Warm-up on board. Sketch problem 1 from the HW. Which star: i) Is largest? Is second smallest? Could be the same size as D? Bright A.

Similar documents
Agenda for Ast 309N, Sep. 27. Measuring Masses from Binary Stars

Stellar Evolution. The lives of low-mass stars. And the lives of massive stars

Lecture 24: Testing Stellar Evolution Readings: 20-6, 21-3, 21-4

17.1 Lives in the Balance. Our goals for learning: How does a star's mass affect nuclear fusion?

Announcement: Quiz Friday, Oct 31

Late Stages of Stellar Evolution. Late Stages of Stellar Evolution

Astronomy 210. Outline. Stellar Properties. The Mosquito Dilemma. Solar Observing & HW9 due April 15 th Stardial 2 is available.

Stars and their properties: (Chapters 11 and 12)

Why Do Stars Leave the Main Sequence? Running out of fuel

Birth & Death of Stars

Review Questions for the new topics that will be on the Final Exam

A1101, Lab 8: Distances and Ages of Star Clusters Lab Worksheet

Phys 100 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 9

Lecture 16: The life of a low-mass star. Astronomy 111 Monday October 23, 2017

AST 101 Introduction to Astronomy: Stars & Galaxies

Lecture 21 Formation of Stars November 15, 2017

Age of M13: 14 billion years. Mass of stars leaving the main-sequence ~0.8 solar masses

20. Stellar Death. Interior of Old Low-Mass AGB Stars

Filling the intellectual Vacuum: Energy Production. Contenders: From early 1920s: probably fusion, but how?

The life of a low-mass star. Astronomy 111

Star Clusters. stars are usually near other stars - CLUSTER

8.8A describe components of the universe, including stars, nebulae, galaxies and use models such as HR diagrams for classification

Lecture 33: The Lives of Stars

Evolution of Stars Population III: Population II: Population I:

Stellar Midlife. A. Main Sequence Lifetimes. (1b) Lifetime of Sun. Stellar Evolution Part II. A. Main Sequence Lifetimes. B. Giants and Supergiants

Lifespan on the main sequence. Lecture 9: Post-main sequence evolution of stars. Evolution on the main sequence. Evolution after the main sequence

Chapter 12 Stellar Evolution

Low-mass Stellar Evolution

Chapter 17: Stellar Evolution

Chapter 20 Stellar Evolution Part 2. Secs. 20.4, 20.5

Heading for death. q q

Astro 21 first lecture. stars are born but also helps us study how. Density increases in the center of the star. The core does change from hydrogen to

Stellar Evolution Notes

Before proceeding to Chapter 20 More on Cluster H-R diagrams: The key to the chronology of our Galaxy Below are two important HR diagrams:

Notepack 23 12/19/2014 Stellar Evolution: Aim: The Life Cycle of a Star

The Sun - Size and Mass. Masses. Note: Most of solar system mass is in. Radii } } Densities

Last time: looked at proton-proton chain to convert Hydrogen into Helium, releases energy.

AST 101 Introduction to Astronomy: Stars & Galaxies

Astronomy 1504 Section 002 Astronomy 1514 Section 10 Midterm 2, Version 1 October 19, 2012

TA feedback forms are online!

Chapter 17 Lecture. The Cosmic Perspective Seventh Edition. Star Stuff Pearson Education, Inc.

Stellar Evolution and the HertzsprungRussell Diagram 7/14/09. Astronomy 101

Exam # 3 Tue 12/06/2011 Astronomy 100/190Y Exploring the Universe Fall 11 Instructor: Daniela Calzetti

Chapter 12 Review. 2) About 90% of the star's total life is spent on the main sequence. 2)

Stars. The composition of the star It s temperature It s lifespan

Today. Stars. Properties (Recap) Binaries. Stellar Lifetimes

the nature of the universe, galaxies, and stars can be determined by observations over time by using telescopes

Chapters 12 and 13 Review: The Life Cycle and Death of Stars. How are stars born, and how do they die? 4/1/2009 Habbal Astro Lecture 27 1

