Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

What was before the Big Bang, and howmight we be able to tell?

Cosmology of the Very Early Universe

Robert BrandenbergerMcGill University

Physics Matters Lecture, September 7, 2017

1 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Outline

1 What is Cosmology?

2 FrameworkSpace-TimeStandard Big Bang Cosmology

3 Inflationary Cosmology

4 String Cosmology

5 Conclusions

2 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Plan

1 What is Cosmology?

2 FrameworkSpace-TimeStandard Big Bang Cosmology

3 Inflationary Cosmology

4 String Cosmology

5 Conclusions

3 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Goals of Early Universe Cosmology

1. Understand origin and early evolution of the universe.

What is the “Big Bang"?Was there a “Big Bang"?What was before the “Big Bang"?

2. Explain observed large-scale structure.

4 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Goals of Early Universe Cosmology

1. Understand origin and early evolution of the universe.

What is the “Big Bang"?Was there a “Big Bang"?What was before the “Big Bang"?

2. Explain observed large-scale structure.

4 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Goals of Early Universe Cosmology

1. Understand origin and early evolution of the universe.

What is the “Big Bang"?Was there a “Big Bang"?What was before the “Big Bang"?

2. Explain observed large-scale structure.

4 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Optical Telescopes: Gemini Telescope

5 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Galaxies: Building Blocks of the Cosmology

6 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Large-Scale Structure

From: talk by O. Lahav

7 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Microwave Telescopes on the Earth: ACTTelescope

8 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Microwave Telescopes on the Earth: SPTTelescope

9 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Microwave Telescopes in Space: WMAPTelescope

10 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Isotropic CMB Background

11 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Anisotropies in the Cosmic MicrowaveBackground (CMB)

Credit: NASA/WMAP Science Team12 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Quantification of the CMB data

Credit: NASA/WMAP Science Team

13 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Goals of Early Universe Cosmology

1. Understand origin and early evolution of the universe.

What is the “Big Bang"?Was there a “Big Bang"?What was before the “Big Bang"?

2. Explain observed large-scale structure.

Patterns in the distribution of galaxies on large scales.Anisotropies in CMB maps.

3. Make predictions for future observations.

14 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Goals of Early Universe Cosmology

1. Understand origin and early evolution of the universe.

What is the “Big Bang"?Was there a “Big Bang"?What was before the “Big Bang"?

2. Explain observed large-scale structure.

Patterns in the distribution of galaxies on large scales.Anisotropies in CMB maps.

3. Make predictions for future observations.

14 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Plan

1 What is Cosmology?

2 FrameworkSpace-TimeStandard Big Bang Cosmology

3 Inflationary Cosmology

4 String Cosmology

5 Conclusions

15 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Framework

The Universe is:

Space-timeMatter which lives in space-time.

To describe the Universe:

Space-time described by Einstein’s theory of GeneralRelativity.Matter as described by Physics.More specifically: matter described on large scales byclassical physics, on small scales by quantummechanics and on even smaller scales by superstringtheory ?

16 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Framework

The Universe is:

Space-timeMatter which lives in space-time.

To describe the Universe:

Space-time described by Einstein’s theory of GeneralRelativity.Matter as described by Physics.More specifically: matter described on large scales byclassical physics, on small scales by quantummechanics and on even smaller scales by superstringtheory ?

16 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Framework

The Universe is:

Space-timeMatter which lives in space-time.

To describe the Universe:

Space-time described by Einstein’s theory of GeneralRelativity.Matter as described by Physics.More specifically: matter described on large scales byclassical physics, on small scales by quantummechanics and on even smaller scales by superstringtheory ?

16 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Framework

The Universe is:

Space-timeMatter which lives in space-time.

To describe the Universe:

Space-time described by Einstein’s theory of GeneralRelativity.Matter as described by Physics.More specifically: matter described on large scales byclassical physics, on small scales by quantummechanics and on even smaller scales by superstringtheory ?

16 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Framework

The Universe is:

Space-timeMatter which lives in space-time.

To describe the Universe:

Space-time described by Einstein’s theory of GeneralRelativity.Matter as described by Physics.More specifically: matter described on large scales byclassical physics, on small scales by quantummechanics and on even smaller scales by superstringtheory ?

16 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Framework

The Universe is:

Space-timeMatter which lives in space-time.

To describe the Universe:

Space-time described by Einstein’s theory of GeneralRelativity.Matter as described by Physics.More specifically: matter described on large scales byclassical physics, on small scales by quantummechanics and on even smaller scales by superstringtheory ?

