Chapter 12: Evolution of Low Mass Stars Chapter 12 Reading - - PowerPoint PPT Presentation

▶
chapter 12 evolution of low mass stars
SMART_READER_LITE
LIVE PREVIEW

Chapter 12: Evolution of Low Mass Stars Chapter 12 Reading - - PowerPoint PPT Presentation

Jan 21, 2024 128 likes •549 views

Chapter 12: Evolution of Low Mass Stars Chapter 12 Reading Assignment due Wednesday at 10:45am Are your grades in Canvas correct??? In-class/HW Assignment due now! Midterms available up front Turn in extra credit planetarium reports up front

slide-1
SLIDE 1

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

Chapter 12: Evolution of Low Mass Stars

1

Chapter 12 Reading Assignment due Wednesday at 10:45am In-class/HW Assignment due now! Turn in extra credit planetarium reports up front (not “due” today, but please turn in this week if you went) Are your grades in Canvas correct??? Midterms available up front

slide-2
SLIDE 2

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

Stellar Properties

2

Age Color Luminosity Size Mass Temperature Spectral Type

Which of these is most important?

slide-3
SLIDE 3

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

Stellar Properties

3

Age Color Luminosity Size Mass Temperature Spectral Type

slide-4
SLIDE 4

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

Luminosity depends on mass

4

slide-5
SLIDE 5

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 5

High Mass Low Mass

slide-6
SLIDE 6

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

Why are fainter (and less massive) stars more common than brighter ones?

6

A) They live longer B) They form more frequently C) They aren’t more common, we just see them more easily

slide-7
SLIDE 7

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

The future of our Sun and the evolution of low-mass stars

7

slide-8
SLIDE 8

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 8

Protostars to Stars

slide-9
SLIDE 9

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

Chapter 12: Evolution of Low Mass Stars

9

Chapter 12 Reading Assignment due now! Turn in extra credit planetarium reports up front (not “due” today, but please turn in this week if you went) Are your grades in Canvas correct??? Midterms available up front

slide-10
SLIDE 10

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 10

9x106 1x109 4x1010 3x1011

slide-11
SLIDE 11

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 11

Main Sequence Power: Hydrogen Core Burning Temperature = 5800 K Luminosity = 1 LSun Lifetime = 10 billion years

slide-12
SLIDE 12

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 12

Red Giant Branch Power: Hydrogen Shell Burning Final Temperature = 3200 K Final Luminosity = 1000 LSun Lifetime = 200 million years

slide-13
SLIDE 13

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 13

Helium Burning or Horizontal Branch Power: Helium (into Carbon) Core Burning + Hydrogen shell burning Temperature = 4500 K Luminosity = 100 LSun Lifetime = 100 million years

slide-14
SLIDE 14

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 14

Asymptotic Giant Branch Power: Helium shell burning + Hydrogen shell burning Final Temperature = 3000 K Final Luminosity = 5000 LSun Lifetime = 1 million years

slide-15
SLIDE 15

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 15

Planetary Nebulae

  • uter atmosphere ejected by

radiation from the core

slide-16
SLIDE 16

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 16

White Dwarf Power: None Temperature = 15000 K Luminosity = 0.001 LSun Lifetime = 1 billion years (to cool down to ~7000 K)

slide-17
SLIDE 17

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

Chapter 12: Evolution of Low Mass Stars

17

Chapter 13 Reading Assignment due Monday, October 22nd Makeup in-class assignment from Wednesday online, due on Monday (for late credit) Are your grades in Canvas correct??? Midterms available up front Turn in extra credit planetarium reports up front (not “due” today, but please turn in this week if you went)

slide-18
SLIDE 18

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

Lifetime as a function of mass

18

slide-19
SLIDE 19

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 19

slide-20
SLIDE 20

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 20

slide-21
SLIDE 21

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 21

slide-22
SLIDE 22

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 22

slide-23
SLIDE 23

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 23

slide-24
SLIDE 24

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

Future Evolution

  • f the Sun

24

Again, this time with feeling!

slide-25
SLIDE 25

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 25

Size changes along with temperature

slide-26
SLIDE 26

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 26

The universe is about 13 billion years old. If I see a 0.7 solar mass star, what phase of evolution will it be in?

A) Main Sequence B) Red Giant Branch C) Helium Burning D) Asymptotic Giant Branch

slide-27
SLIDE 27

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 27

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.

slide-28
SLIDE 28

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 28

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

slide-29
SLIDE 29

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 29

Which of these star clusters is the oldest?

A B C

slide-30
SLIDE 30

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 30

Theory (red line) & Observations (white dots)

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

slide-31
SLIDE 31

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe 31

Which stars in this cluster are the most massive?

A B C D

slide-32
SLIDE 32

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

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

32

slide-33
SLIDE 33

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

What happens when close binary stars evolve?

33

What is this???

slide-34
SLIDE 34

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

What happens when close binary stars evolve?

34

slide-35
SLIDE 35

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

What happens when close binary stars evolve?

35

slide-36
SLIDE 36

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

What happens when close binary stars evolve?

36

slide-37
SLIDE 37

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

What happens when close binary stars evolve?

37

slide-38
SLIDE 38

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

What happens when close binary stars evolve?

38

A “nova” is what? A) Material from Star 2 hits the surface of the white dwarf, causing it to heat up B) Material from Star 2 accumulates on the surface until it’s hot enough to burn (fuse H -> He) C) Enough material falls on the white dwarf to cause the entire star to explode

slide-39
SLIDE 39

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

What happens when close binary stars evolve?

39

slide-40
SLIDE 40

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

What happens when close binary stars evolve?

40

slide-41
SLIDE 41

Fall 2018: Chapter 12 ASTR/PHYS 1060: The Universe

Type Ia Supernovae

41