ASTRONOMY 1 EXAM 3 a Name

SEQUENCING THE STARS

OPEN CLUSTERS LAB. I. Introduction: II. HR Diagram NAME:

Chapter 12 Stellar Evolution

NSB ideas on Hertzsprung-Russell diagram

Chapter 9: Measuring the Stars

3/1/18. Things to do. Topics for Today

Stellar Astronomy Sample Questions for Exam 4

Lecture 16: Evolution of Low-Mass Stars Readings: 21-1, 21-2, 22-1, 22-3 and 22-4

Lecture 24. Reprise: Evolution Timescale

Chapter 15 Surveying the Stars Pearson Education, Inc.

The Distances and Ages of Star Clusters

The physics of stars. A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure.

Stellar Evolution. Eta Carinae

Star Formation. gas cloud protostar Star equilibrium PHYS 162 1

HR Diagram, Star Clusters, and Stellar Evolution

Today. When does a star leave the main sequence?

AST 101 Introduction to Astronomy: Stars & Galaxies

Brought to you in glorious, gaseous fusion-surround. Intro to Stars Star Lives 1

Chapter 12: The Life Cycle of Stars (contʼd) How are stars born, and how do they die? 4/9/09 Habbal Astro Lecture 25 1

The Local Group of Galaxies

L = 4 d 2 B p. 4. Which of the letters at right corresponds roughly to where one would find a red giant star on the Hertzsprung-Russell diagram?

L = 4 d 2 B p. 1. Which outer layer of the Sun has the highest temperature? A) Photosphere B) Corona C) Chromosphere D) Exosphere E) Thermosphere

OPEN CLUSTER PRELAB The first place to look for answers is in the lab script!

AST101 Lecture 13. The Lives of the Stars

Life and Death of a Star. Chapters 20 and 21

Chapter 19: The Evolution of Stars

CONTENT EXPECTATIONS

Guiding Questions. The Deaths of Stars. Pathways of Stellar Evolution GOOD TO KNOW. Low-mass stars go through two distinct red-giant stages

The Deaths of Stars 1

Astronomy 104: Second Exam

Chapter 15: Surveying the Stars

Fusion in first few minutes after Big Bang form lightest elements

Stellar Evolution: The Deaths of Stars. Guiding Questions. Pathways of Stellar Evolution. Chapter Twenty-Two

The structure and evolution of stars

Announcements. L! m 3.5 BRIGHT FAINT. Mass Luminosity Relation: Why? Homework#3 will be handed out at the end of this lecture.

ASTR Look over Chapter 15. Good things to Know. Triangulation

Guiding Questions. The Deaths of Stars. Pathways of Stellar Evolution GOOD TO KNOW. Low-mass stars go through two distinct red-giant stages

The Evolution of Low Mass Stars

Astronomy Ch. 20 Stellar Evolution. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

Astronomy Ch. 20 Stellar Evolution. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

Quiz Question: Binary Stars

Stellar energy generation on the main sequence

Protostars on the HR Diagram. Lifetimes of Stars. Lifetimes of Stars: Example. Pressure-Temperature Thermostat. Hydrostatic Equilibrium

1. Basic Properties of Stars

Stars & Galaxies. Chapter 27, Section 1. Composition & Temperature. Chapter 27 Modern Earth Science Characteristics of Stars

The distance modulus in the presence of absorption is given by

The Cosmic Perspective. Surveying the Properties of Stars. Surveying the Stars. How do we measure stellar luminosities?

Astronomy 122 Midterm

Astronomy. Stellar Evolution

The dying sun/ creation of elements

The Later Evolution of Low Mass Stars (< 8 solar masses)

Transcription:

Warm-up on board Sketch problem 1 from the HW. Bright A C Which star: L D i) Is largest? ii) iii) Is second smallest? Could be the same size as D? Dim Hot B T = Main Sequence E Cool

Why are stars seen in clusters? What makes up a stellar population? Open Star Clusters M35 and NGC 2158 Credit & Copyright: Canada-France-Hawaii Telescope, J.-C. Cuillandre (CFHT), Coelum

Goals from Last Time 1) predict trends in stellar radius with L and T in the HR diagram on and off the Main Sequence 2) Recognize how apparent vs. intrinsic brightness creates selection bias we must remove to decide whether the Sun is typical.