16 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Framework

The Universe is:

Space-timeMatter which lives in space-time.

To describe the Universe:

Space-time described by Einstein’s theory of GeneralRelativity.Matter as described by Physics.More specifically: matter described on large scales byclassical physics, on small scales by quantummechanics and on even smaller scales by superstringtheory ?

16 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Space-Time as Described by General Relativity

Space-time dynamical (no longer absolute like inNewtonian theory)Matter curves space-time.

17 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Space-Time as Described by General Relativity

Space-time dynamical (no longer absolute like inNewtonian theory)Matter curves space-time.

17 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Mass curves Space-Time

18 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Space-Time as Described by General Relativity

Space-time dynamical (no longer absolute like inNewtonian theory)Matter curves space-time: Space-time is dynamical.Note: Newton’s gravitational force is a consequence ofthe curvature of space.Einstein Equivalence Principle determines the motionof matter in curved space-time.Space with a homogeneous distribution of mattercannot be static - it must expand (or contract).

19 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Space-Time as Described by General Relativity

Space-time dynamical (no longer absolute like inNewtonian theory)Matter curves space-time: Space-time is dynamical.Note: Newton’s gravitational force is a consequence ofthe curvature of space.Einstein Equivalence Principle determines the motionof matter in curved space-time.Space with a homogeneous distribution of mattercannot be static - it must expand (or contract).

19 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Space-Time as Described by General Relativity

Space-time dynamical (no longer absolute like inNewtonian theory)Matter curves space-time: Space-time is dynamical.Note: Newton’s gravitational force is a consequence ofthe curvature of space.Einstein Equivalence Principle determines the motionof matter in curved space-time.Space with a homogeneous distribution of mattercannot be static - it must expand (or contract).

19 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Space-Time as Described by General Relativity

Space-time dynamical (no longer absolute like inNewtonian theory)Matter curves space-time: Space-time is dynamical.Note: Newton’s gravitational force is a consequence ofthe curvature of space.Einstein Equivalence Principle determines the motionof matter in curved space-time.Space with a homogeneous distribution of mattercannot be static - it must expand (or contract).

19 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

The Expanding Universe

20 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Evidence for the Expansion of Space

The Hubble diagram for type Ia supernovae.

Kirshner R P PNAS 2004;101:8-13

©2004 by National Academy of Sciences 21 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology

Standard Big Bang Cosmology (SBB): the old paradigm ofcosmology (ca. 1960).

The SBB is based on:

Cosmological principle: universe homogeneous andisotropic on large scales.General Relativity governing dynamics of space-time.Classical matter as source in the Einstein equations.Classical matter: cold (pressure-less) matter(describing the galaxies) + radiation(describing theCMB).

22 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology

Standard Big Bang Cosmology (SBB): the old paradigm ofcosmology (ca. 1960).

The SBB is based on:

Cosmological principle: universe homogeneous andisotropic on large scales.General Relativity governing dynamics of space-time.Classical matter as source in the Einstein equations.Classical matter: cold (pressure-less) matter(describing the galaxies) + radiation(describing theCMB).

22 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology

Standard Big Bang Cosmology (SBB): the old paradigm ofcosmology (ca. 1960).

The SBB is based on:

Cosmological principle: universe homogeneous andisotropic on large scales.General Relativity governing dynamics of space-time.Classical matter as source in the Einstein equations.Classical matter: cold (pressure-less) matter(describing the galaxies) + radiation(describing theCMB).

22 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology

Standard Big Bang Cosmology (SBB): the old paradigm ofcosmology (ca. 1960).

The SBB is based on:

Cosmological principle: universe homogeneous andisotropic on large scales.General Relativity governing dynamics of space-time.Classical matter as source in the Einstein equations.Classical matter: cold (pressure-less) matter(describing the galaxies) + radiation(describing theCMB).

22 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology

Standard Big Bang Cosmology (SBB): the old paradigm ofcosmology (ca. 1960).

The SBB is based on:

Cosmological principle: universe homogeneous andisotropic on large scales.General Relativity governing dynamics of space-time.Classical matter as source in the Einstein equations.Classical matter: cold (pressure-less) matter(describing the galaxies) + radiation(describing theCMB).

22 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

The universe is expanding now.In the past it was hotter and more dense.Thus, it was expanding faster in the past.At a finite time in the past the temperature was infinite .A finite box of space had zero size at that time.This is the Big Bang!

What is the Big Bang? What was before the Big Bang?

