chapter 12 evolution of low mass stars
play

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

Jan 21, 2024 •128 likes •548 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

  1. 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 (not “due” today, but please turn in this week if you went) ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 1

  2. Stellar Properties Age Color Luminosity Which of these is most Spectral Type important? Mass Temperature Size ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 2

  3. Stellar Properties Color Luminosity Mass Spectral Type Age Temperature Size ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 3

  4. Luminosity depends on mass ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 4

  5. Low High Mass Mass ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 5

  6. Why are fainter (and less massive) stars more common than brighter ones? A) They live longer B) They form more frequently C) They aren’t more common, we just see them more easily ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 6

  7. The future of our Sun and the evolution of low-mass stars ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 7

  8. Protostars to Stars ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 8

  9. Chapter 12: Evolution of Low Mass Stars Chapter 12 Reading Assignment due now! Are your grades in Canvas correct??? Turn in extra credit planetarium reports up Midterms available up front front (not “due” today, but please turn in this week if you went) ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 9

  10. 9x10 6 1x10 9 4x10 10 3x10 11 ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 10

  11. Main Sequence Power: Hydrogen Core Burning Temperature = 5800 K Luminosity = 1 L Sun Lifetime = 10 billion years ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 11

  12. Red Giant Branch Power: Hydrogen Shell Burning Final Temperature = 3200 K Final Luminosity = 1000 L Sun Lifetime = 200 million years ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 12

  13. Helium Burning or Horizontal Branch Power: Helium (into Carbon) Core Burning + Hydrogen shell burning Temperature = 4500 K Luminosity = 100 L Sun Lifetime = 100 million years ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 13

  14. Asymptotic Giant Branch Power: Helium shell burning + Hydrogen shell burning Final Temperature = 3000 K Final Luminosity = 5000 L Sun Lifetime = 1 million years ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 14

  15. Planetary Nebulae outer atmosphere ejected by radiation from the core ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 15

  16. White Dwarf Power: None Temperature = 15000 K Luminosity = 0.001 L Sun Lifetime = 1 billion years (to cool down to ~7000 K) ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 16

  17. Chapter 12: Evolution of Low Mass Stars Are your grades in Canvas correct??? Chapter 13 Reading Assignment due Monday, October 22nd Midterms available up front Makeup in-class assignment from Wednesday online, due on Monday (for Turn in extra credit planetarium reports late credit) up front (not “due” today, but please turn in this week if you went) ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 17

  18. Lifetime as a function of mass ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 18

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

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

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

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

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

  24. Future Evolution of the Sun Again, this time with feeling! ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 24

  25. Size changes along with temperature ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 25

  26. The universe is about 13 billion years old. If I see a 0.7 solar mass star, what phase of A) Main Sequence evolution will it be in? B) Red Giant Branch C) Helium Burning D) Asymptotic Giant Branch ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 26

  27. How do we know the different stages of a star's life? We obviously have not been observing stars for long enough to see it go through all the stages. ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 27

  28. Star Clusters: stars of many masses born at the same time ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 28

  29. Which of these star clusters is the oldest? A B C ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 29

  30. Theory (red line) & Observations (white dots) We can make a model of any star based on its mass and age ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 30

  31. D Which stars in C this cluster are the most B massive? A ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 31

  32. Because stars in clusters form at the same time, and a star’s evolution is determined primarily by its mass, we can observe many clusters and figure out how stars evolve ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 32

  33. What happens when close binary stars evolve? What is this??? ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 33

  34. What happens when close binary stars evolve? ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 34

  35. What happens when close binary stars evolve? ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 35

  36. What happens when close binary stars evolve? ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 36

  37. What happens when close binary stars evolve? ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 37

  38. What happens when close binary stars evolve? 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 ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 38

  39. What happens when close binary stars evolve? ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 39

  40. What happens when close binary stars evolve? ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 40

  41. Type Ia Supernovae ASTR/PHYS 1060: The Universe Fall 2018: Chapter 12 � 41

Download Presentation
Download Policy: The content available on the website is offered to you 'AS IS' for your personal information and use only. It cannot be commercialized, licensed, or distributed on other websites without prior consent from the author. To download a presentation, simply click this link. If you encounter any difficulties during the download process, it's possible that the publisher has removed the file from their server.

