# Planets are plentiful

Size: px
Start display at page:

Transcription

1 Extra-Solar Planets

2 Planets are plentiful The first planet orbiting another Sun-like star was discovered in We now know of 209 (Feb 07). Including several stars with more than one planet - true planetary systems

3 How do we find these planets? We can t easily take photographs of them - they re too faint in comparison to their parent star

4 Observed with the VLT

5 The Doppler wobble method The star wobbles back and forth under the gravitational influence of its orbiting planet

6 The Doppler wobble method The spectra of stars show absorption lines at specific wavelengths

7 Discovering Extra-Solar Planets Method 1 Use the fact that the Sun and Planet corotate around their common centre of gravity. So the star will be moving around a small ellipse whose size depends on the mass and distance of the planet. Precise measurements of the doppler shift in the spectral lines of the star can show up this motion and hence detect the planet.

8 Using a very sensitive spectrometer!

9 Doppler method will not work if orbital plane is at right angles to us

10 The Doppler wobble method The light from the star is Doppler shifted back and forth Biased to high-mass planets close to parent stars

11 51 Pegasai The first planet detected around a normal star. Period just 4 days! A gas giant very close to its star.

12

13 An elliptical orbit

14 How do you find the Mass and Distance of the Planet? 1) From the peak velocity of the star when it is coming towards us or going away from us - and the period of the oscillation we can calculate the circumference of the orbit of the star and hence its distance from the centre of mass of the system. r star = V max x P / 2 x π

15 To simplify the the following calculation assume that the planet is very much less massive that the star. From Kepler s Third Law we can calculate the Radius of the orbit of the Planet. If R is in AU, and the period is in years, then for a 1 solar mass star. p 2 = R 3 So this gives us the distance in AU Knowing 1 AU in metres one can then calculate R in metres balancing about the centre of Mass M r = m R So m = (M sun x r ) / R

16 Example: 1 Solar Mass Star, Period 4 years, V max = 20m/sec R star = 20 x 4 x 365 x 24 x 3600 / 2 x π = 4 x 10 8 m From Kepler s third law : p 2 = R 3 R planet = ((4) 2 ) 1/3 = 2.5 AU m planet = 1x r/r = 1 x 4 x 10 8 / 2.5 x 1.49x10 11 =.001 Solar masses NB Jupiter has a mass of.001 Solar masses so this is a gas giant planet of 1 Jovian Mass.

17 What objects might there be orbiting a star? Other Stars in Binary or Multiple Star systems. masses > 0.08 M sun 2) Brown Dwarfs Not quite stars 0.08 M sun > m > 0.03 M sun 3) Planets masses < 0.01 M sun So planets so far found only up to 17 x Jovian Mass

18 Doppler Shift Limitations Present doppler precision is ~ 3m/sec. Effect of Jupiter on the Sun gives a V max of ~20m/sec BUT that of Earth is a 1/10 m 30 times less than can be detected at present We must observe for at least one orbit of the planet. Saturn orbits the Sun every 29.4 years. Only ~ 12 years of observations so far so, as yet, difficult to detect planets distant from their Sun.

19 Extra-solar planet masses from Doppler Method

20 Method 2

21 Wiggles in the motion of a star across the sky Called Proper Motion, usually a straight line, but not in the case of Sirius! Its companion is a dead star called a White Dwarf. No planets discovered this way yet.

22 NB Method 1 cannot work if the orbital plane of the extra solar planet is at right angles to us. Method 2 will work when Method 1 cannot. Method 2 cannot work if the if the orbital plane of the extra solar planet includes the Earth. BOTH will work when the orbit of the planet is inclined at intermediate angles

23 Method 3: Planetary transits - Detect the transit of a planet as it crosses the face of the star. This results in a slight drop in luminosity Method 3 can only work if the orbital plane of the planet includes the Earth.

