Modern ideas. A Brief History of Beginnings Non mythological beginnings, that is Non mythological...
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Modern ideas
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A Brief History of Beginnings
Non mythological beginnings, that is Georges Lemaître and his primordial atom
Vatican Astronomer Alexander Friedman: Big Bang
Russian Mathematician He didn’t name the beginning ‘The Big Bang’
It wasn’t remotely big and it didn’t go BANG! A pejorative term given by Sir Frederick Hoyle
Einstein wasn’t comfortable with either theory, although he did verify the correctness of Friedman’s mathematics
N.B. We will have to think in very, v-e-r-y short times scales here!
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The Evidence
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Hubble’s Law Edwin Hubble found
that, the more distant the galaxy, the faster it was receding from us Ho is the slope of this
line Currently is thought to
be ~ 73
Ho is in units of km/sec/Mpc Ultimately units of time Gives us the age of the
Universe! 13.75 +/- 0.12 Gyr
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The Rationale:
According to the Red Shift of distant galaxies, the Universe is expanding
If the Universe is expanding, we can run the clock backwards and find the starting point (whatever that means)
Important! Wrap your minds around this: By the beginning we don’t mean that all the
matter and energy exploded into an existing space.
We mean that all matter, energy, SPACE and TIME all began at this singular point.
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Definitions
Homogeneous The same everywhere
at a certain scale
Isotropic The same in every
direction
12
3rf.co
m
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String-Theory
Stems from the transition from continuum Physics to quantum Physics at the turn of the 20th C
Starting in the ‘80’s the notion arose that strings were a better model for the basic constituents of matter
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Strings were on the Planck length scale 10-35m Since we can’t see detail at that scale,
particles would naturally be the first approximation
First applied to describe strong interaction, but the theory generated gravitons, much to everyone’s surprise
And strings demanded 10 dimensions!
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Feynman diagrams too convoluted to incorporate these extra dimensions
“Branes” are introduced to explain interactions
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Dimensions
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M-Theory
String theory required 9+1 dimensions
However, this produced 5 equally valid variations! Unacceptable!
A lesser known theory, Supergravity, postulated 10+1 dimensions
Merging the two ideas resolved the 5 variations
However, the addition of the 11thdimension caused the strings to weave into Membranes
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Insane in the
(mem)Brane
A theory of the “trigger”
Multidimensional Universe or multiverse
Gravity is the weakest force because it stretches between branes and is diluted
Intersection of branes initiates a BB
So time didn’t have to begin with the BB
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Other Dimensions
Flatland, a Romance in Many Dimensions Edwin Abbott
Abbott, 1885 A square and his
wife in Flatland
An introduction to greater dimensions
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Lisa Randall
Astrophysicist at Harvard
Leading ‘Brane’ proponent
Warped Passages: Unraveling the Universe's Hidden Dimensions
See also David Deutsch, Hugh Everett…
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How the Universe Got Its Spots
Jenna Levin and others propose a more topological description of cosmology than String Theory
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An Aside About Theories…
Theories like Newton’s Law of Gravitation and Einstein’s General Theory of Relativity are testable and have been verified many, many times
Inflation is not yet testable because the energies are too high to be currently reproduced in the laboratory
Furthermore, direct evidence supporting inflation is not visible because it happened long before the Universe was transparent
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Why Bother with Inflation?
It accounts for certain observed phenomena: Flatness Horizons No monopoles
Not a “deus ex machina” The Universe is currently inflating, after
all
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Stelliferous Era From about 380,000 years A.B.B (after the Big
Bang) until now Galaxies at about 1 billion A.B.B
Average temp = 3K The era of stars, galaxies, and us
What we’ve talked about most of the semester! Top down vs. bottom up
Did massive clouds of gas form first, generating the stars (top down) or did stars form first, collecting into galaxies (bottom up)?
Probably a combination Where gas was dense enough, stars formed first Where gas was rarefied, dark galaxies formed, later
yielding stars Era will continue until the year 100 trillion A.B.BYoungest object ever imaged @
800MYr A.B.B
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The First Stars
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The Universe at 2 Gyr Old
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Hubble Ultra Deep Field
1 million second exposure
Red shifts allow for dating and therefore 3D imaging
Looking back to 700 million years A.B.B.
The last image shows a red galaxy, the earliest object ever imaged
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Then, 40 Years Ago
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Current Mix of Cosmological Stuff
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Vacuum and/or Dark Energy
Very low energy density If the whole Earth volume were V.E. it would be about 1
day’s worth of electricity for 1 person The Quintessence (f) is B-A-C-K!
If true, then constants evolve
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And here we are today…
What will happen in the distant future?
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Fate
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Entropy vs Gravity (curvature)
Entropy: a thermodynamic law dictating the inevitable march to disorder Simple disorder, like breaking glass Thermodynamics disorder:
concentrations of energy, as in a star The ‘arrow’ of time
Gravity (curvature) pulls together (order), entropy corrupts (disorder) over time
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Expansion
The Universe continues to expand
Expansion occurs partially due to L, the cosmological constant
Where matter is closely spaced, gravity (curvature) overwhelms L
Elsewhere L wins And ultimately L will
win!
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The Future:
The most likely* outcome will be the open Universe AKA The Big R.I.P.
The actual density of the Universe is less than the critical density
The Universe will expand forever Three Foreseeable Epochs (after the
Stelliferous Era): The Time of Degeneracy The Time of Black Holes The Time of Photons
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But first… A way to get a handle on these massive time
scales Remember from our first lectures, the idea of
powers of 10? 101 = 10 102 = 100 103 = 1000, etc
Let’s define a cosmic decade, 10t years 101 years is the first cosmic decade, 102 is the second,
and so on The decade is ‘t’ Like stairs where every next step is 10X the height of
the last We are in the 10th cosmic decade The Stelliferous Era will last to the 14th cosmic
decade
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The Time of Degeneracy
Not about deplorable behavior: how matter behaves
From cosmic decade 14 to 37 How do we know?
From the mean half-life of a proton, 1037 years Once in a while, two White Dwarfs may
collide and produce a supernova If not, all WDs will shine away all their
energy The End of Structure
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The Time of Black Holes
Cosmic Decade 37 to 100 How do we know?
Steven Hawking determine the rate of black hole evaporation, now know as Hawking radiation
Particle pair production near the event horizon
Due to the stretching of space-time One particle falls in, the other escapes Radiation follows blackbody curve
‘Cooling’ time can be calculated
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The Time of Photons
Cosmic Decade 100 until ??? Very long wavelength photons Cold, dark Entropy wins Or does it?
Very difficult to make predictions 10100 years in the future
Could be that new complexity begins From other ‘branes’ Via processes we can’t imagine
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THANK YOU FOR YOUR INDULGENCE!
But this will all happen after the final exam