To be taken seriously a theory must have made successfulobservational predictions.

23 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

The universe is expanding now.In the past it was hotter and more dense.Thus, it was expanding faster in the past.At a finite time in the past the temperature was infinite .A finite box of space had zero size at that time.This is the Big Bang!

What is the Big Bang? What was before the Big Bang?

To be taken seriously a theory must have made successfulobservational predictions.

23 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

The universe is expanding now.In the past it was hotter and more dense.Thus, it was expanding faster in the past.At a finite time in the past the temperature was infinite .A finite box of space had zero size at that time.This is the Big Bang!

What is the Big Bang? What was before the Big Bang?

To be taken seriously a theory must have made successfulobservational predictions.

23 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

The universe is expanding now.In the past it was hotter and more dense.Thus, it was expanding faster in the past.At a finite time in the past the temperature was infinite .A finite box of space had zero size at that time.This is the Big Bang!

What is the Big Bang? What was before the Big Bang?

To be taken seriously a theory must have made successfulobservational predictions.

23 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

The universe is expanding now.In the past it was hotter and more dense.Thus, it was expanding faster in the past.At a finite time in the past the temperature was infinite .A finite box of space had zero size at that time.This is the Big Bang!

What is the Big Bang? What was before the Big Bang?

To be taken seriously a theory must have made successfulobservational predictions.

23 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

The universe is expanding now.In the past it was hotter and more dense.Thus, it was expanding faster in the past.At a finite time in the past the temperature was infinite .A finite box of space had zero size at that time.This is the Big Bang!

What is the Big Bang? What was before the Big Bang?

To be taken seriously a theory must have made successfulobservational predictions.

23 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

The universe is expanding now.In the past it was hotter and more dense.Thus, it was expanding faster in the past.At a finite time in the past the temperature was infinite .A finite box of space had zero size at that time.This is the Big Bang!

What is the Big Bang? What was before the Big Bang?

To be taken seriously a theory must have made successfulobservational predictions.

23 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

The universe is expanding now.In the past it was hotter and more dense.Thus, it was expanding faster in the past.At a finite time in the past the temperature was infinite .A finite box of space had zero size at that time.This is the Big Bang!

What is the Big Bang? What was before the Big Bang?

To be taken seriously a theory must have made successfulobservational predictions.

23 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

The universe is expanding now.In the past it was hotter and more dense.Thus, it was expanding faster in the past.At a finite time in the past the temperature was infinite .A finite box of space had zero size at that time.This is the Big Bang!

What is the Big Bang? What was before the Big Bang?

To be taken seriously a theory must have made successfulobservational predictions.

23 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

Universe begins as a homogeneous and very hotfireball.Initially radiation dominates: hot plasma.Space expands and matter cools.After about 30,000 years cold matter starts to dominate.After about 300,000 years atoms (hydrogen) forms anduniverse becomes transparent to lightNow the age of the universe is about 13 billion years.

Prediction: Existence and black body nature of the CosmicMicrowave Background.

24 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

Universe begins as a homogeneous and very hotfireball.Initially radiation dominates: hot plasma.Space expands and matter cools.After about 30,000 years cold matter starts to dominate.After about 300,000 years atoms (hydrogen) forms anduniverse becomes transparent to lightNow the age of the universe is about 13 billion years.

Prediction: Existence and black body nature of the CosmicMicrowave Background.

24 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

Universe begins as a homogeneous and very hotfireball.Initially radiation dominates: hot plasma.Space expands and matter cools.After about 30,000 years cold matter starts to dominate.After about 300,000 years atoms (hydrogen) forms anduniverse becomes transparent to lightNow the age of the universe is about 13 billion years.

Prediction: Existence and black body nature of the CosmicMicrowave Background.

24 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

Universe begins as a homogeneous and very hotfireball.Initially radiation dominates: hot plasma.Space expands and matter cools.After about 30,000 years cold matter starts to dominate.After about 300,000 years atoms (hydrogen) forms anduniverse becomes transparent to lightNow the age of the universe is about 13 billion years.

Prediction: Existence and black body nature of the CosmicMicrowave Background.

24 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

Universe begins as a homogeneous and very hotfireball.Initially radiation dominates: hot plasma.Space expands and matter cools.After about 30,000 years cold matter starts to dominate.After about 300,000 years atoms (hydrogen) forms anduniverse becomes transparent to lightNow the age of the universe is about 13 billion years.

Prediction: Existence and black body nature of the CosmicMicrowave Background.