24

25 An example

26 The Transit Method Look for the dip in light from a star as a planet passes in front Best done from space NASA Kepler mission in planning phase Has the potential to detect Earthlike planets

27 Method 4 Gravitational Micro-lensing

28 Look for the increase in brightness of a distant star as another star with planet passes in front. The microlensing method

29 Magnification

30 Size of the patch indicates relative brightness

31 What we see

32 Effect of a planet

33 The microlensing method First discovery announced 2004 May 10. Has the potential to detect Earth-like planets.

34

35 Smallest Planet So Far 5 x Earth mass Discovered by a collaboration including Jodrell astronomers 100 million stars routinely monitored 120 lensing events in progress at any one time

36

37

38

39 Today Notice: planets have now been found out to nearly 6 AU

40 Separation from their Sun

41

42

43 Distribution of mass Properties of planets

44 Properties of planets

45 The Future Direct detection Must eliminate the overwhelming brightness of the star. 1) Use Infrared as planets are brighter in relation to their Sun. 2) Use a multiple mirror system as an Interferometer - a bit like Young s Slits to put a null on the stars position. Nasa s Planet Finder ESO s Darwin

46 Direct Detection: A planet in orbit around a Brown Dwarf

47 How can we see the planet close to its Sun?

48 1) Occult the Star

49 Use a Coronograph

50 2) Use an occulter

51 Detecting life NASA Terrestrial Planet Finder ESA Darwin

52 3) Use an Infra-red Interferometer Terrestrial Planet Finder

53 Darwin

54

55

56

57 What does it tell us?

58

59 Detecting life Water vapour and ozone are signs of life Simulated spectrum of Earth at 10pc as seen by Darwin

60 Exploring extrasolar planets It s difficult to go there. The nearest other star is about 40,000 billion km away. Some typical speeds and travel times to nearest star: Supersonic jet 1600 km/hour 3 million years Space probe 60,000 km/hour 75,000 years (fastest thing we ve ever built) Light 1 billion km/hour 4.5 years

### Planets & Life. Planets & Life PHYS 214. Please start all class related s with 214: 214: Dept of Physics (308A)

Planets & Life Planets & Life PHYS 214 Dr Rob Thacker Dept of Physics (308A) thacker@astro.queensu.ca Please start all class related emails with 214: 214: Today s s lecture Assignment 1 marked will hand

### Extrasolar Planets. Today. Dwarf Planets. Extrasolar Planets. Next week. Review Tuesday. Exam Thursday. also, Homework 6 Due

Extrasolar Planets Today Dwarf Planets Extrasolar Planets Next week Review Tuesday Exam Thursday also, Homework 6 Due will count best 5 of 6 homeworks 2007 Pearson Education Inc., publishing as Pearson

### Key Ideas: The Search for New Planets. Scientific Questions. Are we alone in the Universe? Direct Imaging. Searches for Extrasolar Planets

The Search for New Planets Key Ideas: Search for planets around other stars. Successful Search Techniques: Astrometric Wobble Doppler Wobble major discovery method Planetary Transits planets we can study

### 10/16/ Detecting Planets Around Other Stars. Chapter 10: Other Planetary Systems The New Science of Distant Worlds

10/16/17 Lecture Outline 10.1 Detecting Planets Around Other Stars Chapter 10: Other Planetary Systems The New Science of Distant Worlds Our goals for learning: How do we detect planets around other stars?

### Searching for Other Worlds

Searching for Other Worlds Lecture 32 1 In-Class Question What is the Greenhouse effect? a) Optical light from the Sun is reflected into space while infrared light passes through the atmosphere and heats

### Extrasolar Planets. Methods of detection Characterization Theoretical ideas Future prospects

Extrasolar Planets Methods of detection Characterization Theoretical ideas Future prospects Methods of detection Methods of detection Methods of detection Pulsar timing Planetary motion around pulsar

### 13 - EXTRASOLAR PLANETS

NSCI 314 LIFE IN THE COSMOS 13 - EXTRASOLAR PLANETS Dr. Karen Kolehmainen Department of Physics, CSUSB http://physics.csusb.edu/~karen/ EXTRASOLAR PLANETS? DO PLANETS ORBIT AROUND OTHER STARS? WE WOULD

