The Search For Life in the Universe. Lecture 27
|
|
|
- Richard James
- 5 years ago
- Views:
Transcription
1 The Search For Life in the Universe Lecture 27
2 Our basic search technique: 1: Find the planets 2: Isolate the planets light from the stars light 3: Get a spectrum of the planet Its atmosphere, maybe is reflected surface light
3 4 basic techniques to find planets: 1: Transits 2: Radial Velocity 3: Microlensing 4: Direct imaging
4 Brown Dwarf + exo planet
5
6
7
8
9
10 One dip in the stars brightness is not sufficient to say that you have found a planet. Requires at least three dips, at a regular period. (Any two dips could still be random) So you need to stare at a star for a long time, and you need to be able to measure its brightness with great accuracy. Why does this mean that we need to do such a mission from space?
11
12
13 What does the transit method tell you about a planet? 1: Planets diameter compared to stellar diameter. Only gives the size of the planet if we know the size of the star. 2: Orbital period of the planet This tells us the size of the orbit if we know the mass of the star 3: Does not tell us the mass of the planet or the density of the planet But it does seem that big planets are gas giants and smaller planets are rocky
14
15
16
17 Kepler detector array: note the attempt to match the field curvature
18
19 Kepler Mirror
20 Kepler focal plane
21
22 Mission Operations at the University of Colorado (research park) 15/03/04/cu-boulder-students-help-controlinstruments-nasa-spacecraft-probemagnetic
23
24
25 105 square degrees Moon is about 3/16 square degrees
26
27
28
29
30
31
32 Radial velocity
33
34
35
36
37
38
39
40
41 2010 Transits: green M Earth Radial velocity: blue 1AU
42 October, 2013 Blue = Radial Velocity Green = Transits
43
44 What s next for radial velocity techniques? Need high precision. Want 10 cm/s accuracy (1 part in 3 Billion accuracy) Very difficult Would allow detection of Earths
45 Aspen Center for Physics Approaching the Stellar Astrophysical Limits of Exoplanet Detection: Getting to 10 cm/s
46
47 Direct Imaging of exoplanets
48
49
50
51
52
53
54
55
56
57
58
59
60
61
62 Sign of Life: BioMarkers or BioSignatures
63 BioMarkers are features in the spectrum of exo-planet that will indicate the presence of biological activity. The spectrum will tell us about atoms and molecules in the atmosphere, as well as the reflectance of the surface (whatever the starlight is reflecting off of).
64 Three fundamental BioMarkers 1: Reflected light from living organisms 2:Gases in atmosphere that we attribute to life 3: Inferred biology due to incompatible gasses in atmospheres
65 Detecting Life Remotely Pale Blue Dot Visible or IR radiation contain spectral fingerprint of planet s surface or atmosphere: look for BIOSIGNATURES Some slides from Nigel J Mason Physics & Astronomy, The Open University, UK.
66
67
68
69 Oxygen (either as O 2 or Ozone (O 3 ) Is considered a good bio-marker Oxygen is highly reactive it wants to bond with other materials (burn). The only known process to produce atmospheric oxygen on earth is photosynthesis
70 Methane (CH4) will react with oxygen The presence of both gasses indicates a continuing supply of both On earth, this is biology
71 Neptune has plenty of methane, but no oxygen: NO LIFE
72
73
74 Terrestrial exoplanets Magma Snowball Jurassic Early Mars Early Venus Jungleworld Desertworld Waterworld Superearth
75 Earth-in-Time Atmospheres Magma Hadean Archaean Proterozoic Snowball Atmospheric Composition Silicate CO 2 CO 2 N 2 N 2 Steam H 2 O N 2 O 2 CO 2 O 2
76 Factors affecting terrestrial atmospheres Size, Mass (gravity, pressure) Orbit (mean distance, eccentricity) Central star (spectral type) Atmospheric composition (greenhouse gases, photochemistry) Atmospheric mass (pressure) Ocean (hydrological cycle) Tectonics (volcanism, magnetism) Age (Photon flux, evolution) Biology (Emissions, CO 2 cycle...)
