The HR Diagram: A Laboratory Exercise
|
|
|
- Ann Briggs
- 5 years ago
- Views:
Transcription
1 Pisgah Astronomical Research Institute 2009 The HR Diagram: A Laboratory Exercise The HR Diagram Lab gives students the opportunity to construct an HR Diagram based on their own classifications of 119 stars. This lab has four documents: A document with a list of 119 stars with spectral classifications A document with a list of 119 stars without spectral classifications A blank graph page to plot the HR Diagram A document with spectral types and absolute magnitudes of standard stars A document with complete catalog information on the 119 stars
2 I. THE SPECTRA OF STARS: TEACHER COPY Table 1 lists over 100 stars that can be observed with SCOPE and classified. Log into SCOPE and select the plate listed in column 1 of the table. Then, pick one of the stars. Note the name of star, and locate it in Table 1, where you will record your classification of the star. Complete as many of the stars as you can. Once you re done classifying as many stars as you can, let s find out how many stars of each spectral type you ve classified. Fill in the table below. Spectral Type Number of Stars O B A F G K M 0 (0%) 38 (33%) 29 (25%) 12 (10%) 15 (14%) 15 (13%) 6 (5%) Question: What is going on? Are there equal numbers of each spectral type? To answer this question, let s build a Hertzsprung-Russsell Diagram. Table 1. Stars to Classify from Their Spectra as observed with SCOPE Catalog Spectral Type Vela BC HD B1/B2 I HD B8/B9V HD K2 HD B0.5III HD B9V HD B5V HD A3 HD G0 HD73367 F0 1 of 8
3 I. THE SPECTRA OF STARS: TEACHER COPY Catalog Spectral Type HD B5 HD A0 HD Ma HD K3III HD K2III V* T Vel G0II HD A6V HD K5 HD B9I HD B3IV HD F8 HD72939 B5 HD A2 HD72286 A0 HD72975 F2 HD G0 2 of 8
4 I. THE SPECTRA OF STARS: TEACHER COPY Catalog Spectral Type HD B2.5V Vela AL HD B8 HD B8III HD71787 B9IV CD B2IVe HD B7IV HD71743 B9 HD B5IV HD72351 A0 HD B8 HD B8/B9V HD G8/K0III HD B9 HD B8V HD B6V HD F2V 3 of 8
5 I. THE SPECTRA OF STARS: TEACHER COPY Catalog Spectral Type HD B9 HD71237 B9 HD71125 A8/A9V Vela MA HD B9V HD G0V HD B6V HD B8IV HD K1III HD A5V HD F5 HD B9 HD G0 HD Ap... HD70142 A7V V* IT Vel B7III HD70766 B9 4 of 8
6 I. THE SPECTRA OF STARS: TEACHER COPY Catalog Spectral Type HD K1/K2III HD A0 CD A2 HD G5 HD G8III HD G5 HD B9 HD K0 HD A4IV Vela SK HD68805 B8 V* Al Vel 1.64 A3IV HD68322 B8 HD A0 HD G5 HD69130a 5.92 F2 HD B3V 5 of 8
7 I. THE SPECTRA OF STARS: TEACHER COPY Catalog Spectral Type HD A3IV V* AH Vel F7p HD68555 B8 V* BN Vel M HD K2 HD A2 HD68187 M3III HD B9 HD B8 Hydra-2 BC HD K0III HD F0 HD A3V HD F5 HD K0III HD K0III HD A6V 6 of 8
8 I. THE SPECTRA OF STARS: TEACHER COPY Catalog Spectral Type HD G3/G5V HD A1m... HD97444 K0 HD A0 HD M2III Hydra-2 AL HD96745 F0 HD A0/A1V HD G8III/IV HD B9V HD Ma HD A1V Hydra-2 MA HD F6V HD G1V HD F2/F3V HD K0/K1III HD K0 7 of 8
9 I. THE SPECTRA OF STARS: TEACHER COPY Catalog Spectral Type HD A2 / A6-A9 Hydra-2 SK HD A2/A3 II/III HD95190** 2.07 A5V HD G3V HD M7/8III HD95194 A0 HD K0III HD G0V HD95315 G5 HD95158 A5 HD A5V ** HD95190 is actually HD of 8
10 I. THE SPECTRA OF STARS Table 1 lists over 100 stars that can be observed with SCOPE and classified. Log into SCOPE and select the plate listed in column 1 of the table. Then, pick one of the stars. Note the name of star, and locate it in Table 1, where you will record your classification of the star. Complete as many of the stars as you can. Once you re done classifying as many stars as you can, let s find out how many stars of each spectral type you ve classified. Fill in the table below. Spectral Type Number of Stars O B A F G K M Question: What is going on? Are there equal numbers of each spectral type? To answer this question, let s build a Hertzsprung-Russsell Diagram. Table 1. Stars to Classify from Their Spectra as observed with SCOPE Vela BC HD HD HD HD HD HD HD HD HD of 8