### Credit: NASA/Kepler Mission/Dana Berry. Exoplanets

Credit: NASA/Kepler Mission/Dana Berry Exoplanets Outline What is an exoplanet? Why are they interesting? How can we find them? Exolife?? The future... Jon Thaler Exoplanets 2 What is an Exoplanet? Most

### Can We See Them?! Planet Detection! Planet is Much Fainter than Star!

Can We See Them?! Planet Detection! Estimating f p! Not easily! Best cases were reported in late 2008! Will see these later! Problem is separating planet light from star light! Star is 10 9 times brighter

### Chapter 13 Other Planetary Systems. Why is it so difficult to detect planets around other stars? Brightness Difference

Chapter 13 Other Planetary Systems The New Science of Distant Worlds 13.1 Detecting Extrasolar Planets Our goals for learning:! Why is it so difficult to detect planets around other stars?! How do we detect

### II Planet Finding.

II Planet Finding http://sgoodwin.staff.shef.ac.uk/phy229.html 1.0 Introduction There are a lot of slides in this lecture. Much of this should be familiar from PHY104 (Introduction to Astrophysics) and

### Chapter 13 Other Planetary Systems. The New Science of Distant Worlds

Chapter 13 Other Planetary Systems The New Science of Distant Worlds 13.1 Detecting Extrasolar Planets Our goals for learning Why is it so difficult to detect planets around other stars? How do we detect

### Extrasolar planets. Lecture 23, 4/22/14

Extrasolar planets Lecture 23, 4/22/14 Extrasolar planets Extrasolar planets: planets around other stars Also called exoplanets 1783 exoplanets discovered as of 4/21/14 Orbitting 1105 different stars Number

### Chapter 13 Other Planetary Systems. Why is it so difficult to detect planets around other stars? Size Difference. Brightness Difference

Chapter 13 Other Planetary Systems Why is it so difficult to detect planets around other stars? Size Difference Planets are small compared to interstellar distances 10 billion to 1 scale Sun is size of

### Planet Detection. Estimating f p

Planet Detection Estimating f p Can We See Them? Not yet, but there are plans 3 recent claims, but planets very far from star, so some doubts Problem is separating planet light from star light Star is

### Planet Detection. AST 105 Intro Astronomy The Solar System

Review AST 105 Intro Astronomy The Solar System MIDTERM III this THURSDAY 04/8 covering LECT. 17 through We ve talked about the Terrestrial Planets and the Jovian Planets - What about planets around other

### Planets and Brown Dwarfs

Extra Solar Planets Extra Solar Planets We have estimated there may be 10 20 billion stars in Milky Way with Earth like planets, hospitable for life. But what evidence do we have that such planets even

### Planet Detection! Estimating f p!

Planet Detection! Estimating f p! Can We See Them?! Not easily! Best cases were reported in late 2008! Will see these later! Problem is separating planet light from star light! Star is 10 9 times brighter

### Chapter 13 Lecture. The Cosmic Perspective Seventh Edition. Other Planetary Systems: The New Science of Distant Worlds Pearson Education, Inc.

Chapter 13 Lecture The Cosmic Perspective Seventh Edition Other Planetary Systems: The New Science of Distant Worlds 13.1 Detecting Planets Around Other Stars Our goals for learning: Why is it so challenging

### Lab #5. Searching for Extrasolar Planets

Lab #5 Searching for Extrasolar Planets Introduction Since the beginning of recorded history, humans have wondered whether we are alone in the Universe. Recently, Astronomers have begun to make significant

### Detecting Extra Solar Planets

Detecting Extra Solar Planets The Extrasolar Planet Count Currently, 288 stars have been discovered to have planets. Some of these have more than one, so a total of 380 planets have been discovered as

### 2010 Pearson Education, Inc.

Thought Question Suppose you found a star with the same mass as the Sun moving back and forth with a period of 16 months. What could you conclude? A. It has a planet orbiting at less than 1 AU. B. It has

### Chapter 13 Lecture. The Cosmic Perspective Seventh Edition. Other Planetary Systems: The New Science of Distant Worlds Pearson Education, Inc.