24 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

Universe begins as a homogeneous and very hotfireball.Initially radiation dominates: hot plasma.Space expands and matter cools.After about 30,000 years cold matter starts to dominate.After about 300,000 years atoms (hydrogen) forms anduniverse becomes transparent to lightNow the age of the universe is about 13 billion years.

Prediction: Existence and black body nature of the CosmicMicrowave Background.

24 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Standard Big Bang Cosmology (ctd.)

Universe begins as a homogeneous and very hotfireball.Initially radiation dominates: hot plasma.Space expands and matter cools.After about 30,000 years cold matter starts to dominate.After about 300,000 years atoms (hydrogen) forms anduniverse becomes transparent to lightNow the age of the universe is about 13 billion years.

Prediction: Existence and black body nature of the CosmicMicrowave Background.

24 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Credit: NASA/WMAP Science Team

25 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Spectrometer

26 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Successes of the SBB Model

Key success: Existence and black body nature of the CMB.

27 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Unanswered Questions

What is the Big Bang?What was before the Big Bang?

28 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Isotropic CMB Background

29 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Conceptual Problems of the SBB Model

No explanation for the homogeneity, spatial flatness andlarge size and entropy of the universe.Horizon problem of the SBB:

30 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Conceptual Problems of the SBB Model II

No explanation of the observed inhomogeneities in thedistribution of matter and anisotropies in the CosmicMicrowave Background possible!

31 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

What to do?

With a little help from a friend , the particle physicist:

At very high temperatures close to the Big Bangclassical physics breaks down - and quantummechanics and particle physics give the rightdescription of matter.→ Standard Big Bang theory breaks down.In the very early universe matter is a plasma ofelementary particles.All described in terms of quantum fields.Quantum field (scalar fields) can lead to a differentexpansion rate of space namely inflationary expansion.

32 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

What to do?

With a little help from a friend , the particle physicist:

At very high temperatures close to the Big Bangclassical physics breaks down - and quantummechanics and particle physics give the rightdescription of matter.→ Standard Big Bang theory breaks down.In the very early universe matter is a plasma ofelementary particles.All described in terms of quantum fields.Quantum field (scalar fields) can lead to a differentexpansion rate of space namely inflationary expansion.

32 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

What to do?

With a little help from a friend , the particle physicist:

At very high temperatures close to the Big Bangclassical physics breaks down - and quantummechanics and particle physics give the rightdescription of matter.→ Standard Big Bang theory breaks down.In the very early universe matter is a plasma ofelementary particles.All described in terms of quantum fields.Quantum field (scalar fields) can lead to a differentexpansion rate of space namely inflationary expansion.

32 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

What to do?

With a little help from a friend , the particle physicist:

At very high temperatures close to the Big Bangclassical physics breaks down - and quantummechanics and particle physics give the rightdescription of matter.→ Standard Big Bang theory breaks down.In the very early universe matter is a plasma ofelementary particles.All described in terms of quantum fields.Quantum field (scalar fields) can lead to a differentexpansion rate of space namely inflationary expansion.

32 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

What to do?

With a little help from a friend , the particle physicist:

At very high temperatures close to the Big Bangclassical physics breaks down - and quantummechanics and particle physics give the rightdescription of matter.→ Standard Big Bang theory breaks down.In the very early universe matter is a plasma ofelementary particles.All described in terms of quantum fields.Quantum field (scalar fields) can lead to a differentexpansion rate of space namely inflationary expansion.

32 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

What to do?

With a little help from a friend , the particle physicist:

At very high temperatures close to the Big Bangclassical physics breaks down - and quantummechanics and particle physics give the rightdescription of matter.→ Standard Big Bang theory breaks down.In the very early universe matter is a plasma ofelementary particles.All described in terms of quantum fields.Quantum field (scalar fields) can lead to a differentexpansion rate of space namely inflationary expansion.

32 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

What to do?

With a little help from a friend , the particle physicist:

At very high temperatures close to the Big Bangclassical physics breaks down - and quantummechanics and particle physics give the rightdescription of matter.→ Standard Big Bang theory breaks down.In the very early universe matter is a plasma ofelementary particles.All described in terms of quantum fields.Quantum field (scalar fields) can lead to a differentexpansion rate of space namely inflationary expansion.

32 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Plan

1 What is Cosmology?

2 FrameworkSpace-TimeStandard Big Bang Cosmology

3 Inflationary Cosmology

4 String Cosmology

5 Conclusions

33 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Time line of inflationary cosmology

ti : inflation beginstR: inflation ends, reheating

34 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Successes of Inflationary Cosmology

The Inflationary Universe Scenario is the current paradigmof early universe cosmology (1980).

