Statistics on Venus: Craters and Catastrophes (?) Steven A. Hauck, II
|
|
- Morris Bradley
- 5 years ago
- Views:
Transcription
1 Statistics on Venus: Craters and Catastrophes (?) Steven A. Hauck, II Department of Terrestrial Magnetism Carnegie Institution of Washington
2 Acknowledgements Roger Phillips Washington University Maribeth Price South Dakota School of Mines and Technology Sean Solomon Carnegie Institution of Washington
3 The big question What does it mean for the evolution of a planet if the spatial distribution of impact craters on its surface cannot be distinguished from a completely spatially random distribution?
4 Outline Why Venus? Why impact craters? Dating with craters. Geology in brief. Monte Carlo models and statistical tests. Implications for Venus.
5 The Basics 2 nd planet from Sun Mean radius = 6052 km ( = 6371 km) Mean density = 5243 kg/m 3 ( = 5515 kg/m 3 ) 1 Venus year = 225 days 1 Venus day = 243 days (retrograde) Surface pressure = 91 atmospheres Surface temperature = 740 K
6
7
8 Magellan SAR Mosaic of Venus
9
10 Why study impact craters?
11
12 50 km
13 Motivation Can we learn something about the history of Venus from the distribution of impact craters on the surface?
14 Relevance Surface history places a constraint on the evolution of the whole planet. Ultimately provides a contrast to the Earth which is comparable in size and presumably composition.
15 Venusian Impact Craters
16 Martian Impact Craters Craters > 4km from Barlow database over Mars shaded relief from MOLA
17 Terrestrial Impact Craters Space Imagery Center:
18 Craters Surface Ages 1) Assume the rate of impact crater formation is approximately constant (only to first-order) The rate has an impact size-dependence 2) Assume that cratering process is spatially and temporally random 3) Divide the surface into units based upon geologic criteria (e.g., morphology, superposition relationships) 4) Calculate area density of points (craters) within units 5) Relative differences give relative ages Convert to absolute age if an estimate of mean surface age is available
19 Absolute Ages Calibration points: Earth and moon Other bodies? Assumption that Mars, Venus, and Mercury have some multiple of the lunar impactor population Comparison of present day minor planets with (asteroids) known oribital elements with planetary orbits Uncertainty abounds Venus has the additional problem of its thick atmosphere
20 Crater Ages Production Age: Number of craters superposed on a geologic unit reflect the time since the unit was emplaced. Retention Age: Number of craters within a geologic unit reflect a competition between crater emplacement and removal.
21 More Background ~1000 impact craters on the surface Early analysis showed that the spatial distribution of impact craters cannot be distinguished from one that is completely spatially random [CSR] Most craters appear pristine. Dense atmosphere has a profound filtering effect Surface mean crater production age ~750 Myr Refs: Phillips et al., 1992; Schaber et al., 1992; Herrick and Phillips, 1994; McKinnon et al., 1997
22 Venusian Impact Craters
23 The big question What does it mean for the evolution of a planet if the spatial distribution of impact craters on its surface cannot be distinguished from a completely spatially random distribution?
24 Early Models Based on the notion that Venus impact craters are randomly distributed, two end-member models were proposed : The equilibrium resurfacing model (ERM) [Phillips et al., 1992] The catastrophic resurfacing model (CRM CRM) [Phillips et al., 1992; Schaber et al., 1992; Bullock et al., 1993; Strom et al., 1994]
25 Large-scale Geology Distinct morphologic units can be defined at the 1:8,000,000 scale (C1-MIDR). [Price and Suppe, 1994, 1995; Tanaka et al., 1997] The volcanic plains are the areally most extensive unit covering ~65% of the planetary surface. Plains can be divided into sub-units based upon dominant flow morphology and radar brightness. [Price, 1995; Tanaka et al., 1997]
26 SAR Images of Type PL1 and PS PL1 PS 100 km 200 km
27 Venusian Plains Units N 0 0 PL1 PL2 PL3 PS Impact Crater 45 S Plains units after Price [1995]
28 Age of the Plains Unit Area Craters Relative Age Estimated Age (Ma) PL ± 0.36 T 589 ± 270 PL ± 0.14 T 649 ± 106 PL ± 0.16 T 857 ± 116 PS ± 0.16 T 983 ± 120 PL1+PL ± 0.13 T 641 ± 99 PL3+PS ± 0.11 T 923 ± 84 SAP ± 0.09 T 829 ± 65 A unit of area is 10 6 km 2. Errors listed are 2σ. Note that both PL2 and PL1+PL2 have relative ages that do not overlap within 2σ of the single-age plains (SAP) model, suggesting that the younger plains have distinct ages that are statistically significant. The mean surface production age, used to calculate the last column, is estimated as T = 750 Ma [McKinnon et al., 1997].
29 Modeling > 200 Monte Carlo simulations Density of craters within a unit prescribed Modeling done with ArcView GIS Results post-processed to measure distances to all neighbors Mean distances to nearest neighbors compared to Venus observations using Mth nearest neighbor analysis.