Chapter 13 Lecture The Cosmic Perspective Seventh Edition Other Planetary Systems: The New Science of Distant Worlds 13.1 Detecting Planets Around Other Stars Our goals for learning: Why is it so challenging

### Other Planetary Systems (Chapter 13) Extrasolar Planets. Is our solar system the only collection of planets in the universe?

Other Planetary Systems (Chapter 13) Extrasolar Planets Is our solar system the only collection of planets in the universe? Based on Chapter 13 No subsequent chapters depend on the material in this lecture

### Observations of extrasolar planets

Observations of extrasolar planets 1 Mercury 2 Venus radar image from Magellan (vertical scale exaggerated 10 X) 3 Mars 4 Jupiter 5 Saturn 6 Saturn 7 Uranus and Neptune 8 we need to look out about 10 parsecs

### Chapter 13 Lecture. The Cosmic Perspective. Seventh Edition. Other Planetary Systems: The New Science of Distant Worlds Pearson Education, Inc.

Chapter 13 Lecture The Cosmic Perspective Seventh Edition Other Planetary Systems: The New Science of Distant Worlds 13.1 Detecting Planets Around Other Stars Our goals for learning: Why is it so challenging

### Lecture 12: Extrasolar planets. Astronomy 111 Monday October 9, 2017

Lecture 12: Extrasolar planets Astronomy 111 Monday October 9, 2017 Reminders Star party Thursday night! Homework #6 due Monday The search for extrasolar planets The nature of life on earth and the quest

### » How vast those Orbs must be, and how inconsiderable this Earth, the Theatre upon which all our mighty Designs, all our Navigations, and all our

» How vast those Orbs must be, and how inconsiderable this Earth, the Theatre upon which all our mighty Designs, all our Navigations, and all our Wars are transacted, is when compared to them. A very fit

### The Main Point(s) Lecture #36: Planets Around Other Stars. Extrasolar Planets! Reading: Chapter 13. Theory Observations

Lecture #36: Planets Around Other Stars Extrasolar Planets! Theory Observations Detection methods Results to date... Implications for "Habitable Zones" Reading: Chapter 13 Astro 102/104 1 The Main Point(s)

### Searching for Other Worlds: The Methods

Searching for Other Worlds: The Methods John Bally 1 1 Center for Astrophysics and Space Astronomy Department of Astrophysical and Planetary Sciences University of Colorado, Boulder The Search Extra-Solar

### Exoplanets Direct imaging. Direct method of exoplanet detection. Direct imaging: observational challenges

Black body flux (in units 10-26 W m -2 Hz -1 ) of some Solar System bodies as seen from 10 pc. A putative hot Jupiter is also shown. The planets have two peaks in their spectra. The short-wavelength peak

### HD Transits HST/STIS First Transiting Exo-Planet. Exoplanet Discovery Methods. Paper Due Tue, Feb 23. (4) Transits. Transits.

Paper Due Tue, Feb 23 Exoplanet Discovery Methods (1) Direct imaging (2) Astrometry position (3) Radial velocity velocity Seager & Mallen-Ornelas 2003 ApJ 585, 1038. "A Unique Solution of Planet and Star

### 18 An Eclipsing Extrasolar Planet

Name: Date: 18 An Eclipsing Extrasolar Planet 18.1 Introduction One of the more recent new fields in astronomy is the search for (and discovery of) planets orbiting around stars other than our Sun, or

### There are 4 x stars in the Galaxy

ExtraSolar Planets Our solar system consists of 1 Star 4 Jovian planets (+ icy moons) 4 Terrestrial planets The asteroid belt (minor planets) The Kuiper belt (dwarf planets, plutinos and TNOs) The Oort