11 I. THE SPECTRA OF STARS HD HD HD HD HD V* T Vel HD HD HD HD HD HD72939 HD HD72286 HD72975 HD of 8
12 I. THE SPECTRA OF STARS HD Vela AL HD HD HD71787 CD HD HD71743 HD HD72351 HD HD HD HD HD HD HD of 8
13 I. THE SPECTRA OF STARS HD HD71237 HD71125 Vela MA HD HD HD HD HD HD HD HD HD HD HD70142 V* IT Vel HD of 8
14 I. THE SPECTRA OF STARS HD HD CD HD HD HD HD HD HD Vela SK HD68805 V* Al Vel 1.64 HD68322 HD HD HD69130a 5.92 HD of 8
15 I. THE SPECTRA OF STARS HD V* AH Vel HD68555 V* BN Vel HD HD HD68187 HD HD Hydra-2 BC HD HD HD HD HD HD HD of 8
16 I. THE SPECTRA OF STARS HD HD HD97444 HD HD Hydra-2 AL HD96745 HD HD HD HD HD Hydra-2 MA HD HD HD HD HD of 8
17 I. THE SPECTRA OF STARS HD Hydra-2 SK HD HD95190** 2.07 HD HD HD95194 HD HD HD95315 HD95158 HD ** HD95190 is actually HD of 8
18 II. THE HERTZSPRUNG RUSSELL DIAGRAM Once you have completed the classification of stars you observed with SCOPE, you can explore the natures of the stars by plotting the stars on the Hertzsprung Russell (HR) Diagram. You noticed that there is a larger number of G, K, and M stars, than O, B, and F. Table 1 lists the Absolute Magnitudes (M V ) of the stars. Use those magnitudes and your classifications to plot on the graph below the Spectral Type versus the Absolute Magnitude. You will begin to notice the same thing astronomers notice stars are not random, but are located in specific areas of the graph. What produces this trend? The answer gives us important clues to the masses, energies, and life cycles of stars.
19 III. The Nature of Stars. Star Spectral Type Absolute Magnitude Temperature (K) Luminosity (x Sun) Mass (x Sun) Sun G2V 4.8 6, Vega A0V 0.6 9, Altair A7V 2.3 8, Sirius A1V 1.4 9, Arcturus K2III , Capella G , Procyon F5V 2.6 6, Aldeberan K5III , Spica B1V ,000 1, Castor A , Antares M1 I ,000 31, Plot the stars listed above on your HR Diagram. Look at the masses, temperatures, and luminosities. What trend do you notice in each of these stellar properties as a function of spectral type? Now, go back to the stars you classified. How many are more massive than the Sun? How many are less massive? In the same way, compare the luminosities and temperatures of your stars to the Sun. Summary: You cam determine the basic properties of stars simply by looking at their spectra! Spectroscopy is an extremely powerful tool for astronomers.
20 COMPLETE STAR CATALOG Star _r _RAJ2000 _DEJ2000 RAJ2000DEJ2000 Plx e_ pmra pmde Bmag Vmag SpType TYC1 TYC2 TYC3 (B-V) Distance Mv 1 arcsec "h:m:s" "d:m:s" deg deg mas mas mas/yr mas/yr mag mag Parsecs 2 HD B1/B2Ib HD B8/B9V HD K HD B0.5III HD B9V HD B5V HD A HD G HD F HD B HD A HD Ma HD K3III HD K2III V* T Vel G0II HD A6V HD K HD B9Iab: HD B3IV HD F HD B HD A HD A HD F HD G HD B2.5V HD B HD B8III HD B9IV CD HD B7IV HD B HD B5IV HD A HD B HD B8/B9V HD G8/K0III HD B HD B8V HD B6V HD F2V HD B of 3
21 Star _r _RAJ2000 _DEJ2000 RAJ2000DEJ2000 Plx e_ pmra pmde Bmag Vmag SpType TYC1 TYC2 TYC3 (B-V) Distance Mv 1 arcsec "h:m:s" "d:m:s" deg deg mas mas mas/yr mas/yr mag mag Parsecs 2 HD B HD HD B9V HD HD B6V HD B8IV HD K1III HD A5V HD F HD B HD G HD Ap HD V* IT Vel B7III HD B HD HD A CD HD G HD G8III HD G HD B HD K HD A4IV HD B V* Al Vel F2pvar HD B HD A HD G HD69130a HD B3Vnne HD V* AH Vel F7p HD B V* BN Vel Mb HD K HD A HD HD B HD B HD K0III HD F HD A3V HD F of 3
22 Star _r _RAJ2000 _DEJ2000 RAJ2000DEJ2000 Plx e_ pmra pmde Bmag Vmag SpType TYC1 TYC2 TYC3 (B-V) Distance Mv 1 arcsec "h:m:s" "d:m:s" deg deg mas mas mas/yr mas/yr mag mag Parsecs 2 HD K0III HD K0III HD A6V HD G3/G5V HD A1m HD K HD A HD M2III HD F HD A0/A1V HD G8III/IV HD B9V HD Ma HD A1V HD F6V HD G1V HD F2/F3V HD K0/K1III HD K HD A2mA6-A HD A2/A3II/III HD A5V HD G3V HD M7/8III HD A HD K0III HD G0V HD G HD A HD A5V of 3
Astron 104 Laboratory #8 The H-R Diagram
Name: Date: Section: Astron 104 Laboratory #8 The H-R Diagram Section 10.1, 10.5 Introduction The Hertzsprung-Russell diagram, or H-R diagram for short, relates two fundamental properties of stars and
Lab 8: Stellar Classification and the H-R Diagram
Name: Section: Date: Lab 8: Stellar Classification and the H-R Diagram 1 Introduction Stellar Classification As early as the beginning of the 19th century, scientists have studied absorption spectra in
Astron 104 Laboratory #9 The H-R Diagram
Name: Date: Section: Astron 104 Laboratory #9 The H-R Diagram Section 10.1, 10.5 If we know the temperature of a star (or its Spectral Type) and the stars intrinsic brightness (or luminosity), a great
Stellar Spectrum Classification Lab Activity
Stellar Spectrum Classification Lab Activity Directions In this exercise you will be given a table of the standard spectral classes and a number of sample spectra to be used as the accepted spectra. While
HOMEWORK - Chapter 17 The Stars
Astronomy 20 HOMEWORK - Chapter 7 The Stars Use a calculator whenever necessary. For full credit, always show your work and explain how you got your answer in full, complete sentences on a separate sheet
The Hertzprung-Russell (HR) Diagram
Name: Partner(s): 1102 or 3311: Desk # Date: The Hertzprung-Russell (HR) Diagram Purpose Reproduce Hertzsprung s and Russell s simultaneous discovery Investigate the relationships between luminosity, mass,
How can we use an H-R diagram to know where a star is in its life cycle?
How can we use an H-R diagram to know where a star is in its life cycle? Just like humans, stars go through a life cycle. Over the course of their lives, stars change in ways that make each stage different
H-R Diagram Lab. Vocabulary:
H-R Diagram Lab Vocabulary: luminosity: brightness dependent on a star s size; temperature and distance spectral class: classification of stars by their spectrum and luminosity magnitude: measure of the
Spectral Classification of Stars
Department of Physics and Geology Spectral Classification of Stars Astronomy 1402 Part 1: Background Spectral Classification of Stars 1.1 Spectral Types: O, B, A, F, G, K, M On a dark, clear night far
The Hertzsprung - Russell Diagram Laboratory 11
The Hertzsprung - Russell Diagram Laboratory 11 Objective: In this laboratory a random sample of stars will be used to create a HR Diagram. From the diagram it will be determined which category certain
PH104 Lab 5 Stellar Classification Pre-Lab
Name: Lab Time: 1 PH104 Lab 5 Stellar Classification Pre-Lab 5.1 Goals This is a series of labs designed to help is in understanding the nature and lives of stars. There are 3 total labs in this sequence.
Lecture 10: The Hertzsprung-Russell Diagram Reading: Sections
Lecture 10: The Hertzsprung-Russell Diagram Reading: Sections 19.7-19.8 Key Ideas The Hertzsprung-Russell (H-R) Diagram Plot of Luminosity vs. Temperature for stars Features: Main Sequence Giant & Supergiant
My God, it s full of stars! AST 248
My God, it s full of stars! AST 248 N * The number of stars in the Galaxy N = N * f s f p n h f l f i f c L/T The Galaxy M31, the Andromeda Galaxy 2 million light years from Earth The Shape of the Galaxy
Each star is born with a specific mass. This mass is the main factor in determining the star s brightness, temperature, expected lifetime, type of
Each star is born with a specific mass. This mass is the main factor in determining the star s brightness, temperature, expected lifetime, type of death, and spectra. Stars are classified according to
StarTalk. Sanjay Yengul May "To know ourselves, we must know the stars."
StarTalk Sanjay Yengul May 2016 "To know ourselves, we must know the stars." Twinkle Twinkle How many stars are there? How big are these stars? Picture of night sky What are they made of? Why do they shine?
HR Diagram Lab. Area 1 Area 4. Area 5. Area 2. Area 6 Area 3
Name / 65 pts HR Diagram Lab Introduction Some of the greatest advances concerning the nature of stars have come about by comparing their properties using graphs. In the early 1900 s, while studying the
Daily Science 04/04/2017
Daily Science 04/04/2017 Which statement best describes the difference between type A stars and type B stars as shown in the diagram? a. Type A stars burn for a shorter amount of time than type B stars.
Exploratorium Teacher Institute page 1 Linda S. Shore
Exploratorium Teacher Institute page 1 Growing Up A Star This activity helps students understand and interpret the Hertzsprung Russell (HR) diagram a graphical representation of how stars evolve that is
THE PLEIADES OPEN CLUSTER
THE PLEIADES OPEN CLUSTER G. Iafrate (a), M. Ramella (a) and P. Padovani (b) (a) INAF - Astronomical Observatory of Trieste (b) ESO - European Southern Observatory 1 Introduction Open star clusters are
1 of 6 5/2/2015 6:12 PM
1 of 6 5/2/2015 6:12 PM 1. What is parallax? The distance to an object, measured in parsecs. The difference between the apparent and absolute magnitude. The apparent shift in POSITION of an object caused
Characterizing Stars
Characterizing Stars 1 Guiding Questions 1. How far away are the stars? 2. What evidence do astronomers have that the Sun is a typical star? 3. What is meant by a first-magnitude or second magnitude star?
Characterizing Stars. Guiding Questions. Parallax. Careful measurements of the parallaxes of stars reveal their distances
Guiding Questions Characterizing Stars 1. How far away are the stars? 2. What evidence do astronomers have that the Sun is a typical star? 3. What is meant by a first-magnitude or second magnitude star?
The Sun and the Stars
Classification of stellar spectra Potted History : 1802 William Wallaston showed that the spectrum of the sun is not simply a continuous spectrum, but is broken up by a series of dark lines (absorption
Calculating Main Sequence Lifetimes
Calculating Main Sequence ifetimes At the beginning of the twentieth century two astronomers, the Danish E. Hertzsprung and the American H. N. Russell, established a correlation between two important stellar
LAB: Star Classification
Name: LAB: Star Classification INTRODUCTION: Like most scientists, astronomers like to categorize the Universe around them, and stars are no exception. Here s how astronomers classify stars into different
5. A particular star has an angle of parallax of 0.2 arcsecond. What is the distance to this star? A) 50 pc B) 2 pc C) 5 pc D) 0.
Name: Date: 1. How far away is the nearest star beyond the Sun, in parsecs? A) between 1 and 2 pc B) about 12 pc C) about 4 pc D) between 1/2 and 1 pc 2. Parallax of a nearby star is used to estimate its
Measuring the Stars. Chapter 10. Chapters 17, 19, 18
Measuring the Stars Chapter 10 Chapters 17, 19, 18 1 2 3 Bessel Hipparcos 4 Lecture-Tutorial on Parallax and the Parsec p 37 6) Consider two stars (C and D) that both exhibit parallax. If C appears to
The Distance Modulus. Absolute Magnitude. Chapter 9. Family of the Stars
Foundations of Astronomy 13e Seeds Phys1403 Introductory Astronomy Instructor: Dr. Goderya Chapter 9 Family of the Stars Cengage Learning 016 Topics for Today s Class 1. Recap: Intrinsic Brightness a)
Some Basic Properties of Stars
Some Basic Properties of Stars Thinking about what data tells us Stars have a variety of properties that can be measured: brightness, distance, rotation rate, temperature, radius, mass There are a variety
THE STARS. Information and contacts: -
THE STARS G. Iafrate (a), M. Ramella (a) and V. Bologna (b) (a) INAF - Astronomical Observatory of Trieste (b) Istituto Comprensivo S. Giovanni Sc. Sec. di primo grado M. Codermatz" - Trieste Information
Universe. Tenth Edition. The Nature of the Stars. Parallax. CHAPTER 17 The Nature of Stars
Universe Tenth Edition The Nature of the Stars Roger A. Freedman, Robert M. Geller, William J. Kaufmann III CHAPTER 17 The Nature of Stars W. H. Freeman and Company Parallax Careful measurements of the
Chapter 8: The Family of Stars
Chapter 8: The Family of Stars We already know how to determine a star s surface temperature chemical composition motion Next, we will learn how we can determine its distance luminosity radius mass Measuring
Student Exploration: H-R Diagram
Name: Date: Student Exploration: H-R Diagram Vocabulary: giant, H-R diagram, luminosity, main sequence, star, supergiant, white dwarf Prior Knowledge Questions (Do these BEFORE using the Gizmo.) 1. The
Write It! Students should be encouraged to do the Research and Explore station before attempting this one.
Kesler Science Station Lab H-R Diagram Teacher Directions Explore It! I will spend much of my time at this station making sure that the students are doing the Celebrity H-R diagram correctly and not wasting
Revision: Sun, Stars (and Planets) See web slides of Dr Clements for Planets revision. Juliet Pickering Office: Huxley 706
Revision: Sun, Stars (and Planets) See web slides of Dr Clements for Planets revision Juliet Pickering Office: Huxley 706 Office hour (Pickering): Thursday 22nd May 12-11 pm Outline overview of first part
Hot Stars as Targets for Intensity Interferometry. Hannes Jensen Lund Observatory, Sweden
Hot Stars as Targets for Intensity Interferometry Hannes Jensen Lund Observatory, Sweden Aims Given recent progress in phase interferometry: which should be the prime observational targets for II? What
Atlantis Challenger Columbia. Discovery Endeavour Enterprise
T1 T2 T3 T4 T5 SCORE: 150 / 150 + Bonus 2 KEY: Alternative, acceptable answers are given in brackets Bonus: Name NASA s 6 space shuttles 1 bonus point per 3 correct answers. (2 pts total) Atlantis Challenger
HR Diagram Student Guide
Name: HR Diagram Student Guide Pretest Score: Background Information Work through the background sections on Spectral Classification, Luminosity, and the Hertzsprung-Russell Diagram. Then complete the
Organizing the Family of Stars:
Organizing the Family of Stars: We know: Stars have different temperatures, different luminosities, and different sizes. To bring some order into that zoo of different types of stars: organize them in
Properties of Stars & H-R Diagram
Properties of Stars & H-R Diagram What is a star? A cloud of gas, mainly hydrogen and helium The core is so hot/dense that nuclear fusion can occur. The fusion converts light nuclei (elements) into heavier
Reading and Announcements. Read Chapters 8.3, 11.5, 12.1 Quiz #5, Thursday, March 21 Homework #5 due Tuesday, March 19
Reading and Announcements Read Chapters 8.3, 11.5, 12.1 Quiz #5, Thursday, March 21 Homework #5 due Tuesday, March 19 Measurements of Star Properties Apparent brightness Direct measurement Parallax Distance
Y Centauri A 6. Alpha O Centauri B 7. Alpha
H-R Star Spectrum Lab The H-R diagram, as it s known for short, plots a star s luminosity its true brightness against its surface temperature in Kelvin. Are there patterns that emerge and what does this
How do we know the distance to these stars? The Ping Pong Ball Challenge -Devise a method for determining the height of the ping pong ball above the floor. -You are restricted to the floor. -You can only
INSIDE LAB 8: Plotting Stars on the Hertzsprung- Russell Diagram
INSIDE LAB 8: Plotting Stars on the Hertzsprung- Russell Diagram OBJECTIVE: To become familiar with the Hertzsprung-Russell diagram and the method of spectroscopic parallax. DISCUSSION: The Hertzsprung-Russell
Book page cgrahamphysics.com Stellar Spectra
Book page 650-652 Stellar Spectra Emission and absorption Spectra The black lines of the absorption spectrum match up with the bright lines of the emission spectrum Spectra unique to each element Emission
Lecture 26 The Hertzsprung- Russell Diagram January 13b, 2014
1 Lecture 26 The Hertzsprung- Russell Diagram January 13b, 2014 2 Hertzsprung-Russell Diagram Hertzsprung and Russell found a correlation between luminosity and spectral type (temperature) 10000 Hot, bright
Mass-Luminosity and Stellar Lifetimes WS
Name Mass-Luminosity and Stellar Lifetimes WS The graph shows the Mass-Luminosity Relationship for main sequence stars. Use it to answer questions 1-3. 1) A star with a mass of 0.5 solar masses would be
Hertzprung-Russel and colormagnitude. ASTR320 Wednesday January 31, 2018
Hertzprung-Russel and colormagnitude diagrams ASTR320 Wednesday January 31, 2018 H-R diagram vs. Color- Magnitude Diagram (CMD) H-R diagram: Plot of Luminosity vs. Temperature CMD: Plot of magnitude vs.
Ohio University - Lancaster Campus slide 1 of 47 Spring 2009 PSC 100. A star s color, temperature, size, brightness and distance are all related!
