65
Stars

Stars. I.Introduction A. Some ‘observations’ During the 20 th Century 1. Our Sun is not the center of our Galaxy

Embed Size (px)

Citation preview

Stars

Stars

I. Introduction

A. Some ‘observations’

During the 20th Century

1. Our Sun is not the center of our Galaxy

During the 20th Century

1. Our Sun is not the center of our Galaxy

2. There is nothing special about our Sun - it is quite ordinary among billions of other stars.

During the 20th Century

1. Our Sun is not the center of our Galaxy

2. There is nothing special about our Sun - it is quite ordinary among billions of other stars.

3. Our galaxy is not the only one. There are billions of other galaxies.

During the 20th Century

1. Our Sun is not the center of our Galaxy

2. There is nothing special about our Sun - it is quite ordinary among billions of other stars.

3. Our galaxy is not the only one. There are billions of other galaxies.

4. Our existence on Earth depends upon the Sun’sstability . Both the Sun and the Earth are

quite mortal, and will not exist forever.

During the 20th Century

1. Our Sun is not the center of our Galaxy

2. There is nothing special about our Sun - it is quite ordinary among billions of other stars.

3. Our galaxy is not the only one. There are billions of other galaxies.

4. Our existence on Earth depends upon the Sun’sstability . Both the Sun and the Earth are

quite mortal, and will not exist forever.

5. The Universe is expanding.

Stars

I. Introduction

A. Some ‘observations’

B. The expanding Universe

‘how do we know?’

The Doppler EffectDoppler Effect

The “RED SHIFT”

THE BIG BANG THEORYTHE BIG BANG THEORY

The Universe is Expanding Everywhere - Everything is moving away from everything else.

The “RED SHIFT”

The Doppler EffectDoppler Effect

THE BIG BANG THEORYTHE BIG BANG THEORY

The Universe is Expanding Everywhere - Everything is moving away from everything else.

The “RED SHIFT”

The Doppler EffectDoppler Effect

Edwin Hubble: HUBBLE’ LAWHUBBLE’ LAW - Galaxies are receding in every direction. Those furthest away are moving at the fastest rate: v = H d

[H = 50 km/sec per megaparsec]

Megaparsec = 3.26 x 106 Light Years

Stars

I. Introduction

A. Some ‘observations’

B. The expanding Universe

C. Classifying Stars

HERTZPRUNG - RUSSEL DIAGRAMHERTZPRUNG - RUSSEL DIAGRAM

A Classification of Stars

And

The Evolution of Stars

HERTZPRUNG - RUSSEL DIAGRAMHERTZPRUNG - RUSSEL DIAGRAM

A Classification of Stars

And

The Evolution of StarsLuminosity (Brightness) vs. Surface Temperature

See Fig. 14-6 in Text

Main Sequence

Red Giants

Super Giants

White Dwarfs

Black Dwarfs

II. The Life Cycles of Stars

A. The Birth of Stars

Planetary Nebula

II. The Life Cycles of Stars

A. The Birth of StarsB. The Main Sequence and the Death of

Stars

II. The Life Cycles of Stars

A. The Birth of StarsB. The Main Sequence and the Death of

Stars1. Our Sun Hydrogen burning (fusion)

H + H He

II. The Life Cycles of Stars

A. The Birth of StarsB. The Main Sequence and the Death of Stars

1. Our Sun Hydrogen burning (fusion)

H + H He

1H2 + 1H2 = 2He3 + neutron + Energy

Hydrogen [H] is fusing to Helium [He] which accumulates in the core.

Hydrogen [H] is fusing to Helium [He] which accumulates in the core.

No Fusion in the core: results in less pressure pushing outward

Hydrogen [H] is fusing to Helium [He] which accumulates in the core.

No Fusion in the core: results in less pressure pushing outward

Greater mass concentration: Gravitational collapse inward which causes increased (100x) Hydrogen fusion of sun

Hydrogen [H] is fusing to Helium [He] which accumulates in the core.

No Fusion in the core: results in less pressure pushing outward

Greater mass concentration: Gravitational collapse inward which causes increased (100x) Hydrogen fusion of sun

This event causes rapid expansion of the outer layers into a Red Giant .This causes a cooling of the outer portion of sun.

Helium [He] continues to accumulate at rapid rate in core until 100 million degrees is reached.

Additional burning………

Helium [He] continues to accumulate at rapid rate in core until 100 million degrees is reached.

Additional burning……… Helium burning (fusion)

He + He + He C

Helium [He] continues to accumulate at rapid rate in core until 100 million degrees is reached.

Additional burning……… Helium burning (fusion)

He + He + He C

2He4 + 2He4 +

2He4 = 6C12 + Energy

Carbon accumulates in core continually……

……. raising pressure, temperature and mass.

Carbon accumulates in core continually raising pressure, temperature and mass.

Gravitational Forces Take over and Red Giant collapses to size of planet earth. Most H and He has been consumed and converted to Carbon

Carbon accumulates in core continually raising pressure, temperature and mass.