### Exoplanets Direct imaging. Direct method of exoplanet detection. Direct imaging: observational challenges

Black body flux (in units 10-26 W m -2 Hz -1 ) of some Solar System bodies as seen from 10 pc. A putative hot Jupiter is also shown. The planets have two peaks in their spectra. The short-wavelength peak

### 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

### Astronomy 330 HW 2. Outline. Presentations. ! Kira Bonk ascension.html

Astronomy 330 This class (Lecture 11): What is f p? Eric Gobst Suharsh Sivakumar Next Class: Life in the Solar System HW 2 Kira Bonk http://www.ufodigest.com/news/0308/ ascension.html Matthew Tenpas http://morphman.hubpages.com/hub/alien-

### Doppler Technique Measuring a star's Doppler shift can tell us its motion toward and away from us.

Doppler Technique Measuring a star's Doppler shift can tell us its motion toward and away from us. Current techniques can measure motions as small as 1 m/s (walking speed!). Sun motion due to: Jupiter:

### Astronomy 101 Lab: Hunt for Alien Worlds

Name: Astronomy 101 Lab: Hunt for Alien Worlds Be prepared to make calculations in today s lab. Laptops will also be used for part of the lab, but you aren t required to bring your own. Pre-Lab Assignment:

### Exoplanets. Saturday Physics for Everyone. Jon Thaler October 27, Credit: NASA/Kepler Mission/Dana Berry

Exoplanets Saturday Physics for Everyone Jon Thaler October 27, 2012 Credit: NASA/Kepler Mission/Dana Berry Outline What is an exoplanet? Why are they intereskng? How can we find them? Exolife?? The future...

### Habitability Outside the Solar System. A discussion of Bennett & Shostak Chapter 11 HNRS 228 Dr. H. Geller

Habitability Outside the Solar System A discussion of Bennett & Shostak Chapter 11 HNRS 228 Dr. H. Geller 1 Chapter Overview Distant Suns (11.1) Life cycle of stars and their habitability zones Extrasolar

### Other planetary systems

Exoplanets are faint! Other planetary systems Planets are seen only by reflected light at optical wavelengths At the distance of another star the faint light of a planet is lost in the glare of the star

### ASTRONOMY 202 Spring 2007: Solar System Exploration. Instructor: Dr. David Alexander Web-site:

ASTRONOMY 202 Spring 2007: Solar System Exploration Instructor: Dr. David Alexander Web-site: www.ruf.rice.edu/~dalex/astr202_s07 Class 37: Life in the Universe [4/18/07] Announcements Habitability of

### 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

### Why is it hard to detect planets around other stars?

Extrasolar planets Why is it hard to detect planets around other stars? Planets are small and low in mass Planets are faint The angular separation between planets and their stars is tiny Why is it hard

### Young Solar-like Systems

Young Solar-like Systems FIG.2. Panels(a),(b),and(c)show 2.9,1.3,and 0.87 mm ALMA continuum images of other panels, as well as an inset with an enlarged view of the inner 300 mas centered on the (f) show

### Searching for extrasolar planets using microlensing

Searching for extrasolar planets using microlensing Dijana Dominis Prester 7.8.2007, Belgrade Extrasolar planets Planets outside of the Solar System (exoplanets) Various methods: mostly massive hot gaseous

### Simon P. Balm Astro 5 Test #3 Sample Questions

Simon P. Balm Astro 5 Test #3 Sample Questions 1. What do we mean by the general habitability of a planet? A. the suitability for Life on it surface B. the suitability for Life beneath its surface C. its

### 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

### Search for Extra-Terrestrial Intelligence

Search for Extra-Terrestrial Intelligence Life in the Universe? What is life? (as we know it) Auto-regulation (ex. : sweating) Organization (A cell is more organized than a bunch of atoms) Metabolism :

### ! p. 1. Observations. 1.1 Parameters

1 Observations 11 Parameters - Distance d : measured by triangulation (parallax method), or the amount that the star has dimmed (if it s the same type of star as the Sun ) - Brightness or flux f : energy

### Chapter 8: The Family of Stars

Chapter 8: The Family of Stars Motivation We already know how to determine a star s surface temperature chemical composition surface density In this chapter, we will learn how we can determine its distance