Successes:

Solves horizon problemSolves flatness problemSolves size/entropy problemProvides a causal mechanism of generating primordialcosmological perturbations (Chibisov & Mukhanov,1981).

35 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Successes of Inflationary Cosmology

The Inflationary Universe Scenario is the current paradigmof early universe cosmology (1980).

Successes:

Solves horizon problemSolves flatness problemSolves size/entropy problemProvides a causal mechanism of generating primordialcosmological perturbations (Chibisov & Mukhanov,1981).

35 / 70

Early Universe

R. Branden-berger

Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Successes of Inflationary Cosmology

The Inflationary Universe Scenario is the current paradigmof early universe cosmology (1980).

Successes:

Solves horizon problemSolves flatness problemSolves size/entropy problemProvides a causal mechanism of generating primordialcosmological perturbations (Chibisov & Mukhanov,1981).

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Credit: NASA/WMAP Science Team

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How to Obtain Inflation?

Assume: Space-time described by General RelativityPhase with exponential expansion of space requiresmatter with negative pressureCheap way to obtain this: assume the existence of aslowly rolling scalar field ϕ

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How to Obtain Inflation?

Assume: Space-time described by General RelativityPhase with exponential expansion of space requiresmatter with negative pressureCheap way to obtain this: assume the existence of aslowly rolling scalar field ϕ

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How to Obtain Inflation?

Assume: Space-time described by General RelativityPhase with exponential expansion of space requiresmatter with negative pressureCheap way to obtain this: assume the existence of aslowly rolling scalar field ϕ

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Toy Model of a Scalar Field

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Review of Inflationary Cosmology II

Space-time sketch of inflationary cosmology:

Note:H = a

acurve labelled by k : wavelength of a fluctuation

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Successes of Inflation

inflation renders the universe large, homogeneous andspatially flatclassical matter redshifts → matter vacuum remainsquantum vacuum fluctuations: seeds for the observedstructure [Chibisov & Mukhanov, 1981]

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Status of the Big Bang in InflationaryCosmology

The inflationary phase had a beginning.There was a Big Bang before the period of inflation.

Unanswered questions:

What is the Big Bang?What was before the Big Bang?

Note: quantum field theory is not applicable very close tothe singularity.

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Status of the Big Bang in InflationaryCosmology

The inflationary phase had a beginning.There was a Big Bang before the period of inflation.

Unanswered questions:

What is the Big Bang?What was before the Big Bang?

Note: quantum field theory is not applicable very close tothe singularity.

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Status of the Big Bang in InflationaryCosmology

The inflationary phase had a beginning.There was a Big Bang before the period of inflation.

Unanswered questions:

What is the Big Bang?What was before the Big Bang?

Note: quantum field theory is not applicable very close tothe singularity.

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Conclusions

Challenges for the Current Paradigm

In spite of the phenomenological successes, theinflationary scenario suffers from several conceptualproblems.In light of these problems we need to look for input fromnew fundamental physics to construct a new theorywhich will overcome these problems.Question: Can Superstring theory lead to a new andimproved paradigm?Question: Can this new paradigm be tested incosmological observations?Question: Was there a Big Bang ?

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Conclusions

Challenges for the Current Paradigm

In spite of the phenomenological successes, theinflationary scenario suffers from several conceptualproblems.In light of these problems we need to look for input fromnew fundamental physics to construct a new theorywhich will overcome these problems.Question: Can Superstring theory lead to a new andimproved paradigm?Question: Can this new paradigm be tested incosmological observations?Question: Was there a Big Bang ?

43 / 70

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Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Challenges for the Current Paradigm

In spite of the phenomenological successes, theinflationary scenario suffers from several conceptualproblems.In light of these problems we need to look for input fromnew fundamental physics to construct a new theorywhich will overcome these problems.Question: Can Superstring theory lead to a new andimproved paradigm?Question: Can this new paradigm be tested incosmological observations?Question: Was there a Big Bang ?

43 / 70

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Cosmology

FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

Challenges for the Current Paradigm

In spite of the phenomenological successes, theinflationary scenario suffers from several conceptualproblems.In light of these problems we need to look for input fromnew fundamental physics to construct a new theorywhich will overcome these problems.Question: Can Superstring theory lead to a new andimproved paradigm?Question: Can this new paradigm be tested incosmological observations?Question: Was there a Big Bang ?