30 Resurfacing Models Nominal MB1 MB2 SAP DAP DAP2 TAP Each unit has the observed age PL3-2σ, PS+2σ PL2-2σ, PS+1.5σ Single age for all plains units Combine young and old units as PL1+PL2 and PL3+PS DAP young + 2σ, DAP old - 2σ Divide units as PL1, PL2, and PL3+PS
31 Model
32 QQ and PP Plots QQ Plot of Venus Resurfacing Model with UnitsofDistinctCraterProductionAges PP Plot of Venus Resurfacing Model with Units of Distinct Crater Production Ages Observed [Deg] ExpectedDistance [Deg] Observed Distance [Deg/Deg] Expected Distance [Deg/Deg]
33 Tests Distance based Nearest Neighbor Analysis (and M th Nearest Neighbor ) compare mean distance from each crater to the 1 st,2 nd,,m th nearest neighbor to the expected distance. Density based Binomial probability probability of finding the number of craters that are observed in each unit if the hypothesis that distribution of craters in the plains is controlled only by a single random process is true. Chi-squared goodness-of-fit test compare the observed number of craters in each plains unit to the number expected by a particular model.
34 Two-sided p values of Testing the Hypothesis that Plains Resurfacing Models Represent Venus 1.0 p value Nominal MB 1 MB 2 SAP DAP DAP 2 TAP CSR CSR vs. Random M th Nearest Neighbor
35 Statistical Results Binomial Probability Unit P PL1 1.7 x 10-1 PL2 3.0 x 10-2 PL3 1.3 x 10-2 PS 4.5 x 10-7 PL1+PL2 1.4 x 10-2 PL3+PS 6.5 x SAP 4.2 x 10-6 Chi-squared goodness-of-fit Model P SAP 2.0 x 10-4 DAP 4.9 x 10-1 TAP 5.2 x 10-1 CRM 4.0 x 10-6
36 Results M th Nearest Neighbor Analysis None of the models presented (including a CSR population) can be distinguished from Venus crater distribution. Binomial probability The hypothesis that variations in the crater distribution are due to a single random process for the planet can be rejected for all units except PL1. Chi-squared goodness-of-fit test It is extremely unlikely that a SAP or CRM could result in the observed number of craters in each plains unit. Dual- or tri-age plains models cannot be rejected.
37 Conclusions CSR cannot be used as a constraint on resurfacing or geodynamic models because it is a non-unique interpretation of the crater distribution. None of the resurfacing models can be rejected as being representative of Venus based upon M th nearest neighbor analysis. Chi-squared test on crater populations within the plains units suggests that both the single-age plains and single-age planet (CSR) models can be rejected as being representative of Venus.
38 Conclusions II Binomial probability tests on plains crater populations suggest that the sub-unit ages are significant. The spread in plains ages on the order of one-half the mean production age of the surface is significant and suggests that Venus has been geologically active more recently than believed in the past. Hypotheses such as CRM and episodic resurfacing [Turcotte, 1993;1995] are unnecessary to explain the crater distribution of Venus.
39 50 km
VENUS RESURFACING RATES: CONSTRAINTS PROVIDED BY 3-D MONTE CARLO SIMULATIONS. Mark A. Bullock and David H. Grinspoon. LASP, University of Colorado
1 VENUS RESURFACING RATES: CONSTRAINTS PROVIDED BY 3-D MONTE CARLO SIMULATIONS Mark A. Bullock and David H. Grinspoon LASP, University of Colorado James W. Head, III Department of Geological Sciences,
More informationAssignment 2. Due March 4, 2019
Assignment 2 Due March 4, 2019 Show all work and turn in answers on separate pages, not on these pages. Circle your final answers for clarity. Be sure to show/explain all of your reasoning and that your
More informationAssignment 4. Due TBD
Assignment 4 Due TBD Show all work and turn in answers on separate pages, not on these pages. Circle your final answers for clarity. Be sure to show/explain all of your reasoning and that your work is
More informationDifferentiation of planetary interiors. Rocky Planets Interiors and surface geophysics
Differentiation of planetary interiors Rocky Planets Interiors and surface geophysics Process of separation of internal planetary layers that takes place as a result of the physical and chemical properties
More informationImpact Age Dating. ASTRO 202 Lecture Thursday, February 14, Review. What is relative age dating? What is relative age dating?
Review Impact Age Dating ASTRO 202 Lecture Thursday, February 14, 2008 Carbon-14, Potassium-Argon isotopic age determination: (1) Parent decays to daughter at some predictable rate (2) How much now? (3)
More informationVenus. Venus. (The most visited planet) Orbit, Rotation Atmosphere. Surface Features Interior. (Greenhouse effect) Mariner 10 image
Venus Orbit, Rotation Atmosphere (Greenhouse effect) Surface Features Interior Mariner 10 image Venus (The most visited planet) Mariner 2 (1962) