the consequences of a dynamical dark energy density on the evolution of the universe
DESCRIPTION
The Consequences of a Dynamical Dark Energy Density on the Evolution of the Universe. By Christopher Limbach, Alexander Luce, and Amanda Stiteler. Background image: Andrey Kravtsov., University of Chicago, 2003. Presentation Overview. Image by Martin Altmann, Observatory Hoher List, 1997. - PowerPoint PPT PresentationTRANSCRIPT
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The Consequences of a The Consequences of a Dynamical Dark Energy Dynamical Dark Energy
Density on the Evolution of Density on the Evolution of the Universethe Universe
By Christopher Limbach, By Christopher Limbach, Alexander Luce, and Amanda Alexander Luce, and Amanda
StitelerStitelerBackground image: Andrey Kravtsov., University of Chicago, 2003.
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Presentation Overview• Amanda Stiteler
– Introduction– Theory
• Chris Limbach– Assumptions– Verification of Methods
• Alex Luce– Results– Conclusion
Image by Martin Altmann, Observatory Hoher List, 1997.
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The Big Bang in BriefThe Big Bang in Brief
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Einstein’s Cosmological ModelEinstein’s Cosmological Model
Rij = Ricci tensorR = curvature scalargij = space-time metric tensorG = Newton’s gravitational constantTij = stress-energy tensorΛ = cosmological constant
ijijijij GTgRgR 821
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The Friedmann EquationThe Friedmann Equation
a = dimensionless scale factorρR = relativistic matter densityρM = non-relativistic matter densityρΛ = dark energy densityk = curvature of the universec = speed of lightl0 = present distance between two galaxies
220
22
381
alkcG
dtda
a MR
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QuintessenceQuintessence• Equation relating the scalar field, , and its
potential, :
• Energy density of the scalar field:
• Evolution of the scalar field:
22
2
32 pp m
m
02
3 )1(2 pmaa
V
V
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Free Parameters Free Parameters andand
• Parameters which characterize potential
• Chosen such that V(φ) mimics nearly constant Λ at present
V
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Purpose of this ProjectPurpose of this Project
• Compare the evolution of a universe Compare the evolution of a universe with constant dark energy density to with constant dark energy density to one with variable dark energy densityone with variable dark energy density
• Determine restrictions of the Determine restrictions of the constants constants κκ and and αα
Image by NASA., 2006.
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AssumptionsAssumptions• Homogeneous, Isotropic Universe• (from WMAP)
• Total Density = Critical Density
• Initial Conditions for ΩR, ΩM, ΩΛ from WMAP
• No Spatial Curvature
MpckmH 1sec
680
critMR
critcrit
MM
crit
RR
,,
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MethodMethod• 4th Order Runge-Kutta• Equations Solved:
RMadtda
38
dtd
aa
dtd 3
2)1(
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Numeric SolutionsNumeric Solutions
Time Relative to Present [Gyrs]
Scale Factor
a
1
0
0.01
“Time of Big Bang”
t
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Verification Verification
h= 0.02
h = 0.01
h = 0.005
Time From Present [Gyrs]
Scale Factor
1
Solution error δh
t
a
h= time step
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Simulation ResultsSimulation Results
Constant Dark Energy vs. Time Dependent Dark Energy?
Restrictions on Free Parameters of Model
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Dark Energy: Dark Energy: ConstantConstant
• Radiation Plays Large role at early times
• Matter Increases as radiation dies off
• Dominated by Dark Energy at later times
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Dark Energy: Dark Energy: Time DependentTime Dependent
• Dominated by Dark Energy at early times
• Again dominated by Dark Energy at later times
• Kappa and Alpha were chosen to agree w/ observations
• Amount of radiation is relatively lower
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Dark Energy: Constant vs. Time Dependent
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Free Parameters Constrained Free Parameters Constrained by Age of Universeby Age of Universe
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Scale FactorScale Factor• Represents
relative expansion of universe
• Independent of Free Parameters which characterize expansion
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Power Law Model of Time Power Law Model of Time Dependent dark energy: Dependent dark energy:
PossiblePossible• Free Parameters do
not influence Dynamical behaviour
• WMAP findings: Universe is >13.7 billion years old
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AcknowledgmentsAcknowledgments
• Dimitrios Psaltis• Chi Kwan Chan• Drew Milsom
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Sources CitedSources CitedKravtsov, Andrey. “Computer-generated image of the distribution of dark matter.” Image
from “Cosmologists to plot strategy for dark energy research campaign at Chicago workshop Sept. 17-20.” 3 Sept 2003. 29 April 2007. <http://www-news.uchicago.edu/ releases/03/030903.darkmatter.shtml>.
Limbach, Christopher, Alexander Luce, and Amanda Stiteler. “The Consequences of a Dynamical Dark Energy Density on the Evolution of the Universe.” 5 Dec 2006. 29 April 2007. <http://www.physics.arizona.edu/~dpsaltis/Phys205/limbach_luce_stiteler.pdf >.
NASA. “WMAP picture of the infant universe.” Image from “Ringside Seat to the Universe’s First Split Second.” 20 March 2006. 30 April 2007. <http://imagine.gsfc.nasa.gov/docs/ features/news/20mar06.html>.
National Taiwan Science Education Center. “The origin and the evolution of the Universe.” Image from “The Emergence of the Cosmos.” 29 April 2007. <http://www.ntsec.gov.tw/ space/EN/show.asp?XH36>.
WMAP. “Geometry of the Universe.” “Image from “Sachs-Wolfe Effect.” 2 May 2007. <http://zebu.uoregon.edu/2004/a321/lec15.html>.
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Free Parameters Constrained by Free Parameters Constrained by Age of UniverseAge of Universe
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Energy DensityEnergy Density