennoy & Mayor (1991) - BinariesWhere should
Caltech - GEL - 133
Extrasolar planet detection:Methods and limitsGe/Ay133How do you find a planet? Look for it? Hard (as well see)!Only planets imagedare very young andfar from their stars.Are such objectscommon or rare?Duquennoy & Mayor (1991) - BinariesWhere sh
Caltech - GEL - 133
Extrasolar planet detection:Methods and limitsGe/Ay133How do you find a planet? Look for it? Hard (as well see)!Only planets imagedare very young andfar from their stars.Are such objectscommon or rare?Duquennoy & Mayor (1991) - BinariesWhere sh
Caltech - GEL - 133
What have radial velocity surveys toldus about (exo)-planetary science?Ge/Ay133Discovery space forindirect methods:Radial velocityAstrometry(r=distance to the star)Mayor, M. & Queloz, D. 1995, Nature, 378, 355Udry, S. et al. 2002, A&A, 390, 26Jo
Caltech - GEL - 133
Extrasolar planet detection: Methods and limitsGe/Ay133Spectral Energy Distributions(or, Blinded by the light!.)How do you find a planet? Look for it? Hard (as weve seen)!Only planets imaged are very young and far from their stars. Are such objects
Caltech - GEL - 133
What have radial velocity surveys toldus about (exo)-planetary science?Ge/Ay133Discovery space forindirect methods:Radial velocityAstrometry(r=distance to the star)Mayor, M. & Queloz, D. 1995, Nature, 378, 355Udry, S. et al. 2002, A&A, 390, 26Jo
Caltech - GEL - 133
What have radial velocity surveys told us about (exo)-planetary science?Ge/Ay133Discovery space for indirect methods:Radial velocityAstrometry(r=distance to the star)Mayor, M. & Queloz, D. 1995, Nature, 378, 355Udry, S. et al. 2002, A&A, 390, 26Jo
Caltech - GEL - 133
What can transit observations tell us about (exo)-planetary science?Ge/Ay133Sometimes the absence of signal is interesting:Gilliland, R.L. et al. 2000, ApJ, 545, L47No transits in 47 Tuc, `expectation'=30-40 (34,000 stars)Transits, approach #1:Sato,
Caltech - GEL - 133
What (exo)-planetary science can bedone with microlensing?Ge/Ay133Other routes to Earth-like planets? = 4GM/bc2bMicrolensing example:Microlensing example:Best geometry uses stars at a few kpc (the lens)against the Galactic Bulge (light source).5
Caltech - GEL - 133
What (exo)-planetary science can bedone with microlensing?Ge/Ay133Other routes to Earth-like planets? = 4GM/bc2bMicrolensing example:Microlensing example:Best geometry uses stars at a few kpc (the lens)against the Galactic Bulge (light source).5
Caltech - GEL - 133
SED studies of disk lifetimes &Long wavelength studies of disksGe/Ay133Characterizinglargedisksamples?SEDModels:HH30G.J. vanZadelhoff2002Chiang &Goldreich1997IRdisk surface within several 0.1 several tens of AU(sub)mmdisk surface at large ra
Caltech - GEL - 133
SED studies of disk lifetimes &Long wavelength studies of disksGe/Ay133Characterizinglargedisksamples?SEDModels:HH30G.J. vanZadelhoff2002Chiang &Goldreich1997IRdisk surface within several 0.1 several tens of AU(sub)mmdisk surface at large ra
Caltech - GEL - 133
SED studies of disk lifetimes & Long wavelength studies of disksGe/Ay133Characterizinglargedisksamples?SEDModels:HH30G.J. van Zadelhoff 2002Chiang & Goldreich 1997IR disk surface within several 0.1 several tens of AU (sub)mm disk surface at large ra
Caltech - GEL - 133
Disk Structure and Evolution(the so-called model of disk viscosity)Ge/Ay 133Recapitulationofpassivediskstructureequations.I.Equation for hydrostatic equilibrium using only stellar gravity.For an ideal gaswhere c is the sound speed (c2 = RT).Solving