### Other Solar Systems. Week 15 (Chapter 13): Other Planetary Systems

Week 15 (Chapter 13): Other Planetary Systems Nov. 30 Please pickup your grade sheet at front. We ll discuss at end of class. Other Solar Systems First one (51 Pegasi) discovered in 1995 Currently 268

### Extrasolar Planet Detection Methods. Tom Koonce September, 2005

Extrasolar Planet Detection Methods Tom Koonce September, 2005 Planets Around Other Stars? How is it possible to see something so small, so far away? If everything is aligned perfectly, we can see the

### Planets: Name Distance from Sun Satellites Year Day Mercury 0.4AU yr 60 days Venus yr 243 days* Earth 1 1 yr 1 day Mars 1.

The Solar System (Ch. 6 in text) We will skip from Ch. 6 to Ch. 15, only a survey of the solar system, the discovery of extrasolar planets (in more detail than the textbook), and the formation of planetary

### III The properties of extrasolar planets

III The properties of extrasolar planets (as of early 2016) http://sgoodwin.staff.shef.ac.uk/phy229.html 3.0 Introduction This lecture will discuss what we have found so far. It is important to remember

### PLANETARY SYSTEM: FROM GALILEO TO EXOPLANETS

PLANETARY SYSTEM: FROM GALILEO TO EXOPLANETS Rosa M. Ros Technical University of Catalonia, Barcelona (Spain) Abstract When in 1610 Galileo Galilei looked at Jupiter with the use of his telescope, he saw

### Planets Around Other Stars Extrasolar Planet Detection Methods. February, 2006

Planets Around Other Stars Extrasolar Planet Detection Methods February, 2006 Distribution of this File Extrasolar_planet_detection.ppt This Powerpoint presentation was put together for the purpose of

### Why Should We Expect to Find Other Planets? Planetary system formation is a natural by-product of star formation

1 Why Should We Expect to Find Other Planets? Planetary system formation is a natural by-product of star formation 2 Why Should We Expect to Find Other Planets? Observations show young stars are surrounded

### Chapter 15: The Origin of the Solar System

Chapter 15: The Origin of the Solar System The Solar Nebula Hypothesis Basis of modern theory of planet formation: Planets form at the same time from the same cloud as the star. Planet formation sites

### Announcements. Lecture 11 Properties of Stars. App Bright = L / 4!d 2

Announcements Quiz#3 today at the end of 60min lecture. Homework#3 will be handed out on Thursday. Due October 14 (next Thursday) Review of Mid-term exam will be handed out next Tuesday. Mid-term exam

### DETECTING TRANSITING PLANETS WITH COROT. Stefania Carpano ESAC (25th of November 2009)

DETECTING TRANSITING PLANETS WITH COROT Stefania Carpano ESAC (25th of November 2009) Outline 1) Introduction: Exoplanet science and detection methods Detection of exoplanets using the transit method The

### Extrasolar Planets. Properties Pearson Education Inc., publishing as Pearson Addison-Wesley

Extrasolar Planets Properties 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley Finding extrasolar planets is hard quick recap Planet Detection Direct: pictures or spectra of the planets

### The formation & evolution of solar systems

The formation & evolution of solar systems Content expectations Birth of the Solar System What did the material that eventually became the Sun and planets look like originally? Interstellar clouds like

### Lecture Outlines. Chapter 15. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.

Lecture Outlines Chapter 15 Astronomy Today 8th Edition Chaisson/McMillan Chapter 15 Exoplanets Units of Chapter 15 15.1 Modeling Planet Formation 15.2 Solar System Regularities and Irregularities 15.3

### Class 15 Formation of the Solar System

Class 16 Extra-solar planets The radial-velocity technique for finding extrasolar planets Other techniques for finding extrasolar planets Class 15 Formation of the Solar System What does a successful model