Gravitational Forces Take over and Red Giant collapses to size of planet earth. Most H and He has been consumed and converted to Carbon

White Hot core of Carbon remains [White Dwarf] which will cool to a Black DwarfBlack Dwarf

Carbon accumulates in core continually raising pressure, temperature and mass.

Gravitational Forces Take over and Red Giant collapses to size of planet earth. Most H and He has been consumed and converted to Carbon

White Hot core of Carbon remains [White Dwarf] which will cool to a Black Dwarf

One Teaspoon weighs about 2000 pounds

II. The Life Cycles of Stars

A. The Birth of StarsB. The Main Sequence and the Death of

Stars1. Our Sun2. Stars ~4x mass of our Sun

2. Stars ~4x mass of our Suna. Red Giant collapses

2. Stars ~4x mass of our Suna. Red Giant collapsesb. Fusion continues

He + He + He C

2. Stars ~4x mass of our Suna. Red Giant collapsesb. Fusion continues

He + He + He C

C O Si Fe

2. Stars ~4x mass of our Suna. Red Giant collapsesb. Fusion continues

He + He + He C

C O Si Fe

c. IMPLOSION!!!!!!

2. Stars ~4x mass of our Suna. Red Giant collapsesb. Fusion continues

He + He + He C

C O Si Fe

c. IMPLOSION!!!!!!

d. Supernova develops

2. Stars ~4x mass of our Suna. Red Giant collapsesb. Fusion continues

He + He + He C

C O Si Fe

c. IMPLOSION!!!!!!

d. Supernova develops

e. New Elements are created

2. Stars ~4x mass of our Suna. Red Giant collapsesb. Fusion continues

He + He + He C

C O Si Fe

c. IMPLOSION!!!!!!

d. Supernova develops

e. New Elements form

f. Neutron Stars and Pulsars

NEUTRON STAR - NEUTRON STAR - Electrons Driven into Protons of the Nucleus by unstoppable gravity

NEUTRON STAR - NEUTRON STAR - Electrons Driven into Protons of the Nucleus by unstoppable gravity

20 - 30 km -Very Rapid Rotation - 1 Trillion Times Denser Than Sun - Not an element - Magnetic Field

NEUTRON STAR - NEUTRON STAR - Electrons Driven into Protons of the Nucleus by unstoppable gravity

20 - 30 km -Very Rapid Rotation - 1 Trillion Times Denser Than Sun - Not an element - Magnetic Field

PULSAR - PULSAR - Neutron Star with strong electromagnetic beam, Neutron Star with strong electromagnetic beam, and rapid rotation.and rapid rotation.

PULSARS

II. The Life Cycles of Stars

A. The Birth of StarsB. The Main Sequence and the Death of

Stars1. Our Sun2. Stars ~4x mass of our Sun3. Mega Stars (~6x mass of our Sun)

II. The Life Cycles of Stars

3. Mega Stars (~6x mass of our Sun)

a. Same progression as before, but….

BLACK HOLE

BLACK HOLE BLACK HOLE - The Extreme- Only from Super Giants – - The Extreme- Only from Super Giants –

Similar to Neutron Star but collapse continues to infinite LargeSimilar to Neutron Star but collapse continues to infinite Large

Mass and Small Size. Mass and Small Size.

- Escape Velocity of Light Exceeded.- Escape Velocity of Light Exceeded.

IN SUMMARY…..

Stars

III. In the beginning……

COSMOLOGYCOSMOLOGY = Studies the beginning and the ending of cosmic time.

COSMOLOGYCOSMOLOGY = Studies the beginning and the ending of cosmic time.

BIG BANGBIG BANG: 15 to 20 Billion Years Ago

COSMOLOGYCOSMOLOGY = Studies the beginning and the ending of cosmic time.

BIG BANGBIG BANG: 15 to 20 Billion Years Ago

10 - 43 Sec after The Big Bang

TEMPERATURE: 10 32 K

COSMOLOGYCOSMOLOGY = Studies the beginning and the ending of cosmic time.

BIG BANGBIG BANG: 15 to 20 Billion Years Ago

10 - 43 Sec after The Big Bang

TEMPERATURE: 10 32 K

0.1 Sec: 100 billion K

COSMOLOGYCOSMOLOGY = Studies the beginning and the ending of cosmic time.

BIG BANGBIG BANG: 15 to 20 Billion Years Ago

10 - 43 Sec after The Big Bang

TEMPERATURE: 10 32 K

0.1 Sec: 100 billion K

1.0 Sec: 10 billion K [ Protons & Neutrons can begin to form]

COSMOLOGYCOSMOLOGY = Studies the beginning and the ending of cosmic time.

BIG BANGBIG BANG: 15 to 20 Billion Years Ago

10 - 43 Sec after The Big Bang

TEMPERATURE: 10 32 K

0.1 Sec: 100 billion K

1.0 Sec: 10 billion K [ Protons & Neutrons can begin to form]

1 Million Years: Temperatures drop where Electrons and Nuclei form atoms

BEFORE THE BEGINNING OF TIME

?Matter, Time, Space, Energy

A “COSMIC EGG” ?

Beyond Scope of Science