Recommend

Stellar Evolution: Low Mass Stars Mass 2-3 M sun But what about High Mass Stars and all of

Stellar Evolution: Low Mass Stars Mass 2-3 M sun But what about High Mass Stars and all of

Stellar Evolution: Low Mass Stars Mass 2-3 M sun But what about High Mass Stars and all of those other elements??? GRAVITY When core T=10 8 K, He fuses into C (& O) What happens when the Helium runs out?? PRESSURE Answer

726 views • 38 slides
Chapter 12: Evolution of Low Mass Stars Are your grades in Canvas correct??? Chapter 12 Reading

Chapter 12: Evolution of Low Mass Stars Are your grades in Canvas correct??? Chapter 12 Reading

Chapter 12: Evolution of Low Mass Stars Are your grades in Canvas correct??? Chapter 12 Reading Assignment due now Midterms available up front In-class/HW Assignment due now! Turn in extra credit planetarium/observing reports up front (no due

636 views • 40 slides
Chapter 20 Stellar Evolution Part 2. Secs. 20.4, 20.5 20.4 Evolution of Stars More Massive than

Chapter 20 Stellar Evolution Part 2. Secs. 20.4, 20.5 20.4 Evolution of Stars More Massive than

Chapter 20 Stellar Evolution Part 2. Secs. 20.4, 20.5 20.4 Evolution of Stars More Massive than the Sun It can be seen from this H-R diagram that stars more massive than the Sun follow very different paths when leaving the Main Sequence,

741 views • 15 slides
Massive Stars Mass Loss Mathieu Renzo Advisors: S. N. Shore, C. D. Ott 1 / 12 Mass Loss - Why

Massive Stars Mass Loss Mathieu Renzo Advisors: S. N. Shore, C. D. Ott 1 / 12 Mass Loss - Why

PhD Recruitment, February 12, API/GRAPPA Massive Stars Mass Loss Mathieu Renzo Advisors: S. N. Shore, C. D. Ott 1 / 12 Mass Loss - Why is it important ... ... for the environment of the stars? Chemical and dynamical evolution of Galaxies

305 views • 13 slides
Evolution of gas and dust in AGB stars Kay Justtanont Chalmers University of Technology Stellar

Evolution of gas and dust in AGB stars Kay Justtanont Chalmers University of Technology Stellar

Evolution of gas and dust in AGB stars Kay Justtanont Chalmers University of Technology Stellar evolution For low- and intermediate-mass stars, they enter the red giant and subsequently, asymptotic giant branch (AGB) phases. During the

713 views • 39 slides
Chapter 13: High Mass Star Evolution and their Remnants: NSs and BHs Chapter 13 Reading

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

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

820 views • 79 slides
Systematic Study of Mass Loss in the Evolution of Massive Stars Mathieu Renzo advisors: Prof.

Systematic Study of Mass Loss in the Evolution of Massive Stars Mathieu Renzo advisors: Prof.