### Measuring the Properties of Stars (ch. 17) [Material in smaller font on this page will not be present on the exam]

Measuring the Properties of Stars (ch. 17) [Material in smaller font on this page will not be present on the exam] Although we can be certain that other stars are as complex as the Sun, we will try to

### Extrasolar Planets = Exoplanets III.

Extrasolar Planets = Exoplanets III http://www.astro.keele.ac.uk/~rdj/planets/images/taugruishydra2.jpg Outline Gravitational microlensing Direct detection Exoplanet atmospheres Detecting planets by microlensing:

### 4 1 Extrasolar Planets

Extrasolar Planets 4 1 Introduction 4 2 So far: have looked at planets around our Sun Physics question: Is our Solar System normal? = Are there planets around other stars? can then compare solar system

### Astronomy 102: Stars and Galaxies Examination 3 April 11, 2003

Name: Seat Number: Astronomy 102: Stars and Galaxies Examination 3 April 11, 2003 Do not open the test until instructed to begin. Instructions: Write your answers in the space provided. If you need additional

### Astro 1010 Planetary Astronomy Sample Questions for Exam 3

Astro 1010 Planetary Astronomy Sample Questions for Exam 3 Chapter 6 1. Which of the following statements is false? a) Refraction is the bending of light when it passes from one medium to another. b) Mirrors

### Searching for Earth-Like Planets:

Searching for Earth-Like Planets: NASA s Terrestrial Planet Finder Space Telescope Robert J. Vanderbei January 11, 2004 Amateur Astronomers Association of Princeton Peyton Hall, Princeton University Page

### 4. Direct imaging of extrasolar planets. 4.1 Expected properties of extrasolar planets. Sizes of gas giants, brown dwarfs & low-mass stars

4. Direct imaging of extrasolar planets Reminder: Direct imaging is challenging: The proximity to its host star: 1 AU at 1 for alpha Cen 0.15 for the 10th most nearby solar-type star The low ratio of planet

### Astronomy 102: Stars and Galaxies Examination 3 Review Problems

Astronomy 102: Stars and Galaxies Examination 3 Review Problems Multiple Choice Questions: The first eight questions are multiple choice. Except where explicitly noted, only one answer is correct for each

### Extra Solar Planetary Systems and Habitable Zones

Lecture Overview Extra Solar Planetary Systems and Habitable Zones Our Galaxy has 200 Billion Stars, Our Sun has 8 planets. It seems like an awful waste if we are alone Exoplanets Karen J. Meech, Svetlana

### Transiting Hot Jupiters near the Galactic Center

National Aeronautics and Space Administration Transiting Hot Jupiters near the Galactic Center Kailash C. Sahu Taken from: Hubble 2006 Science Year in Review The full contents of this book include more

### Lecture 20: Planet formation II. Clues from Exoplanets

Lecture 20: Planet formation II. Clues from Exoplanets 1 Outline Definition of a planet Properties of exoplanets Formation models for exoplanets gravitational instability model core accretion scenario

### Lecture 12: Distances to stars. Astronomy 111

Lecture 12: Distances to stars Astronomy 111 Why are distances important? Distances are necessary for estimating: Total energy released by an object (Luminosity) Masses of objects from orbital motions

### IB Physics - Astronomy

Solar System Our Solar System has eight planets. The picture below shows their relative sizes, but NOT their relative distances. A planet orbits the sun, and has gravitationally cleared its orbital area

### Astronomy 141 Life in the Universe Professor Gaudi Homework #4 Solutions

Astronomy 141 Life in the Universe Autumn Quarter 008 Prof Gaudi Homework #4 Solutions These questions concern the concept of targets for searches for extrasolar planets specifically (a) the number of

### Planets Beyond our Solar System: The New Astronomical Revolution

Planets Beyond our Solar System: The New Astronomical Revolution KITP Teacher Workshop, University of California at Santa Barbara, 2010 Hakan Armağan Burke High, Omaha, NE