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Conclusions

Conceptual Problems of InflationaryCosmology

What is the scalar field?Why does it have the special conditions to obtaininflation?Trans-Planckian problemSingularity problemApplicability of General Relativity

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Trans-Planckian Problem

Success of inflation: At early times scales are insidethe Hubble radius → causal generation mechanism ispossible.Problem: If time period of inflation is slightly more thanthe minimal length it must have, then the wavelength issmaller than the Planck length at the beginning ofinflation→ new physics MUST enter into the calculation of thefluctuations.

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Singularity Problem

Standard cosmology: Penrose-Hawking theorems →initial singularity → incompleteness of the theory.Inflationary cosmology: In scalar field-driveninflationary models the initial singularity persists [Bordeand Vilenkin]→ incompleteness of the theory.

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Singularity Problem

Standard cosmology: Penrose-Hawking theorems →initial singularity → incompleteness of the theory.Inflationary cosmology: In scalar field-driveninflationary models the initial singularity persists [Bordeand Vilenkin]→ incompleteness of the theory.

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Applicability of GR

Einstein’s theory breaks down at extremely highdensities.In models of inflation, the energy scale of at whichinflation takes place is close to the limiting scale for thevalidity of Einstein’s theory.We cannot trust the predictions made using GR.

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Zones of Ignorance

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Message I

The current cosmological paradigm has seriousconceptual problems.We need a new paradigm of very early universecosmology.With a little help from a friend - the string theorist!New cosmological model motivated by superstringtheory: String Gas Cosmology (SGC) [R.B. and C.Vafa, 1989].New structure formation scenario emerges from SGC[A. Nayeri, R.B. and C. Vafa, 2006].

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Message I

The current cosmological paradigm has seriousconceptual problems.We need a new paradigm of very early universecosmology.With a little help from a friend - the string theorist!New cosmological model motivated by superstringtheory: String Gas Cosmology (SGC) [R.B. and C.Vafa, 1989].New structure formation scenario emerges from SGC[A. Nayeri, R.B. and C. Vafa, 2006].

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Message I

The current cosmological paradigm has seriousconceptual problems.We need a new paradigm of very early universecosmology.With a little help from a friend - the string theorist!New cosmological model motivated by superstringtheory: String Gas Cosmology (SGC) [R.B. and C.Vafa, 1989].New structure formation scenario emerges from SGC[A. Nayeri, R.B. and C. Vafa, 2006].

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Message I

The current cosmological paradigm has seriousconceptual problems.We need a new paradigm of very early universecosmology.With a little help from a friend - the string theorist!New cosmological model motivated by superstringtheory: String Gas Cosmology (SGC) [R.B. and C.Vafa, 1989].New structure formation scenario emerges from SGC[A. Nayeri, R.B. and C. Vafa, 2006].

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Message II

String Gas Cosmology makes testable predictions forcosmological observations

Blue tilt in the spectrum of gravitational waves [R.B., A.Nayeri, S. Patil and C. Vafa, 2006]

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Message II

String Gas Cosmology makes testable predictions forcosmological observations

Blue tilt in the spectrum of gravitational waves [R.B., A.Nayeri, S. Patil and C. Vafa, 2006]

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Plan

1 What is Cosmology?

2 FrameworkSpace-TimeStandard Big Bang Cosmology

3 Inflationary Cosmology

4 String Cosmology

5 Conclusions

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What is String Theory?

String theory is a quantum theory of all forces of natureincluding gravity.String theory unifies all forces of nature.Basic objects: elementary strings. Compared toelementary point particles.String theory is mathematically consistent only in 10space-time dimensions.Thus, string theory predicts extra spatial dimensions.

Note: string theory is “in development".

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Conclusions

What is String Theory?

String theory is a quantum theory of all forces of natureincluding gravity.String theory unifies all forces of nature.Basic objects: elementary strings. Compared toelementary point particles.String theory is mathematically consistent only in 10space-time dimensions.Thus, string theory predicts extra spatial dimensions.

Note: string theory is “in development".

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Std. Cosmology

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String gas

Conclusions

What is String Theory?

String theory is a quantum theory of all forces of natureincluding gravity.String theory unifies all forces of nature.Basic objects: elementary strings. Compared toelementary point particles.String theory is mathematically consistent only in 10space-time dimensions.Thus, string theory predicts extra spatial dimensions.

Note: string theory is “in development".

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FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

What is String Theory?