77 Archaean atmosphere 2.5 billion years ago CO 2 (x10,x100) CH 4 (x10) O 2 (x0.1, 0.01) UV (x100) T surface (30-80 o C) Photon flux = 83% modern Biomarker abundances?
78 Proterozoic atmosphere 2.2 billion years ago CO 2 (x5) CH 4 (x2, x5) O 2 (x0.1, 0.01) UV (x100) T surface (30-80 o C) Photon flux = ~90% modern Biomarker abundances? (O 3, N 2 O)
79 Snowball Earth atmosphere CO 2 (x10) CH 4 (x2) O 2 (x0.1, 0.01) UV (x100) Biomarker abundances? (O 3, N 2 O)
80 Jungleworld atmosphere High vegetation emissions High O 2 (21-35%) Biomarker abundances? (O 3, N 2 O)
81 Superearth atmosphere Earth composition P surface e.g. 1bar, 2bar Biomarker abundances? (O 3, N 2 O)
82
83 What do you conclude about this synthetic planet spectrum?
84 This is the real spectrum of Mars
85 It is proposed that these type of observations be made in the 2030 s
86 HDST
87 What would it take to convince you that we had found a planet bearing life?
88 What would it take to convince you that we had found a planet bearing life? What would it mean for you?
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:
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
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
ESA's Rosetta spacecraft What are habitable exoplanets? Is there an Earth 2.0?
ESA's Rosetta spacecraft - 2009 What are habitable exoplanets? Is there an Earth 2.0? Christina Hedges (Institute of Astronomy) For the past 20 years, since the discovery of planets outside our solar system,
Exam# 1 Review Gator 1 Keep the first page of the exam. Scores will be published using the exam number Chapter 0 Charting the Heavens
Exam# 1 Review Exam is Wednesday October 11 h at 10:40AM, room FLG 280 Bring Gator 1 ID card Bring pencil #2 (HB) with eraser. We provide the scantrons No use of calculator or any electronic device during
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
7. Our Solar System. Planetary Orbits to Scale. The Eight Planetary Orbits
7. Our Solar System Terrestrial & Jovian planets Seven large satellites [moons] Chemical composition of the planets Asteroids & comets The Terrestrial & Jovian Planets Four small terrestrial planets Like
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
The Search for Another Earth Part II
The Search for Another Earth Part II Sujan Sengupta In the first part, we discussed the various methods for the detection of planets outside the solar system known as the exoplanets. In this part, we will
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
Edmonds Community College Astronomy 100 Winter Quarter 2007 Sample Exam # 2
Edmonds Community College Astronomy 100 Winter Quarter 2007 Sample Exam # 2 Instructor: L. M. Khandro 1. Relatively speaking, objects with high temperatures emit their peak radiation in short wavelengths
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
Science Olympiad Astronomy C Division Event National Exam
Science Olympiad Astronomy C Division Event National Exam University of Nebraska-Lincoln May 15-16, 2015 Team Number: Team Name: Instructions: 1) Please turn in all materials at the end of the event. 2)
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
Planetary Atmospheres
Planetary Atmospheres Structure Composition Clouds Meteorology Photochemistry Atmospheric Escape EAS 4803/8803 - CP 11:1 Structure Generalized Hydrostatic Equilibrium P( z) = P( 0)e z # ( ) " dr / H r
Finding bio-signatures on extrasolar planets, how close are we?