### 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

### Lecture #15: Plan. Telescopes (cont d) Effects of Earth s Atmosphere Extrasolar planets = Exoplanets

Lecture #15: Plan Telescopes (cont d) Effects of Earth s Atmosphere Extrasolar planets = Exoplanets Resolving Power (review) The bigger the size of the telescope, the better it is at discerning fine details

### The Milky Way Galaxy (ch. 23)

The Milky Way Galaxy (ch. 23) [Exceptions: We won t discuss sec. 23.7 (Galactic Center) much in class, but read it there will probably be a question or a few on it. In following lecture outline, numbers

### 12.3 Pluto: Lone Dog No More

12.3 Pluto: Lone Dog No More Our goals for learning: How big can a comet be? What are the large objects of the Kuiper belt like? Are Pluto and Eris planets? How big can a comet be? Pluto s Orbit Pluto

### Astronomy 330 HW 2. Outline. Presentations. ! Alex Bara

Astronomy 330 This class (Lecture 10): Origin of the Moon Ilana Strauss Next Class: Our Planet Scott Huber Thomas Hymel HW 2! Alex Bara http://userpages.bright.net/~phobia/main.htm! Margaret Sharp http://hubpages.com/hub/proof-that-ufos-exist---

### Gravitational microlensing. Exoplanets Microlensing and Transit methods

Gravitational microlensing Exoplanets Microlensing and s Planets and Astrobiology (2016-2017) G. Vladilo May take place when a star-planet system crosses the visual of a background star, as a result of

### Spectroscopy, the Doppler Shift and Masses of Binary Stars

Doppler Shift At each point the emitter is at the center of a circular wavefront extending out from its present location. Spectroscopy, the Doppler Shift and Masses of Binary Stars http://apod.nasa.gov/apod/astropix.html

### From measuring and classifying the stars to understanding their physics

From measuring and classifying the stars to understanding their physics What we can measure directly: Surface temperature and color Spectrum Apparent magnitude or intensity Diameter of a few nearby stars

### ASTRONOMY 1 FINAL EXAM 1 Name

ASTRONOMY 1 FINAL EXAM 1 Name Multiple Choice (2 pts each) 1. Sullivan Star is an F spectral class star that is part of a binary star system. It has a MS lifetime of 5 billion years. Its life will eventually

### How Common Are Planets Around Other Stars? Transiting Exoplanets. Kailash C. Sahu Space Tel. Sci. Institute

How Common Are Planets Around Other Stars? Transiting Exoplanets Kailash C. Sahu Space Tel. Sci. Institute Earth as viewed by Voyager Zodiacal cloud "Pale blue dot" Look again at that dot. That's here.

### Finding Extrasolar Planets. I

ExtraSolar Planets Finding Extrasolar Planets. I Direct Searches Direct searches are difficult because stars are so bright. How Bright are Planets? Planets shine by reflected light. The amount reflected

### Chapter 10 Measuring the Stars

Chapter 10 Measuring the Stars Some of the topics included in this chapter Stellar parallax Distance to the stars Stellar motion Luminosity and apparent brightness of stars The magnitude scale Stellar

### Astronomy December, 2016 Introduction to Astronomy: The Solar System. Final exam. Practice questions for Unit V. Name (written legibly):

Astronomy 101 12 December, 2016 Introduction to Astronomy: The Solar System Final exam Practice questions for Unit V Name (written legibly): Honor Pledge: On my honor, I have neither given nor received

### Lecture Outlines. Chapter 15. Astronomy Today 7th Edition Chaisson/McMillan Pearson Education, Inc.

Lecture Outlines Chapter 15 Astronomy Today 7th Edition Chaisson/McMillan Chapter 15 The Formation of Planetary Systems Units of Chapter 15 15.1 Modeling Planet Formation 15.2 Terrestrial and Jovian Planets

### 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

### Importance of the study of extrasolar planets. Exoplanets Introduction. Importance of the study of extrasolar planets

Importance of the study of extrasolar planets Exoplanets Introduction Planets and Astrobiology (2017-2018) G. Vladilo Technological and scientific spin-offs Exoplanet observations are driving huge technological

### 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