Chapter 13: High Mass Star Evolution and their Remnants: NSs and BHs - - PowerPoint PPT Presentation

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Chapter 13: High Mass Star Evolution and their Remnants: NSs and BHs - - PowerPoint PPT Presentation

Jan 01, 2024 30 likes •820 views

Chapter 13: High Mass Star Evolution and their Remnants: NSs and BHs Chapter 13 Reading Assignment due now! Are your grades in Canvas correct??? Midterms available up front Turn in extra credit planetarium and public observing reports up front

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Fall 2019: Chapter 13 ASTR/PHYS 1060: The Universe

Chapter 13: High Mass Star Evolution and their Remnants: NSs and BHs

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Chapter 13 Reading Assignment due now! Are your grades in Canvas correct??? Midterms available up front Turn in extra credit planetarium and public

  • bserving reports up front when complete
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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Nobel Prize in Physics goes to… Astronomers!

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Jim Peebles various contributions to cosmology Michel Mayor and Didier Queloz first exoplanet around a main sequence star

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Nobel Prize in Physics goes to… Astronomers!

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Jim Peebles various contributions to cosmology Michel Mayor and Didier Queloz first exoplanet around a main sequence star

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13 4 4

Future Evolution

  • f the Sun
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How do we know the different stages of a star's life? We

  • bviously have not been observing

stars for long enough to see it go through all the stages.

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 12 6

Star Clusters: stars of many masses born at the same time

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Which of these star clusters is the oldest?

A B C

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Theory (red line) & Observations (white dots)

We can make a model of any star based on its mass and age

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Which stars in this cluster are the most massive?

A B C D

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 12

Because stars in clusters form at the same time, and a star’s evolution is determined primarily by its mass, we can

  • bserve many

clusters and figure

  • ut how stars evolve

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How do these stars evolve?

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

H Burning in High Mass Stars: CNO Cycle

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Very Temperature Sensitive (higher temp = more energy)

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

High Mass Stars = High Core Temps = CNO

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High Mass Low Mass

Llamas live hard and fast. CNO cycling is my bag, baby

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Evolution of High Mass Stars

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Time spent on the Main Sequence is short: why? A) CNO is much more efficient B) Massive stars use up their fuel more quickly C) Not all the hydrogen in the core gets burned D) The core is much smaller than a low mass star

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Evolution

  • f High

Mass Stars

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Based on this graph, what do you think the heaviest element is that is fused inside of stars?

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A) Lithium B) Iron C) Lead D) Uranium

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Cepheid Variables

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Aside: Standard Candles

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Cepheid Variables Type Ia Supernovae

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

What happens when close binary stars evolve?

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What is this???

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

What happens when close binary stars evolve?

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

What happens when close binary stars evolve?

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

What happens when close binary stars evolve?

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

What happens when close binary stars evolve?

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

What happens when close binary stars evolve?

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

What happens when close binary stars evolve?

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

What happens when close binary stars evolve?

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Type Ia Supernovae

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Back to Massive Star Evolution

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Eta Carinae binary star

What causes massive stars to have strong winds?

A) High surface temperatures B) Light elements in their atmospheres C) Strong radiation pressure (from photons) D) Like Llamas, they’re quite gassy

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13 28

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Type II Supernovae

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Before After

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Betelgeuse: Future Supernova

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… were a supernova to go off within about 30 light- years of us, that would lead to major effects on the Earth, possibly mass extinctions. X-rays and more energetic gamma-rays from the supernova could destroy the ozone layer that protects us from solar ultraviolet rays. It also could ionize nitrogen and

  • xygen in the atmosphere, leading to the formation
  • f large amounts of smog-like nitrous oxide in the

atmosphere.

  • Mark Reid, Harvard-Smithsonian CfA

430 light-years away (safe distance, unless it explodes as a gamma ray burst pointed at us) May appear as bright as the full moon, visible during the day!

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Fall 2019: Chapter 13 ASTR/PHYS 1060: The Universe

Chapter 13: High Mass Star Evolution and their Remnants: NSs and BHs

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Chapter 14 Reading Assignment due next Tuesday Turn in extra credit planetarium and public

  • bserving reports up front when complete

Stellar Lifetimes worksheet due now! Are your grades in Canvas correct??? Midterms available up front

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Fall 2019: Chapter 13 ASTR/PHYS 1060: The Universe

How lost are you regarding stellar evolution? (Chapters 12 & 13, the most recent ones)

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A) Not lost at all - I’m a little bored to be honest B)It mostly makes sense - I’m following it as well as I followed the material in previous chapters C)It’s a lot more confusing - I kind of get it, but am really worried about what I need to know for the next midterm exam D)What’s stellar evolution?

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 10

Hertzsprung-Russell (HR) Diagram

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Spectral Type, Color, Temperature

  • n the x-axis

Luminosity (intrinsic brightness)

  • n the y-axis

Blackbody Spectra

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High Mass Star Low Mass Star

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Nuclear Reactions

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Hydrogen or higher atomic number element collides with proton Proton fuses with the element, producing a photon and sometimes a neutrino

(if the proton turns into a neutron, the new nucleus has to eject a positron [anti-electron] and a neutrino to conserve charge and angular momentum)

Process continues with new elements until temperature can no longer get high enough

  • r Iron (Fe) is all that’s left in the core

[To fuse Fe, the reaction no longer produces a photon but NEEDS to absorb a photon]

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Type II Supernovae

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Type II Supernovae

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Supernova Remnants

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Cygnus Loop

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Grefenstette+ 14,16

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Cas A

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Heavy elements are created in massive stars, with the heaviest elements created in and returned to interstellar space by supernovae

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Created in supernovae caused by NS-NS mergers??