Finding bio-signatures on extrasolar planets, how close are we? Enric Palle Instituto de Astrofisica de Canarias TMT Forum 2017, Mysore Exoplanet discoveries 3703 planets 2773 system 621 multiple Exoplanets:
Ast 281 Review for Exam 1 Tuesday, February 25, 2014 in class
Ast 281 Review for Exam 1 Tuesday, February 25, 2014 in class The Exam will be a CLOSED BOOK exam, lasting the whole period. You will be allowed to have calculators and the sheet of planetary data, but
The History of the Earth
The History of the Earth We have talked about how the universe and sun formed, but what about the planets and moons? Review: Origin of the Universe The universe began about 13.7 billion years ago The Big
Lecture 25: The Requirements for Life
Lecture 25: The Requirements for Life Astronomy 141 Winter 2012 This lecture explores the requirements for life, and the factors affecting planetary habitability. The basic requirements are a source of
Predicting the Extreme-UV and Lyman-α Fluxes Received by Exoplanets from their Host Stars
Predicting the Extreme-UV and Lyman-α Fluxes Received by Exoplanets from their Host Stars Jeffrey L. Linsky 1, Kevin France 2, Thomas Ayres 2 1 JILA, University of Colorado and NIST, Boulder, CO 80309-0440
Terrestrial Planet (and Life) Finder. AST 309 part 2: Extraterrestrial Life
Terrestrial Planet (and Life) Finder AST 309 part 2: Extraterrestrial Life The Drake Equation: N = N * f pl n hab f L f C f T L/T Stars? Planets? Habitable Origin Complex Intelligence, Lifetime planets?
Exoplanets Atmospheres. Characterization of planetary atmospheres. Photometry of planetary atmospheres from direct imaging
Photometry of planetary atmospheres from direct imaging Exoplanets Atmospheres Planets and Astrobiology (2016-2017) G. Vladilo Example: planetary system detected with direct imaging HR 8799 b, c, d (Marois
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
Hunting Habitable Shadows. Elizabeth Tasker
Hunting Habitable Shadows Elizabeth Tasker Saturn Earth Uranus Mercury Mars Jupiter Venus Neptune Saturn Earth Uranus Mercury Mars Jupiter Venus Neptune 2013 2012 2011 2010 2009 2008 2007 2006 2005 2004
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
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
RING DISCOVERED AROUND DWARF PLANET
RING DISCOVERED AROUND DWARF PLANET Haumea, a dwarf planet in the Kuiper Belt was just found to have a ring. Why? Hint: what causes the Jovian planet rings? Artist's conception, not a real photo RING DISCOVERED
ASTRO 120 Sample Exam
ASTRO 120 Sample Exam 1) If a planet has a reasonably strong magnetic field, we know that a. It is made entirely of iron b. There is liquid nitrogen below the surface c. It can harbor life d. It has a
Planetary Temperatures
Planetary Temperatures How does Sunlight heat a planet with no atmosphere? This is similar to our dust grain heating problem First pass: Consider a planet of radius a at a distance R from a star of luminosity
Planetary Atmospheres
Planetary Atmospheres Structure Composition Clouds Meteorology Photochemistry Atmospheric Escape EAS 4803/8803 - CP 17:1 Structure Generalized Hydrostatic Equilibrium P( z) = P( 0)e z # ( ) " dr / H r
N = R * f p n e f l f i f c L
Astronomy 230 Section 1 MWF 1400-1450 106 B6 Eng Hall This Class (Lecture 10): Nature of Life Next Class: Nucleic Acids Some Oral Presentation on Feb 16 th and 18 th! Mike Somers Chris Kramer Sarah Goldrich
AST 105 Intro Astronomy The Solar System
AST 105 Intro Astronomy The Solar System STRUCTURE OF A PLANET S ATMOSPHERE If you remember this. X-rays Ultraviolet Heating & Destruction Heating & Destruction Visible Infrared Transmission and Scattering
Planetary Atmospheres (Chapter 10)
Planetary Atmospheres (Chapter 10) Based on Chapter 10 This material will be useful for understanding Chapters 11 and 13 on Jovian planet systems and Extrasolar planets Chapters 4, 5, and 8 on Momentum,
see disks around new stars in Orion nebula where planets are probably being formed 3
Planet Formation contracting cloud forms stars swirling disk of material around forming star (H, He, C, O, heavier elements, molecules, dust ) form planets New born star heats up material, blows away solar
Astronomy 1001/1005 Midterm (200 points) Name:
Astronomy 1001/1005 Midterm (00 points) Name: Instructions: Mark your answers on this test AND your bubble sheet You will NOT get your bubble sheet back One page of notes and calculators are allowed Use
9.2 - Our Solar System
9.2 - Our Solar System Scientists describe our solar system as the Sun and all the planets and other celestial objects, such as moons, comets, and asteroids, that are held by the Sun s gravity and orbit
Radiative Balance and the Faint Young Sun Paradox
Radiative Balance and the Faint Young Sun Paradox Solar Irradiance Inverse Square Law Faint Young Sun Early Atmosphere Earth, Water, and Life 1. Water - essential medium for life. 2. Water - essential
PTYS 214 Spring Announcements. Get exam from Kyle!
PTYS 214 Spring 2018 Announcements Get exam from Kyle! 1 Midterm #3 Total Students: 24 Class Average: 78 Low: 32 High: 100 If you have questions see one of us! 2 All exams Top 2 exams 3 Previously Feedbacks
Adam Burrows, Princeton April 7, KITP Public Lecture
Adam Burrows, Princeton April 7, 2010 KITP Public Lecture The Ancient History of Comparative Planetology There are infinite worlds both like and unlike this world of ours...we must believe that in all
Exoplanet Detection and Characterization with Mid-Infrared Interferometry
Exoplanet Detection and Characterization with Mid-Infrared Interferometry Rachel Akeson NASA Exoplanet Science Institute With thanks to Peter Lawson for providing material Sagan Workshop July 21, 2009
The Ultraviolet Radiation Environment in the Habitable Zones Around Low-Mass Exoplanet Host Stars. Kevin France. University of Colorado at Boulder
The Ultraviolet Radiation Environment in the Habitable Zones Around Low-Mass Exoplanet Host Stars Kevin France University of Colorado at Boulder NUVA Challenges in UV Astronomy 07 October 2013 Co-authors
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
Astronomy 103: First Exam
Name: Astronomy 103: First Exam Stephen Lepp October 27, 2010 Each question is worth 2 points. Write your name on this exam and on the scantron. 1 Short Answer A. What is the largest of the terrestrial
The Solar System consists of
The Universe The Milky Way Galaxy, one of billions of other galaxies in the universe, contains about 400 billion stars and countless other objects. Why is it called the Milky Way? Welcome to your Solar
Coriolis Effect - the apparent curved paths of projectiles, winds, and ocean currents
Regents Earth Science Unit 5: Astronomy Models of the Universe Earliest models of the universe were based on the idea that the Sun, Moon, and planets all orbit the Earth models needed to explain how the
2/24/2014. Early Earth (Hadean) Early Earth. Terms. Chondrule Chondrite Hadean Big Bang Nucleosynthesis Fusion Supernova
Early (Hadean) Early Terms Chondrule Chondrite Hadean Big Bang Nucleosynthesis Fusion Supernova Hadean Time Nucleosynthesis The elements H, He, and traces of Li were formed in the original Big Bang. Latest
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 Collecting Area Light bucket : the bigger the area of the telescope s mirror or lens, the more photons
The Direct Study of Exoplanet Atmospheres
The Direct Study of Exoplanet Atmospheres David Charbonneau (Harvard-Smithsonian Center for Astrophysics) Symposium in Honor of Giovanni Fazio 27 May 2008 Statement about the Astronomy & Astrophysics 2010
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
2. Terrestrial Planet G 9. Coulomb Force C 16. Babcock model Q. 3. Continuous Spectrum K 10. Large-impact hypothesis I 17.
Astronomy 1 S 16 Exam 1 Name Identify terms Label each term with the appropriate letter of a definition listed 1. Spectral line R 8. Albedo H 15. helioseismology E 2. Terrestrial Planet G 9. Coulomb Force
Proxima Cen b: theoretical spectral signatures for different atmospheric scenarios
Proxima Cen b: theoretical spectral signatures for different atmospheric scenarios A. Léger(1), D. Defrère(2), J.L. Grenfell(3), M. Godolt(3), A Garcia Munoz(3), H. Rauer(3), and F. Tian(4) (1) University
Astronomy. physics.wm.edu/~hancock/171/ A. Dayle Hancock. Small 239. Office hours: MTWR 10-11am
Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am Planetology II Key characteristics Chemical elements and planet size Radioactive dating Solar system formation Solar nebula
Exploring Spectra. Origins: Where Are the Aliens? Overhead. The Sun s Spectrum. Continuum. Intensity Absorption Line
Origins: Where Are the Aliens? Overhead Exploring Spectra Both of the following show the visible-light absorption spectrum for our sun. Notice that the second graph reveals more information the amount
The Sun and Planets Lecture Notes 6.
The Sun and Planets Lecture Notes 6. Lecture 6 Venus 1 Spring Semester 2017 Prof Dr Ravit Helled Cover photo: Venus in true color (Courtesy of NASA) Venus Properties Venus is the second brightest natural
Complexity of the climate system: the problem of the time scales. Climate models and planetary habitability
Complexity of the climate system: the problem of the time scales Climate models and planetary habitability Time scales of different components of the climate system Planets and Astrobiology (2016-2017)
Foundations of Astrophysics
Foundations of Astrophysics Barbara Ryden The Ohio State University Bradley M. Peterson The Ohio State University Preface xi 1 Early Astronomy 1 1.1 The Celestial Sphere 1 1.2 Coordinate Systems on a Sphere
Beyond the Book. FOCUS Book
FOCUS Book At the bottom of page 4 is an example of a transit graph. A transit graph shows changes in the brightness of a star s light as a planet crosses in front of the star as seen from Earth. Suppose
UNIT 3: Chapter 8: The Solar System (pages )
CORNELL NOTES Directions: You must create a minimum of 5 questions in this column per page (average). Use these to study your notes and prepare for tests and quizzes. Notes will be turned in to your teacher
Grades 9-12: Earth Sciences
Grades 9-12: Earth Sciences Earth Sciences...1 Earth s Place in the Universe...1 Dynamic Earth Processes...2 Energy in the Earth System...2 Biogeochemical cycles...4 Structure and Composition of the Atmosphere...4
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.
ASTR 200 : Lecture 6 Introduction to the Solar System Pearson Education Inc., publishing as Addison-Wesley
ASTR 200 : Lecture 6 Introduction to the Solar System 1 2004 Pearson Education Inc., publishing as Addison-Wesley Comparative Planetology Studying the similarities among and differences between the planets
Edmonds Community College ASTRONOMY 100 Sample Test #2 Fall Quarter 2006
Edmonds Community College ASTRONOMY 100 Sample Test #2 Fall Quarter 2006 Instructor: L. M. Khandro 10/19/06 Please Note: the following test derives from a course and text that covers the entire topic of
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
EART164: PLANETARY ATMOSPHERES
EART164: PLANETARY ATMOSPHERES Francis Nimmo Last Week - Dynamics Reynolds number, turbulent vs. laminar flow Velocity fluctuations, Kolmogorov cascade Brunt-Vaisala frequency, gravity waves Rossby waves,
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
Helmut Lammer Austrian Academy of Sciences, Space Research Institute Schmiedlstr. 6, A-8042 Graz, Austria (
The search of habitable Earth-like exoplanets Helmut Lammer Austrian Academy of Sciences, Space Research Institute Schmiedlstr. 6, A-8042 Graz, Austria (email: helmut.lammer@oeaw.ac.at) Graz in Space 2008
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-
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
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
Universe Celestial Object Galaxy Solar System
ASTRONOMY Universe- Includes all known matter (everything). Celestial Object Any object outside or above Earth s atmosphere. Galaxy- A large group (billions) of stars (held together by gravity). Our galaxy
Lecture 20. Origin of the atmosphere (Chap. 10) The carbon cycle and long-term climate (Chap. 8 of the textbook: p )
Lecture 20 Origin of the atmosphere (Chap. 10) The carbon cycle and long-term climate (Chap. 8 of the textbook: p.158-170) end of last ice-age; begin civilization beginning of modern era of ice-ages asteroid
Astronomy Today. Eighth edition. Eric Chaisson Steve McMillan
Global edition Astronomy Today Eighth edition Eric Chaisson Steve McMillan The Distance Scale ~1 Gpc Velocity L Distance Hubble s law Supernovae ~200 Mpc Time Tully-Fisher ~25 Mpc ~10,000 pc Time Variable
