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Why are we here?. Dr Martin Hendry University of Glasgow. Why are we here?…. The period of inflation in the very early Universe was invoked to explain some apparent ‘fine tuning’ problems. If the Universe is now inflating, this presents a new set of ‘fine tuning’ problems. Atoms. - PowerPoint PPT Presentation
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Dr Martin HendryUniversity of Glasgow
Why are we here?….
The period of inflation in the very early Universe was invoked to explain some apparent ‘fine tuning’ problems.
If the Universe is now inflating, this presents a new set of ‘fine tuning’ problems
Dark Energy
Cold Dark Matter
Ato
ms
State of the Universe – Nov 2003
Dark Energy
Cold Dark Matter
Ato
ms
State of the Universe – Nov 2003
Why does 96% of the Universe consist of ‘strange’ matter and energy?
CDM
From Lineweaver (1998)
General Relativity:-
Geometry matter / energy
“Spacetime tells matter how to move and matter tells spacetime how to curve”
Einstein’s Field Equations
TGRgRG 82
1
Einstein tensor Ricci tensor Metric tensorCurvature scalar Energy-momentum tensor
of gravitating mass-energy
General Relativity:-
Geometry matter / energy
“Spacetime tells matter how to move and matter tells spacetime how to curve”
Einstein’s Field Equations
Treating the Universe as a perfect fluid, can solve equations to determine the pressure and density, and how they evolve
Einstein originally sought static solution but this isn’t possible, for ‘normal’ pressure and density
He added a ‘cosmological constant’ to the field equations
Can tune to give static Universe, but unstable
(and Hubble expansion made idea redundant anyway!)
Einstein’s greatest blunder?
But what is ?…
Particle physics motivates as energy density of the vacuum but scaling arguments suggest:-
So historically it was easier to believe
12010theory)(
obs)(
0
Re-expressing Friedmann’s Equations
At any time
1 km
Dimensionless matter density
Dimensionless vacuum energy density
Dimensionless curvature density
Re-expressing Friedmann’s Equations
At any time
If the Universe is flat then
1 km
Dimensionless matter density
Dimensionless vacuum energy density
Dimensionless curvature density
0k
Dark Energy
Cold Dark Matter
Ato
ms
State of the Universe – Nov 2003
State of the Universe – Nov 2003
m
CDM
From Lineweaver (1998)
m
Value of
Present-day 0/ RR
If the Concordance Model is right, we live at a special epoch. Why?…
Hydrogen fusion – fuelling a star’s nuclear furnace
E = mc 2
P-P chain, converting hydrogen to helium
This has led to more general Dark Energy or Quintessence models:
Evolving scalar field which ‘tracks’ the matter density
Convenient parametrisation: ‘Equation of State’
Can we measure w(z) ?
wP Matter 0Radiation 1/3Curvature -1/3‘Lambda’ -1Quintessence w(z)
iw
Pressure
Density
SNIa at z = 0.5
Adapted from Schmidt (2002)
mq2
10
At low redshift, SN1a essentially measure the deceleration parameter
SNIa at z = 1.0
Adapted from Schmidt (2002)
At low redshift, SN1a essentially measure the deceleration parameter
mq2
10
SNIa at 0.5<z<1.0
Adapted from Schmidt (2002)
At low redshift, SN1a essentially measure the deceleration parameter
mq2
10
Tegmark et al (1998)
SNIa measure:-
CMBR measures:-
Together, can constrain:-
mq2
10
mk 1
,m
Can we distinguish a constant term from quintessence?…
Not from current ground-based SN observations (combined with e.g. LSS)
Adapted from Schmidt (2002)
Can we distinguish a constant term from quintessence?…
Not from current ground-based SN observations (combined with e.g. LSS)…
…or from future ground-based observations (even with LSS + CMBR)
Adapted from Schmidt (2002)
Can we distinguish a constant term from quintessence?…
Not from current ground-based SN observations (combined with e.g. LSS)…
…or from future ground-based observations (even with LSS + CMBR)
Adapted from Schmidt (2002)
Can we distinguish a constant term from quintessence?…
Not from current ground-based SN observations (combined with e.g. LSS)…
…or from future ground-based observations (even with LSS + CMBR)
Main goal of the SNAP satellite(launch ~2010?)
Adapted from Schmidt (2002)