Think-Pair-Share Both surveys searched for all stars within 10 pc. Which survey can see stars with fainter apparent brightness? A peak at 12 B peak at 14 www.oglethorpe.edu/faculty/~m_rulison/ C: They have the same apparent brightness limit. (Notice that the Sun is not typical in luminosity in fact, there is no typical luminosity.)

Goals for Today 1) Recognize clusters as stars born together; relate the origin and age of field stars to open and bound cluster stars. 2) Identify star classes/evolutionary stages within HR diagrams, relating each to its source of energy. 3) Compare the evolutionary paths of high vs. low mass stars. 4) Know which types of stars follow a standard M-L relation, and use it to prove that massive Main Sequence stars live faster and die younger. 5) Analyze cluster HR diagrams in relation to either general field or other cluster HR diagrams to compare ages. 6) Explain why stellar populations may have different colors and metallicities.

Clusters of stars are born together Globular clusters are bound for life. Open clusters come unbound as they age and blow away their leftover gas. Their stars disperse to become field stars.

Think-Pair-Share luminosity temperature This diagram shows: A) stars born together in a bound cluster B) stars born together in an open cluster C) stars born in several open clusters, each of which produced stars born together at a distinct time

The Hertzsprung Russell diagram luminosity temperature This schematic HR diagram shows a snapshot of a stellar population with stars at all stages of evolution

Red giants, white dwarfs, and planetary nebulae (not planets!) http://en.wikipedia.org/wiki/ngc_2371-2

Fusion Reactions change with temperature and as raw materials run out in the core MINIMUM TEMP. 8 x 10 6 K 20 x 10 6 K 100 x 10 6 K 600 x 10 6 K 10 9 K REACTION proton-proton chain CNO cycle (H fusion) triple alpha (He fusion) carbon-helium fusion carbon burning What fuses on the horizontal branch? A) H in the core B) He in the core C) H in a shell D) He in a shell Massive/hot stars make the heaviest elements stardust! ( metals )

Masses along the Main Sequence Normal hydrogen-burning stars (=Main Sequence stars) follow a mass-luminosity relation L~M 3.5 (Is the Sun on it?) Q: How do we know L~M 3.5? A: orbital motions trace mass

Lifetimes along the Main Sequence L = km 3.5 f conv = % of Mass converted to energy by fusion (E=f conv Mc 2 ) star s lifetime τ=e/l τ = f conv Mc 2 /(km 3.5 ) measured approximate to be constant by definition of lifetime algebra τ 1/M 2.5 massive stars live fast and die young

Evolutionary paths for high & low mass stars When high mass stars explode, stardust disperses

Think-Pair-Share Which star: i) Will live longest (where live = fuse)? ii) Bright Will live longest Dim (where live = not Hot T Cool change form)? L A B = Main Sequence C D E

stars are born in gas polluted with the stardust of earlier generations of stars A B Label A & B: which was born first? which is bluer? which has higher metallicity? which might be seen in a globular cluster?

Think-Pair-Share In the main sequence for clusters, massive stars are often missing why? Real cluster M55 Which cluster is oldest? A B A) They die without leaving a remnant B) They die earlier than other stars C) There aren t as many of them in the population C

Think-Pair-Share Which statement is true? A) If these are both open clusters, M67 probably formed earlier B) If these are both open clusters, M67 probably has more white dwarfs C)If these are both open clusters, M67 is probably bluer

Think-Pair-Share Which statement is true? A) massive stars produce more heavy elements by fusion, so have higher metallicity B) the metals in the cores of old stars were produced mainly by earlier generations of stars C) the photospheres of young stars reveal lines that come from mainly from elements made by earlier generations of stars