Ohio University - Lancaster Campus slide 1 of 47 A star s color, temperature, size, brightness and distance are all related! Ohio University - Lancaster Campus slide 2 of 47 The Beginnings Late 1800 s,
Hertzsprung-Russel Diagrams and Distance to Stars
Chapter 10 Hertzsprung-Russel Diagrams and Distance to Stars 10.1 Purpose In this lab, we will explore how astronomer classify stars. This classificatin one way that can be used to determine the distance
Magnitudes. How Powerful Are the Stars? Luminosities of Different Stars
How Powerful Are the Stars? Some stars are more powerful than others Power is energy output per. (Example: 00 Watts = 00 joules per second) Astronomers measure the power, or brightness of stars in ways:
Chapter 11 Surveying the Stars
Chapter 11 Surveying the Stars Luminosity Luminosity: Rate of energy emitted by star every second. Apparent brightness (flux): Amount of energy passing through every second per unit area. Luninosity =
Pr P ope p rti t es s of o f St S a t rs
Properties of Stars Distances Parallax ( Triangulation ): - observe object from two separate points - use orbit of the Earth (1 AU) - measure angular shift of object - angle depends on distance to object
Astronomical "color"
Astronomical "color" What color is the star Betelgeuse? It's the bright star at upper left in this picture of Orion taken by a student at the RIT Observatory. Orange? Red? Yellow? These are all reasonable
A star is at a distance of 1.3 parsecs, what is its parallax?
Stars Spectral lines from stars Binaries and the masses of stars Classifying stars: HR diagram Luminosity, radius, and temperature Vogt-Russell theorem Main sequence Evolution on the HR diagram A star
Stars: Temperature and Color
Stars: Temperature and Color Goals and Objectives Students will be able to describe essential ideas about the composition and structure of the universe and the Earth s place in it (PASS 3.4.7.D) Students
Lecture 21. Stellar Size
Lecture 21 Stellar Mass; The Main Sequence Visual and Spectroscopic Binaries Mass and the Main Sequence Explaining the Main Sequence Mar 8, 2006 Astro 100 Lecture 21 1 Stellar Size Taking ratios to the
Astrophysical Techniques. opt nd Year Astrophysics Group Research Project
Astrophysical Techniques opt.292 2 nd Year Astrophysics Group Research Project Paul O Brien & Rhaana Starling For this lecture and lab handout see http://www2.star.le.ac.uk/pto/astrolab2.html Aim of this
A Stellar Spectra 3. Stars shine at night (during the day too!). A star is a self-luminous sphere of gas. Stars are held together by gravity.
Stellar Spectra Relativity and Astrophysics Lecture 12 Terry Herter Outline What is a star? Stellar Spectra Kirchhoff s Laws Spectral Classification Spectral Types: O B A F G K M L T Stellar Photometry
The Hertzprung-Russell Diagram. The Hertzprung-Russell Diagram. Question
Key Concepts: Lecture 21: Measuring the properties of stars (cont.) The Hertzsprung-Russell (HR) Diagram (L versus T) The Hertzprung-Russell Diagram The Stefan-Boltzmann Law: flux emitted by a black body
OTHER MOTIONS. Just so far away they appear to move very slowly
OTHER MOTIONS The position of a nearby star changing over a year gives us parallax Stars can also move on their own Real motion, not just our point of view They are just balls of gas and are moving around
The Magnitude Scale Measuring the brightness of astronomical objects
The Magnitude Scale Measuring the brightness of astronomical objects While cataloging stars in the sky, the Greek Astronomer Hipparchus developed the magnitude system, which is still used by astronomers
Determining the Properties of the Stars
Determining the Properties of the Stars This set of notes by Nick Strobel covers: The properties of stars--their distances, luminosities, compositions, velocities, masses, radii, and how we determine those
Star Search Game: Constructing a Hertzsprung-Russell Diagram Inspired by: Ian Christie (VSSEC); Activity created by: Nandita Bajaj
Star Search Game: Constructing a Hertzsprung-Russell Diagram Inspired by: Ian Christie (VSSEC); Activity created by: Nandita Bajaj Introduction: Star Search is an online game developed by the Victorian
Photosphere. Bob Stein s simulation movie. Chromosphere. Corona. Solar wind
Photosphere Layer from which light escapes directly into space. Photosphere is what we see. Light from lower layers scatters. Q: Suppose we observe the neutrinos from the sun. The size of the sun when
Automated classification of sloan digital sky survey (SDSS) stellar spectra using artificial neural networks
DOI 10.1007/s10509-008-9816-5 ORIGINAL ARTICLE Automated classification of sloan digital sky survey (SDSS) stellar spectra using artificial neural networks Mahdi Bazarghan Ranjan Gupta Received: 14 November
Name: Partner(s): 1102 or 3311: Desk # Date: NGC 6633
Name: Partner(s): 1102 or 3311: Desk # Date: NGC 6633 Determining the Age of a Cluster Purpose Understand how HR diagrams reveal information about stellar evolution Use an HR diagram to determine the age
Physical Data Mass = 2x10 30 kg (333,000 time more massive than the Earth) Diameter: 7x10 5 km (about 100 Earth radii) Volume: you can fit about 1.3 m
The Sun Physical Data Mass = 2x10 30 kg (333,000 time more massive than the Earth) Diameter: 7x10 5 km (about 100 Earth radii) Volume: you can fit about 1.3 million earths inside the sun! 70% Hydrogen,
Temperature, Blackbodies & Basic Spectral Characteristics.