Caltech - GEL - 133
Disk Structure and Evolution(the so-called model of disk viscosity)Ge/Ay 133Recapitulationofpassivediskstructureequations.I.Equation for hydrostatic equilibrium using only stellar gravity.For an ideal gaswhere c is the sound speed (c2 = RT).Solving
Caltech - GEL - 133
How do small dust grains growin protoplanetary disks?Ge/Ay133Howdowegofromawellmixedgas/dustgraindisk:Toamatureplanetarysystem?Forsolids,itishelpfultodistinguishamongstseveralregimes:mcmkmmoon/Mars(oligarchs)110MEarthStep#1:Growthfrom~0.1mto~1cmsca
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How do small dust grains grow in protoplanetary disks?Ge/Ay133Howdowegofromawellmixedgas/dustgraindisk:Toamatureplanetarysystem?Forsolids,itishelpfultodistinguishamongstseveralregimes: mcmkmmoon/Mars(oligarchs)110MEarthStep#1:Growthfrom~0.1 mto~1cmsc
Caltech - GEL - 133
How do small dust grains growin protoplanetary disks?Ge/Ay133Howdowegofromawellmixedgas/dustgraindisk:Toamatureplanetarysystem?Forsolids,itishelpfultodistinguishamongstseveralregimes:mcmkmmoon/Mars(oligarchs)110MEarthStep#1:Growthfrom~0.1mto~1cmsca
Caltech - GEL - 133
How do planetesimals grow toform ~terrestrial mass cores?Ge/Ay133Fornow,letsignorethegas.Thismeanswecanjustworryaboutgravity.Forthepairwiseinteractionoftwobodies,wehave:r=a1br=a2Forcollisionsthataregrazing,thevelocityatimpactcanbeshowntobePluggi
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How do planetesimals grow to form ~terrestrial mass cores?Ge/Ay133Fornow,letsignorethegas.Thismeanswecanjustworryaboutgravity.Forthe pairwiseinteractionoftwobodies,wehave: r=a1 br=a2 Forcollisionsthataregrazing,the velocityatimpactcanbeshowntobe Pluggi
Caltech - GEL - 133
How do planetesimals grow toform ~terrestrial mass cores?Ge/Ay133Fornow,letsignorethegas.Thismeanswecanjustworryaboutgravity.Forthepairwiseinteractionoftwobodies,wehave:r=a1br=a2Forcollisionsthataregrazing,thevelocityatimpactcanbeshowntobePluggi
Caltech - GEL - 133
Jovian planet formation. Core-accretion or gravitational instability?Ge/Ay133PropertiesoftheJovianPlanetsintheSolarSystemP 2 forH2HeI/MR2=0.4forauniformsphere I/MR2=0.26forP 2Theradiusmass relationshipandM.o.I. areusedtoinferthe presenceofprimordial
Caltech - GEL - 133
Jovian planet formation. Core-accretionor gravitational instability?Ge/Ay133PropertiesoftheJovianPlanetsintheSolarSystemP2forH2HeI/MR2=0.4forauniformsphereI/MR2=0.26forP2TheradiusmassrelationshipandM.o.I.areusedtoinferthepresenceofprimordialco
Caltech - GEL - 133
Jovian planet formation. Core-accretionor gravitational instability?Ge/Ay133PropertiesoftheJovianPlanetsintheSolarSystemP2forH2HeI/MR2=0.4forauniformsphereI/MR2=0.26forP2TheradiusmassrelationshipandM.o.I.areusedtoinferthepresenceofprimordialco
Caltech - GEL - 133
What effects do 1-10 MEarth cores & Jovian planets have on the surrounding disk? Or, Migration & GapsGe/Ay133Disks can be unstable globally:Toomres criterion Q c/( G) < 1 ( axisymmetric perturbations) = epicyclic frequencyDisks can be unstable globall
Caltech - GEL - 133
What effects do 1-10 MEarth coreshave on the surrounding disk?Today = GapsWednesday = Migration (included here)Ge/Ay133Disks can be unstable globally:Toomres criterionQ c/(G) < 1( axisymmetric perturbations) = epicyclic frequencyDisks can be uns
Caltech - GEL - 133
What effects do 1-10 MEarth coreshave on the surrounding disk?Today = GapsWednesday = Migration (included here)Ge/Ay133Disks can be unstable globally:Toomres criterionQ c/(G) < 1( axisymmetric perturbations) = epicyclic frequencyDisks can be uns
