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Stellar Evolution: Outline Interstellar Medium (dust) Hydrogen and Helium Small amounts of Carbon Dioxide (makes it easier to detect) Massive amounts of material between 100,000 and 10,000,000 solar masses Gravitational Collapse of dust Competing forces of pressure and gravity where gravity “wins” Collapse “ignites” nuclear fuel Causes stellar birth and stellar death

Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

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Page 1: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Stellar Evolution: Outline

● Interstellar Medium (dust)– Hydrogen and Helium– Small amounts of Carbon

Dioxide (makes it easier to detect)

– Massive amounts of material between 100,000 and 10,000,000 solar masses

● Gravitational Collapse of dust– Competing forces of pressure

and gravity where gravity “wins”

– Collapse “ignites” nuclear fuel

– Causes stellar birth and stellar death

Page 2: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Stellar Evolution: Outline part 2

● Contraction of the cloud– Slow gravitational pull on

particles (million years or so)– Collapsing cloud becomes

opaque and heats up– Temperature increases

therefore pressure increase● Slows contraction● Several million years● Shines in IR (is not

ignited yet)● Eventually core gets hot

enough to initiate hydrogen fusion

Page 3: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Proto-star

● Proto-star– The beginnings of a star– 10,000,000 K at which point

hydrogen fuses to helium● Star is ignited● Burns due to nuclear fusion

– Star reaches an equilibrium with gravity● Pressure and gravity are

equal● Will stay equal until gravity

wins again – death– When star transitions into a

“real” star the star is called a Zero Age Main Sequence (ZAMS) star.

Page 4: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Fusion produces a star

● Hydrogen fusion– Hydrogen does NOT burn into helium– Hydrogen fuses together to form

helium

– This reaction has a mass loss (the right side has less mass then the left side)

– Mass loss is converted into energy– Mass loss is mostly due to binding

energy● The two protons and two neutrons in the

helium atom weights less when then they individually due when “binded” into a helium atom

● That mass loss is converted to energy

4 H11+4 e→2 He2

4+2e

Page 5: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Young Star

● http://hubblesite.org/newscenter/newsdesk/archive/releases/2006/07/image/a+zoom

● Young star– Many different types– Hot and blue– Cool and red– Low mass, high mass– On the main sequence now

(H-R diagram)● Off main sequence in

birth and death● In galaxy at right young

blue stars are in the arms and older yellowish stars are in the center

Page 6: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Energetic Young Star and Jets

● Young Star– Energetic outflows associated

with young stars● In this picture your star

responsible is not seen on the top of the picture

● Magnetic fields of collapsing rotating clouds are responsible

● Jets– Used to dissipate excess

angular momentum (important so the star doesn't tear itself apart)

Page 7: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Middle-aged Star

● Middle-aged Star– On main sequence– Many different types– Generally 0.8 to 8 solar

mass– No more jets, just a

“normal” star

Page 8: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Mature Star

● Mature Star– Hydrogen is used up– Nuclear process

ceases and gravity starts to win again

● Inner core compresses

● Outer layers expand

Page 9: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Red Giant● Red Giant

– Outer layer expands– Our Sun: passes Earth– Hydrogen “shell” still burns– Will fuse helium slowly

● Triple fusion into carbon● Some less massive stars fuse

helium fast– Helium flash

● Temperatures rise● Helium burns

– 100,000,000 K allows this fusion to take place

– ~ 500000 years– Blue stars

● Off main sequence

Page 10: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Red Giant example

Page 11: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Planetary Nebula

● Planetary Nebula– Eventually the star

(assuming a “normal star”) will eject material

– This material will spread out into the Universe and will be used again

Page 12: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Death of a star● Death of a star

– Low-mass stars● Universe isn't old enough

to know– Medium-mass stars

● Red Giant for 1 billion years

● Planetary nebula star to form from instabilities

● Core is a white dwarf– Radiates heat, but

has no fuel– Eventually turns to a

black dwarf– Massive stars

● Fusion goes to heavier elements

Page 13: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Supernova

● Massive stars– Fusion goes to iron– Iron absorbs energy but

cannot fuse...boom– Supernova

● Supernova– Neutron stars

● Electrons go into protons to form neutrons

● Rapidly rotating● Very very dense● Size of a city● Pulsars

– Black holes● Light does not escape● Event horizon● Wormhole?

Page 14: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Evolution of stars from Alpha to Omega

● Alpha to Omega– On the edges dark clouds

where formation of stars begin

– As we go into the picture stellar nurseries in pillars of dust

– In the middle young blue stars whose stellar winds blow away the interstellar gas

– Somewhat right of the cluster is the ring typical of supernovas (like 1987A)

Page 15: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

FYI: Our Sun

Page 16: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Why different wavelengths?

● Molecular – Emission in microwave, then infrared● Young star – Emission in IR, note jets● Disk – Emits in the IR● Mature star – Emits in X-ray and UV

● Molecular Young Star Disk Mature Star

Page 17: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Black Holes

● Theorized in Newtonian times, but not like the modern black hole idea

● Forms into a singularity– Zero volume– Not allowed by Quantum

Mechanics...● Types

– Not spinning● Event horizon

– Spinning ● Kerr-Newman black hole● All mass in a singularity● Will have an event

horizon plus● Kerr solution leads to

possible “wormhole” to a negative universe

Page 18: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Black Hole Formation

● Black Hole Formation– Stellar– Accumulation of extra mass

from a companion as in a binary system

– Stellar remains (like white dwarf or neutron stars) merging

● Likely will form super massive black holes

● Galaxies with bulges seem to have super massive black holes – NEW EVIDENCE suggests black holes from before the galaxies...

● Image: Wikipedia

Page 19: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Black Hole Eating a Star

Page 20: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Black Holes colliding (will merge)

Page 21: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Black Holes in Merging Galaxies

Page 22: Stellar Evolution: Outline - Academic Computer Centeracademic.pgcc.edu/~sjohnson/lecture17_psc101.pdfStellar Evolution: Outline part 2 ... – Stellar remains (like white dwarf or

Micro Black Holes

● Black Hole Formation– Mini-black holes? Have been

reported in particle accelerators = fireballs

● Not a gravitational object however; so...

● Some believe there were many micro black holes formed at the beginning of the universe and the “zip” through Earth even today...still needs to be proved….