String theory is a quantum theory of all forces of natureincluding gravity.String theory unifies all forces of nature.Basic objects: elementary strings. Compared toelementary point particles.String theory is mathematically consistent only in 10space-time dimensions.Thus, string theory predicts extra spatial dimensions.

Note: string theory is “in development".

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FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

What is String Theory?

String theory is a quantum theory of all forces of natureincluding gravity.String theory unifies all forces of nature.Basic objects: elementary strings. Compared toelementary point particles.String theory is mathematically consistent only in 10space-time dimensions.Thus, string theory predicts extra spatial dimensions.

Note: string theory is “in development".

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FrameworkSpace-Time

Std. Cosmology

Inflation

String gas

Conclusions

What is String Theory?

String theory is a quantum theory of all forces of natureincluding gravity.String theory unifies all forces of nature.Basic objects: elementary strings. Compared toelementary point particles.String theory is mathematically consistent only in 10space-time dimensions.Thus, string theory predicts extra spatial dimensions.

Note: string theory is “in development".

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PrinciplesR.B. and C. Vafa, Nucl. Phys. B316:391 (1989)

Idea: make use of the new symmetries and new degrees offreedom which string theory provides to construct a newtheory of the very early universe.Assumption: Matter is a gas of fundamental stringsAssumption: Space is compact, e.g. a torus.Key points:

New degrees of freedom: string oscillatory modes.Leads to a maximal temperature for a gas of strings,the Hagedorn temperature.New degrees of freedom: string winding modes.Leads to a new symmetry: physics at large R isequivalent to physics at small R.

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PrinciplesR.B. and C. Vafa, Nucl. Phys. B316:391 (1989)

Idea: make use of the new symmetries and new degrees offreedom which string theory provides to construct a newtheory of the very early universe.Assumption: Matter is a gas of fundamental stringsAssumption: Space is compact, e.g. a torus.Key points:

New degrees of freedom: string oscillatory modes.Leads to a maximal temperature for a gas of strings,the Hagedorn temperature.New degrees of freedom: string winding modes.Leads to a new symmetry: physics at large R isequivalent to physics at small R.

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PrinciplesR.B. and C. Vafa, Nucl. Phys. B316:391 (1989)

Idea: make use of the new symmetries and new degrees offreedom which string theory provides to construct a newtheory of the very early universe.Assumption: Matter is a gas of fundamental stringsAssumption: Space is compact, e.g. a torus.Key points:

New degrees of freedom: string oscillatory modes.Leads to a maximal temperature for a gas of strings,the Hagedorn temperature.New degrees of freedom: string winding modes.Leads to a new symmetry: physics at large R isequivalent to physics at small R.

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“Large" is Equivalent to “Small" in String Theory

T-Duality Symmetry

Momentum modes are light if space is large: En = n/RWinding modes are light if space is small: Em = mRLlarge space is equivalent to small spaceSymmetry: R → 1/R (n,m) → (m,n)Mass spectrum of string states unchanged

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“Large" is Equivalent to “Small" in String Theory

T-Duality Symmetry

Momentum modes are light if space is large: En = n/RWinding modes are light if space is small: Em = mRLlarge space is equivalent to small spaceSymmetry: R → 1/R (n,m) → (m,n)Mass spectrum of string states unchanged

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“Large" is Equivalent to “Small" in String Theory

T-Duality Symmetry

Momentum modes are light if space is large: En = n/RWinding modes are light if space is small: Em = mRLlarge space is equivalent to small spaceSymmetry: R → 1/R (n,m) → (m,n)Mass spectrum of string states unchanged

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Temperature in String CosmologyR.B. and C. Vafa, Nucl. Phys. B316:391 (1989)

Temperature of a box of strings in thermal equilibrium.

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Temperature in Standard and InflationaryCosmology

Temperature of a box of particles in thermal equilibrium.

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String Gas CosmologyR.B. and C. Vafa, Nucl. Phys. B316:391 (1989)

We will thus consider the following background dynamics forthe scale factor a(t):

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Dimensionality of Space in SGC

Begin with all 9 spatial dimensions small, initialtemperature close to TH → winding modes about allspatial sections are excited.Expansion of any one spatial dimension requires theannihilation of the winding modes in that dimension.

Decay only possible in three large spatial dimensions.→ dynamical explanation of why there are exactly threelarge spatial dimensions.

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Dimensionality of Space in SGC

Begin with all 9 spatial dimensions small, initialtemperature close to TH → winding modes about allspatial sections are excited.Expansion of any one spatial dimension requires theannihilation of the winding modes in that dimension.