Planets are plentiful
Extra-Solar Planets Planets are plentiful The first planet orbiting another Sun-like star was discovered in 1995. We now know of 209 (Feb 07). Including several stars with more than one planet - true planetary
The Kepler Exoplanet Survey: Instrumentation, Performance and Results
The Kepler Exoplanet Survey: Instrumentation, Performance and Results Thomas N. Gautier, Kepler Project Scientist Jet Propulsion Laboratory California Institute of Technology 3 July 2012 SAO STScI 2012
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
Evolution of the Atmosphere: The Biological Connection
Evolution of the Atmosphere: The Biological Connection The Earth s Four Spheres How It All Began Or At Least How We Think It Began O.k. it s a good guess Egg of energy The Big Bang splattered radiation
Earth! Objectives: Interior and plate tectonics Atmosphere and greenhouse effect
Earth! Objectives: Interior and plate tectonics Atmosphere and greenhouse effect Earth Fun Facts 1. Only body with liquid water on the surface. 2. Most massive terrestrial body in solar system 3. Only
AST 205. Lecture 22. December 3, 2003 Remote Sensing of Spectroscopic and Photometric Biomarkers. Assignments for week of Dec 8
AST 205. Lecture 22. December 3, 2003 Remote Sensing of Spectroscopic and Photometric Biomarkers Your homework and mine (continental drift/plate tectonics history) The NASA Terrestrial Planet Finder (TPF)
Earth s Formation Unit [Astronomy] Student Success Sheets (SSS)
![Earth s Formation Unit [Astronomy] Student Success Sheets (SSS)](/thumbs/77/76655554.jpg "Earth s Formation Unit [Astronomy] Student Success Sheets (SSS)")
Page1 Earth s Formation Unit [Astronomy] Student Success Sheets (SSS) HS-ESSI-1; HS-ESS1-2; HS-ESS1-3; HS-ESSI-4 NGSS Civic Memorial High School - Earth Science A Concept # What we will be learning Mandatory
Comparative Planetology I: Our Solar System. Chapter Seven
Comparative Planetology I: Our Solar System Chapter Seven ASTR 111 003 Fall 2006 Lecture 07 Oct. 16, 2006 Introduction To Modern Astronomy I Introducing Astronomy (chap. 1-6) Planets and Moons (chap. 7-17)
ESS15 Lecture 7. The Greenhouse effect.
ESS15 Lecture 7 The Greenhouse effect. Housekeeping. First midterm is in one week. Open book, open notes. Covers material through end of Friday s lecture Including today s lecture (greenhouse effect) And
The Earth and Its Atmosphere: 1.Chemical composition and 2. Vertical structure
The Earth and Its Atmosphere: 1.Chemical composition and 2. Vertical structure RECAP Definition of an atmosphere: the gas surrounding a planet/satellite/comet/ Origin of the atmosphere. Three stages: I
Astronomy 1140 Quiz 4 Review
Astronomy 1140 Quiz 4 Review Anil Pradhan December 6, 2016 I The Outer Planets in General 1. How do the sizes, masses and densities of the outer planets compare with the inner planets? The outer planets
Chapter 4! Search for habitable environments, biomarkers and life outside the Earth!
Introduction to Astrobiology! Chapter 4! Search for habitable environments, biomarkers and life outside the Earth! The Solar System! Search for habitable environments and life! Venus! T s =735 K! Examples
Observing Habitable Environments Light & Radiation
Homework 1 Due Thurs 1/14 Observing Habitable Environments Light & Radiation Given what we know about the origin of life on Earth, how would you recognize life on another world? Would this require a physical
The Galactic Exoplanet Survey Telescope (GEST)
The Galactic Exoplanet Survey Telescope (GEST) D. Bennett (Notre Dame), J. Bally (Colorado), I. Bond (Auckland), E. Cheng (GSFC), K. Cook (LLNL), D. Deming, (GSFC) P. Garnavich (Notre Dame), K. Griest
Chapter 11 Review Clickers. The Cosmic Perspective Seventh Edition. Jovian Planet Systems Pearson Education, Inc.