Caltech - GEL - 133
What can the Kuiper belt tell usabout the early solar system?Part I (Part II next lecture)Ge/Ay133Kuipers Hypothesis (1950) Pluto should not be alone!1999 KR 16First (non-Pluto)trans-Neptunianobject found in1992 (Jewitt &Luu), now manymany hund
Caltech - GEL - 133
Can we study extrasolar Kuiper Belts? Pic, A5V starGe/Ay133AU Mic, M1Ve starImpossible to see any exo-KBOs themselves, butHow do we find debris disks?Spitzer Data (FEPS team)Model has 0.1 Mmoon of30 m size dust grainsin a disk from 3060 AUBars a
Caltech - GEL - 133
Can we study extrasolar Kuiper Belts? Pic, A5V starGe/Ay133AU Mic, M1Ve starImpossible to see any exo-KBOs themselves, butHow do we find debris disks?Spitzer Data (FEPS team)Model has 0.1 Mmoon of30 m size dust grainsin a disk from 3060 AUBars a
Caltech - GEL - 133
Can we study extrasolar Kuiper/Asteroid Belts? Pic, A5V starAU Mic, M1Ve starGe/Ay133Impossible to see any exo-KBOs themselves, butNear Earth dust source?How do we find debris disks?Spitzer Data (FEPS team) Model has 0.1 Mmoon of 30 m size dust gra
Caltech - GEL - 133
What can the asteroid belt tell us about the early S.S.?433 Eros? PhobosGe/Ay133These types are not strongly separated, radially.Comets are icy bodies that sublimate and becomeactive when close to the Sun. They are believed tooriginate in two cold
Caltech - GEL - 133
In what sort of region did our own solar system form?Ge/Ay133Inrelativeisolation(Taurus,Bokglobules,)?In what sort of environment did our own solar system form?Oraspartofarichcluster(morelikely)?Oneimportantsetofclues: Shortlivednuclidesinmeteorites
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When and how did the cores of terrestrial planets form?Ge/Ay133Two end member hypotheses for core formation:Estimated core sizesof the terrestrial planets.Two end member hypotheses for core formation:Q: Why is heterogeneousaccretion unlikely?A: In
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When and how did the cores of terrestrial planets form?Ge/Ay133Two end member hypotheses for core formation:Estimated core sizesof the terrestrial planets.Two end member hypotheses for core formation:Q: Why is heterogeneousaccretion unlikely?A: In
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Planetary DynamicsGe/Ay133Orbital elements (3-D),& time evolution:What ARE Lyapounov exponents and times?Regular Chaotic Suppose that twoorbits are separated inphase space by d, andthat d followsd = d0 e- (t-t0)G is the Lyapounovexponent, and
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Planetary DynamicsGe/Ay133Orbital elements (3-D),& time evolution:What ARE Lyapounov exponents and times?Regular Chaotic Suppose that twoorbits are separated inphase space by d, andthat d followsd = d0 e- (t-t0)G is the Lyapounovexponent, and
Caltech - GEL - 133
January 4, 2009APreprint typeset using L TEX style emulateapj v. 03/07/07MODELS OF JUPITERS GROWTH INCORPORATING THERMAL AND HYDRODYNAMIC CONSTRAINTSJack J. Lissauer, Olenka Hubickyj1 , Gennaro DAngelo2NASA Ames Research Center, Space Science and Ast
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Formation of Jupiter and Conditions for Accretion of the GalileanSatellitesarXiv:0809.1418v3 [astro-ph] 16 Jan 2009P. R. Estrada, and I. MosqueiraSETI InstituteJ. J. Lissauer, G. DAngelo, and D. P. CruikshankNASA Ames Research CenterAbstractWe pre