Decay only possible in three large spatial dimensions.→ dynamical explanation of why there are exactly threelarge spatial dimensions.

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Conclusions

Structure formation in inflationary cosmology

N.B. Perturbations originate as quantum vacuumfluctuations.

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Background for string gas cosmology

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Structure formation in string gas cosmologyA. Nayeri, R.B. and C. Vafa, Phys. Rev. Lett. 97:021302 (2006)

N.B. Perturbations originate as thermal string gasfluctuations.

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Power spectrum of cosmological fluctuations

Key features:

scale-invariant like for inflationslight red tilt like for inflation

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Anisotropies in the Cosmic MicrowaveBackground (CMB)

Credit: NASA/WMAP Science Team63 / 70

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Quantification of the CMB data

Credit: NASA/WMAP Science Team

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Spectrum of Gravitational Waves

Key features:

scale-invariant (like for inflation)slight blue tilt (unlike for inflation)

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BICEP-2 Results

0 50 100 150 200 250 300−0.01

0

0.01

0.02

0.03

0.04

0.05

Multipole

l(l+

1)C

lBB/2

π [µ

K2 ]

B2xB2B2xB1cB2xKeck (preliminary)

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Status of the “Big Bang" in String GasCosmology

The universe was very, very hot and dense 13 billionyears ago.In this sense there was a hot “primordial" fireball.But: there was no Big Bang Singularity.There was no beginning of time.

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Status of the “Big Bang" in String GasCosmology

The universe was very, very hot and dense 13 billionyears ago.In this sense there was a hot “primordial" fireball.But: there was no Big Bang Singularity.There was no beginning of time.

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Conclusions

Plan

1 What is Cosmology?

2 FrameworkSpace-TimeStandard Big Bang Cosmology

3 Inflationary Cosmology

4 String Cosmology

5 Conclusions

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Conclusions

Cosmology is a vibrant field with lots of observationaldata.Paradigms of early universe cosmology have beendeveloped.Paradigm 1: Standard Big Bang Model.Paradigm 2: Inflationary Universe scenario - currentparadigm.In both Paradigms 1 and 2 there was a Big Bangsingularity.Paradigms 1 and 2 have conceptual problems →motivates the search for an improved paradigm.Superstring theory may provide a new paradigm.Superstring cosmology may resolve the Big Bangsingularity.It is possible to observationally probe string cosmology.

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Conclusions

Cosmology is a vibrant field with lots of observationaldata.Paradigms of early universe cosmology have beendeveloped.Paradigm 1: Standard Big Bang Model.Paradigm 2: Inflationary Universe scenario - currentparadigm.In both Paradigms 1 and 2 there was a Big Bangsingularity.Paradigms 1 and 2 have conceptual problems →motivates the search for an improved paradigm.Superstring theory may provide a new paradigm.Superstring cosmology may resolve the Big Bangsingularity.It is possible to observationally probe string cosmology.

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Conclusions

Conclusions

Cosmology is a vibrant field with lots of observationaldata.Paradigms of early universe cosmology have beendeveloped.Paradigm 1: Standard Big Bang Model.Paradigm 2: Inflationary Universe scenario - currentparadigm.In both Paradigms 1 and 2 there was a Big Bangsingularity.Paradigms 1 and 2 have conceptual problems →motivates the search for an improved paradigm.Superstring theory may provide a new paradigm.Superstring cosmology may resolve the Big Bangsingularity.It is possible to observationally probe string cosmology.

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Std. Cosmology

Inflation

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Conclusions

Conclusions

Cosmology is a vibrant field with lots of observationaldata.Paradigms of early universe cosmology have beendeveloped.Paradigm 1: Standard Big Bang Model.Paradigm 2: Inflationary Universe scenario - currentparadigm.In both Paradigms 1 and 2 there was a Big Bangsingularity.Paradigms 1 and 2 have conceptual problems →motivates the search for an improved paradigm.Superstring theory may provide a new paradigm.Superstring cosmology may resolve the Big Bangsingularity.It is possible to observationally probe string cosmology.

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Conclusions

Status of the “Big Bang"

We know that going back in time 13 billion years therewas a very hot early phase, a primordial fireball.If this is what you mean by “Big Bang": then there WASa “Big Bang".We do not know if there was a “Big Bang singularity", abeginning of time.Our current paradigms of early universe cosmologypredict a beginning of time.But only if we extrapolate the models beyond wherethey can be used.Superstring theory may lead to a cosmology without abeginning of time.If this is true then there may not have been a “BigBang" (singularity).

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