Temperature, Blackbodies & Basic Spectral Characteristics. Things that have one primary temperature but also exhibit a range of temperatures are known in physics as blackbodies. They radiate energy thermally.
ASTR Look over Chapter 15. Good things to Know. Triangulation
ASTR 1020 Look over Chapter 15 Good things to Know Triangulation Parallax Parsecs Absolute Visual Magnitude Distance Modulus Luminosity Balmer Lines Spectral Classes Hertzsprung-Russell (HR) diagram Main
Wednesday 21 June 2017 Morning
Oxford Cambridge and RSA Wednesday 21 June 2017 Morning A2 GCE PHYSICS B (ADVANCING PHYSICS) G495/01 Field and Particle Pictures ADVANCE NOTICE Duration: 2 hours *6744539949* INSTRUCTIONS TO CANDIDATES
The Hertzsprung Russell Diagram. The Main Sequence
The Hertzsprung Russell Diagram H R diagram plots stellar luminosity against surface temperature Luminosity ranges 10-4 10 4 L. Temperature ranges by a factor of 10 increases to the left spectral sequence
OPTION E, ASTROPHYSICS TEST REVIEW
IB PHYSICS Name: DEVIL PHYSICS Period: Date: BADDEST CLASS ON CAMPUS OPTION E, ASTROPHYSICS TEST REVIEW S1. This question is about the nature of certain stars on the Hertzsprung-Russell diagram and determining
Extragalactic Astronomy
Extragalactic Astronomy Topics: Milky Way Galaxies: types, properties, black holes Active galactic nuclei Clusters and groups of galaxies Cosmology and the expanding universe Formation of structure Galaxies
a. Star A c. The two stars are the same distance b. Star B d. Not enough information
Name: Astro 102 S17 Test 1 Multiple Choice Identify the choice that best completes the statement or answers the question. 1. Your test is Version A. Please fill in the circle for A for this question on
College of San Mateo Observatory
College of San Mateo Observatory Stellar Spectra Catalog SGS Spectrograph Spectra taken from CSM observatory using SBIG Self Guiding Spectrograph (SGS) A work in progress compiled by faculty, staff, and
Stars. For Jupiter: M/Msun = 0.001
Stars Stars are classified by spectral classes O,B,A,F,G,K,M Oh be a fine girl (or guy), kiss me! Key here is the effective temperature of the star (surface temperature) Difference in spectrum is due to
Question: How do we use a Hertzsprung-Russell Diagram to explain star characteristics?
The Hertzsprung-Russell Diagram Assignment Introduction: The development of the H-R Diagram began with Danish astronomer Ejnar Hertzsprung who began plotting the stars around 1911. American astronomer
Star Magnitudes & Distances with Stellarium (Stellarium Exercise #2)
Name Date Star Magnitudes & Distances with Stellarium (Stellarium Exercise #2) Millions of stars are scattered across the sky. Astronomers want to study these stars as carefully as possible. This means
Stars: some basic characteristics
Stars: some basic characteristics Stars! How bright are they? How massive are they? What are the different types? How long do they live? How hot are they? Stellar brightness and luminosity The apparent
OPTION E, ASTROPHYSICS TEST REVIEW
IB PHYSICS Name: DEVIL PHYSICS Period: Date: # Marks: XX Raw Score: IB Curve: BADDEST CLASS ON CAMPUS OPTION E, ASTROPHYSICS TEST REVIEW S1. This question is about the nature of certain stars on the Hertzsprung-Russell
Properties of Stars. N. Sharp (REU/NOAO/AURA/NSF)
Properties of Stars N. Sharp (REU/NOAO/AURA/NSF) What properties of the stars can we determine just from this image? Measuring Stars Measuring Stars Information you can get from 1 image: Position on the
Lines of Hydrogen. Most prominent lines in many astronomical objects: Balmer lines of hydrogen
The Family of Stars Lines of Hydrogen Most prominent lines in many astronomical objects: Balmer lines of hydrogen The Balmer Thermometer Balmer line strength is sensitive to temperature: Most hydrogen
Observed Properties of Stars ASTR 2120 Sarazin
Observed Properties of Stars ASTR 2120 Sarazin Extrinsic Properties Location Motion kinematics Extrinsic Properties Location Use spherical coordinate system centered on Solar System Two angles (θ,φ) Right
Family of stars. Fred Sarazin Physics Department, Colorado School of Mines. PHGN324: Family of stars