Review Clickers The Cosmic Perspective Seventh Edition Jovian Planet Systems If Jupiter was the size of a basketball, Earth would be the size of a(n) a) bacterium. b) grain of rice. c) marble. d) orange.
5. How did Copernicus s model solve the problem of some planets moving backwards?
MODELS OF THE SOLAR SYSTEM Reading Guide: Chapter 27.2 (read text pages 691-694) 1k. Recognize the cumulative nature of scientific evidence. 1n. Know that when an observation does not agree with an accepted
http://eps.mcgill.ca/~courses/c201_winter/ http://eps.mcgill.ca/~courses/c201_winter/ Neutron Proton Nucleosynthesis neutron!! electron!+!proton!!=!!é!!+!h +!! t 1/2 =!12!minutes H + +!neutron!! Deuterium!(D)
Today. Events. Terrestrial Planet Geology - Earth. Terrestrial Planet Atmospheres. Homework DUE next time
Today Terrestrial Planet Geology - Earth Terrestrial Planet Atmospheres Events Homework DUE next time Ring of Fire Boundaries of plates traced by Earthquakes and Volcanos Plate Motions Measurements of
Observational Astronomy - Lecture 6 Solar System I - The Planets
Observational Astronomy - Lecture 6 Solar System I - The Planets Craig Lage New York University - Department of Physics craig.lage@nyu.edu March 23, 2014 1 / 39 The Sun and the Earth The Sun is 23,000
Silicate Atmospheres, Clouds, and Fractional Vaporization of Hot Earth-like Exoplanets
Silicate Atmospheres, Clouds, and Fractional Vaporization of Hot Earth-like Exoplanets Laura Schaefer and Bruce Fegley, Jr. Planetary Chemistry Laboratory Department of Earth and Planetary Sciences Washington
Our Sun. The centre of our solar system
Our Sun The centre of our solar system Nicolaus Copernicus Our Sun The sun represents 99.86% of the mass in our solar system. It is ¾ hydrogen and ¼ helium. More than 1 million Earths can fit inside the
Chapter One. Introduction 1.1 EXOPLANETS FROM AFAR
Chapter One Introduction 1.1 EXOPLANETS FROM AFAR The search for our place in the cosmos has fascinated human beings for thousands of years. For the first time in human history we have technological capabilities
You are here! The Solar System! Jo-Anne Brown
You are here! * The Solar System! Jo-Anne Brown Outline Questions! Earth, Moon, Sun A little, teeny, tiny bit of history... Terrestrial planets Gas Giants Poor Pluto Magnetic fields Tell me what you know!
Module 4: Astronomy The Solar System Topic 3 Content: The Terrestrial Planets Notes Introduction
Introduction The four planets closest to the Sun are called "the terrestrial planets." These inner planets are considered to be small and rocky. Although they are all rocky, their varying distances from
PTYS 214 Spring Announcements. Midterm 3 next Thursday!
PTYS 214 Spring 2018 Announcements Midterm 3 next Thursday! 1 Previously Habitable Zone Energy Balance Emission Temperature Greenhouse Effect Vibration/rotation bands 2 Recap: Greenhouse gases In order
How does your eye form an Refraction
Astronomical Instruments Eyes and Cameras: Everyday Light Sensors How does your eye form an image? How do we record images? How does your eye form an image? Refraction Refraction is the bending of light
MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
ASTRO 102/104 Prelim 2 Name Section MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) This is version E of the exam. Please fill in (E). A) This
Meteorites. A Variety of Meteorite Types. Ages and Compositions of Meteorites. Meteorite Classification
Meteorites A meteor that survives its fall through the atmosphere is called a meteorite Hundreds fall on the Earth every year Meteorites do not come from comets First documented case in modern times was