Tesi di Laurea Magistrale Universit` a di Pisa - Dipartimento di Fisica 03/06/2015 Systematic Study of Mass Loss in the Evolution of Massive Stars Mathieu Renzo advisors: Prof. S. N. Shore, Prof. C. D. Ott 1 / 27 Outline Introduction

690 views • 47 slides
Evolutions of stars just below the critical mass for iron core formation Koh Takahashi, Hideyuki

Evolutions of stars just below the critical mass for iron core formation Koh Takahashi, Hideyuki

Evolutions of stars just below the critical mass for iron core formation Koh Takahashi, Hideyuki Umeda, & Takashi Yoshida Department of Astronomy, University of Tokyo 9-11Mo Introduction 9-11Mo stars evolution

312 views • 18 slides
Chapter 17 17.1 Lives in the Balance Star Stuff Our goals for learning How does a

Chapter 17 17.1 Lives in the Balance Star Stuff Our goals for learning How does a

Chapter 17 17.1 Lives in the Balance Star Stuff Our goals for learning How does a stars mass affect nuclear fusion? How does a stars mass affect Stellar Mass and Fusion nuclear fusion? The mass of a main sequence star

368 views • 11 slides
Chapter 17 Star Stuff 17.1 Lives in the Balance Our goals for learning How does a

Chapter 17 Star Stuff 17.1 Lives in the Balance Our goals for learning How does a

Chapter 17 Star Stuff 17.1 Lives in the Balance Our goals for learning How does a stars mass affect nuclear fusion? How does a stars mass affect nuclear fusion? Stellar Mass and Fusion The mass of a main sequence star

872 views • 62 slides
Life and death of stars CAPAS James Lequeux, 30 septembre 2012 Evolution of binary massive stars

Life and death of stars CAPAS James Lequeux, 30 septembre 2012 Evolution of binary massive stars

Life and death of stars CAPAS James Lequeux, 30 septembre 2012 Evolution of binary massive stars Stellar evolution in the HR diagram HR diagram (Hipparcos) Massive stars are very rare No O-B star within 50 pc Closest O stars

416 views • 16 slides
Chapter 22 Neutron Stars and Black Holes Units of Chapter 22 22.1 Neutron Stars 22.2 Pulsars

Chapter 22 Neutron Stars and Black Holes Units of Chapter 22 22.1 Neutron Stars 22.2 Pulsars

Chapter 22 Neutron Stars and Black Holes Units of Chapter 22 22.1 Neutron Stars 22.2 Pulsars 22.3 XXNeutron-Star Binaries: X-ray bursters [Look at the slides and the pictures in your book, but I wont test you on this in detail, and we

433 views • 31 slides
Neutron Stars Chandrasekhar limit on white dwarf mass Supernova explosions

Neutron Stars Chandrasekhar limit on white dwarf mass Supernova explosions

Neutron Stars Chandrasekhar limit on white dwarf mass Supernova explosions Formation of elements (R, S process) Neutron stars Pulsars Formation of X-Ray binaries High-mass Low-mass Maximum white dwarf mass

275 views • 24 slides
Types of Stars Part 2 Tikhonov Dmitry AS-46i Double Star Consists of 2 stars that rotate their

Types of Stars Part 2 Tikhonov Dmitry AS-46i Double Star Consists of 2 stars that rotate their

Types of Stars Part 2 Tikhonov Dmitry AS-46i Double Star Consists of 2 stars that rotate their common center of mass. Black Hole They have very high density and even light cant escape. Their mass cane be equal 1 billion of solar

393 views • 6 slides
Massive Stars Mass Loss Mathieu Renzo Advisors: S. N. Shore, C. D. Ott 1 / 8 Mass Loss - Why is

Massive Stars Mass Loss Mathieu Renzo Advisors: S. N. Shore, C. D. Ott 1 / 8 Mass Loss - Why is

TASC 2014, November 7, UCSD Massive Stars Mass Loss Mathieu Renzo Advisors: S. N. Shore, C. D. Ott 1 / 8 Mass Loss - Why is it important ... ... for the stellar structure? ... for the environment? Evolutionary timescale chemical and

653 views • 8 slides
Chapter: 14 14 14 14 Chapter: Chapter: Chapter: LTE radio access: LTE radio access: An

Chapter: 14 14 14 14 Chapter: Chapter: Chapter: LTE radio access: LTE radio access: An