Family of stars Reminder: the stellar magnitude scale In the 1900 s, the magnitude scale was defined as follows: a difference of 5 in magnitude corresponds to a change of a factor 100 in brightness. Dm
Light and Stars ASTR 2110 Sarazin
Light and Stars ASTR 2110 Sarazin Doppler Effect Frequency and wavelength of light changes if source or observer move Doppler Effect v r dr radial velocity dt > 0 moving apart < 0 moving toward Doppler
The Hertzsprung-Russell Diagram and Stellar Evolution
The Hertzsprung-Russell Diagram and Stellar Evolution Names: The H-R Diagram and Stellar Properties Activity 1. In which corner of the diagram (upper right, upper left, lower right, or lower left) would
High Science Earth Science Pretest: Data Analysis & Interpretation
High Science Earth Science Pretest: Data Analysis & Interpretation Answer the set of questions that follows each table or figure. Figure 1: Hertzsprung-Russell (H-R) diagram 1. Considering Figure 1, which
The Hertzsprung-Russell Diagram
The Hertzsprung-Russell Diagram Name: Date: 1 Introduction As you may have learned in class, the Hertzsprung-Russell Diagram, or the HR diagram, is one of the most important tools used by astronomers:
29:50 Stars, Galaxies, and the Universe First Hour Exam October 6, 2010 Form A
29:50 Stars, Galaxies, and the Universe First Hour Exam October 6, 2010 Form A There are 32 questions. Read through each question and all the answers before choosing. Budget your time. No whining. Walk
Hertzsprung-Russell Diagram, Flux, Luminosity, Magnitude 10 Oct
Russell Diagram, Flux, Luminosity, Magnitude 10 Oct Outline Review of 7 Oct Thermal radiation Wien s Law Stefan Boltzmann Law How to measure temperature of stars. AJ Cannon s method of classifying spectra.
How does the Sun shine? What is the Sun s structure? Lifetime of the Sun. Luminosity of the Sun. Radiation Zone. Core 3/30/17
What is the Sun s structure? From inside out, the layers are: Core Radiation Zone Convection Zone Photosphere Chromosphere Corona How does the Sun shine? The Sun has its own energy source Main difference
For instance, for a particular star cluster, these data were derived:
Astronomy 100 Name(s): Exercise 5: The H-R diagram and spectroscopy A very basic correlation using the color index By the 1920 s, various astronomers had evidence that the temperature of a star was also
Using the Star Wheel Laboratory 2
Objective: Using the Star Wheel Laboratory 2 This laboratory introduces the Star Wheel; which is a common tool used in backyard observing. This tool helps approximate the location of constellations and
Homework 6, due October 27: Problems in Measuring the Universe:
Homework 6, due October 27: Problems in Measuring the Universe: 4.2. You want to observe a star at -10 degrees declination through no more than two air masses from a telescope at 20 degrees north latitude.
Measuring the Stars. The measurement of distances The family of distance-measurement techniques used by astronomers to chart the universe is called
Measuring the Stars How to measure: Distance Stellar motion Luminosity Temperature Size Evolutionary stage (H-R diagram) Cosmic distances Mass The measurement of distances The family of distance-measurement
OPEN CLUSTER PRELAB The first place to look for answers is in the lab script!
NAME: 1. Define using complete sentences: Globular Cluster: OPEN CLUSTER PRELAB The first place to look for answers is in the lab script! Open Cluster: Main Sequence: Turnoff point: Answer the following
Test #2 results. Grades posted in UNM Learn. Along with current grade in the class
Test #2 results Grades posted in UNM Learn D C B A Along with current grade in the class F Clicker Question: If the Earth had no Moon then what would happen to the tides? A: The tides would not be as strong
Web sites and Worksheets
Introduction Web sites and Worksheets Sandra Woodward Oakhill College Castle Hill (swoodward@oakhill.nsw.edu.au) Astronomy is a practical subject by nature. Unfortunately for teachers, many of the practical
Summary of Stellar Proper/es
Summary of Stellar Proper/es Large range of Stellar Luminosi/es: 10 4 to 10 6 L sun Large range of Stellar Radii: 10 2 to 10 3 R sun Modest range of Stellar Temperatures: 3000 to >50,000 K Wide Range of