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A question for Neil DeGrasse Tyson… http://www.youtube.com/watch?v=9D05ej8u-gU

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Fall 2019: Chapter 13 ASTR/PHYS 1060: The Universe

Chapter 13: High Mass Star Evolution and their Remnants: NSs and BHs

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Chapter 14 Reading Assignment due next Tuesday Turn in extra credit planetarium and public

  • bserving reports up front when complete

Are your grades in Canvas correct??? Midterms available up front

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13 45

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Stellar Remnant Activity

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Goal: Contrast the end-stages of stars’ lives, black holes, neutron stars, and white dwarfs. Group Activity: Groups of 3-4 Hand in one sheet for the group Roles: Secretary (write on the sheet) Spokesperson (for class discussion) Group Leader (keep on task)

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Neutron Stars

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https://www.youtube.com/watch?v=WTKA2biEVgg

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Neutron Stars / Pulsars

Exploded 1054

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https://www.youtube.com/watch?v=_KCCKl9SB90 Crab Nebula Expansion

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https://www.youtube.com/watch?v=_diLnFGRSFQ Exploded 1572 Exploded ~1680

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www.youtube.com/watch?v=t5uA1RJsDhw&feature=related

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Neutron Stars are born with strong magnetic fields (get stronger as the core collapses) Field accelerates electrons and positrons, which causes them to emit radiation across the spectrum We see the beam once

  • r twice each time the

star rotates

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https://www.youtube.com/watch?v=jwC6_oWwbSE Pulsar Computer Simulation

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Low magnetic field neutron stars and black holes are observed through accretion

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https://www.youtube.com/watch?v=MPpDTvYL5ik Millisecond Pulsar

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https://www.youtube.com/watch?v=-SoZ1xvCpMw Black Widow Pulsar

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https://youtu.be/aMTwtb3TVIk Official NASA Black Hole Safety Video

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Fall 2019: Chapter 13 ASTR/PHYS 1060: The Universe

How do we know black holes ACTUALLY exist in the Universe?

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Highly suggestive results that black holes exist

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Animation of gas falling into SMBH in M87 galaxy Stars orbiting SMBH in center of our galaxy

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Cygnus X-1: First X-ray source and confirmed black hole

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https://www.youtube.com/watch?v=ZdjCpSCh02g

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

GALEX NuSTAR

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Andromeda Galaxy (M31)

Cygnus X-1

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Fall 2019: Chapter 13 ASTR/PHYS 1060: The Universe

To understand black holes and extreme gravity, we need help from Einstein and Hawking

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But first, what do you know about black holes and/or relativity?

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Reference Frames

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Special Relativity (postulates) 1) Physical laws same for all reference frames 2) Speed of light is always measured to be c

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Reference Frames

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Special Relativity (postulates) 1) Physical laws same for all reference frames 2) Speed of light is always measured to be c

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Time Dilation

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The passage of time is not the same everywhere!

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Muons created by cosmic rays colliding with the atmosphere exhibit time dilation

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Faster a muon is traveling, the slower time passes for it, so it survives longer before decaying

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Implications of Special Relativity

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E = mc2

when moving, have kinetic energy —> increase your mass!

Time passes more slowly for moving reference frames Length of moving

  • bjects contract in the

direction of motion Speed of Light is the universal speed limit (can only approach it)

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

General Relativity: analogous case for gravity

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General Relativity: analogous case for gravity

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Equivalence Principle

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Space-time is curved

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Gravitational Redshift

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

What are Black Holes?

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Particular solutions to Einstein’s equations of General Relativity Inevitable end-state of ultra-dense matter Inside the event horizon, the escape velocity is larger than the speed of light (c) Matter inside the event horizon must fall to the center, toward the singularity Black holes have “no hair” - defined only by their mass, charge, and spin (rotation) —> all other info about what formed it is lost

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

The black hole in Interstellar

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called Gargantua, b/c it’s supermassive (like the one in the centers of galaxies) keeps Matthew McConaughey from “spaghettification” as he crosses the event horizon —> stellar mass black holes have huuuuuge tidal forces here that would kill you!

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Black holes are not completely black after all

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Emit Hawking radiation Hawking himself popularized the explanation used in the textbook, but that explanation is wrong! The virtual “particles,” which have large quantum waveforms (uncertainty in their position is as large as the black hole), separate at a distance several times larger than the event horizon They result mainly from space-time changing dynamically when the black hole forms, creating thermal radiation Temperature is very tiny, but carries away energy, causing the black hole to lose mass (E=mc2), but it takes a looooong time (~1066 years)

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ASTR/PHYS 1060: The Universe Fall 2019: Chapter 13

Gravitational Waves: LIGO!

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Virgo facility near Pisa, Italy

  • ther detectors in Louisiana and

Washington state

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First 5 BH-BH mergers

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BHs and NSs with known masses

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Solar Masses

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First NS-NS merger, explosion also seen

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