3G Evolution 3G Evolution 3G Evolution 3G Evolution Chapter: 14 14 14 14 Chapter: Chapter: Chapter: LTE radio access: LTE radio access: An overview Deepak Dasalukunte Department of Electrical and Information Technology 29-Apr-2009 3G

262 views • 11 slides
Generalization via Modularity Deepak Chris Trevor Phillip Alyosha Pathak* Lu* Darrell

Generalization via Modularity Deepak Chris Trevor Phillip Alyosha Pathak* Lu* Darrell

Learning to Control Self-Assembling Morphologies Generalization via Modularity Deepak Chris Trevor Phillip Alyosha Pathak* Lu* Darrell Isola Efros * equal contribution NeurIPS 2019 How do we train a robot? Multiple tasks

685 views • 49 slides
Techniques for Evolution-Aware Runtime Verification Owolabi Legunsen, Yi Zhang, Milica

Techniques for Evolution-Aware Runtime Verification Owolabi Legunsen, Yi Zhang, Milica

Techniques for Evolution-Aware Runtime Verification Owolabi Legunsen, Yi Zhang, Milica Hadi-Tanovi, Grigore Rou, Darko Marinov ICST 2019 4/26/2019 CCF-1421503, CCF-1421575, CCF-1763788, CNS-1619275, CNS-1646305, CNS-1740916 Runtime

448 views • 30 slides
Evolution to 5G: An operator's perspective Dr. Ivo Maljevic TELUS team IEEE 5G Summit | Nov

Evolution to 5G: An operator's perspective Dr. Ivo Maljevic TELUS team IEEE 5G Summit | Nov

Evolution to 5G: An operator's perspective Dr. Ivo Maljevic TELUS team IEEE 5G Summit | Nov 2015 2 Cellular Standards Evolution ? 1980 1G 1990 2G 2000 3G 2010 - 4G 2020 5G Analog systems Digital

225 views • 11 slides
The 5G Evolution:

The 5G Evolution:

The 5G Evolution:

512 views • 14 slides
Authenticated Encryption Requirements David McGrew mcgrew@cisco.com Directions in Authenticated

Authenticated Encryption Requirements David McGrew mcgrew@cisco.com Directions in Authenticated

Desiderata Current AEAD use Evolution Conclusions Authenticated Encryption Requirements David McGrew mcgrew@cisco.com Directions in Authenticated Ciphers, 2012 Desiderata Current AEAD use Evolution Conclusions Many desirable attributes

284 views • 26 slides
The Evolution of Microservices Adrian Cockcroft @adrianco Technology Fellow - Battery Ventures

The Evolution of Microservices Adrian Cockcroft @adrianco Technology Fellow - Battery Ventures

The Evolution of Microservices Adrian Cockcroft @adrianco Technology Fellow - Battery Ventures June 2016 What does @adrianco do? Maintain Relationship with Presentations at Technology Due Cloud Vendors Conferences Diligence on Deals

1.15k views • 66 slides
Evolution of Connections in SHRUTI Networks Joe Townsend, Ed Keedwell and Antony Galton

Evolution of Connections in SHRUTI Networks Joe Townsend, Ed Keedwell and Antony Galton

Evolution of Connections in SHRUTI Networks Joe Townsend, Ed Keedwell and Antony Galton Motivation Neural-Symbolic Reasoning: Adaptable representations of logic programs in neural networks. Can help us understand how reasoning might be

1.05k views • 40 slides
Large-scale Cancer Genomics Data Analysis David Haussler Center for Biomolecular Science and

Large-scale Cancer Genomics Data Analysis David Haussler Center for Biomolecular Science and

Large-scale Cancer Genomics Data Analysis David Haussler Center for Biomolecular Science and Engineering, UC Santa Cruz Cancer Genomics Hub Being built to store BAM & VCF for TCGA, TARGET and CGAP/CGCI projects Designed for 25,000

413 views • 29 slides

More recommend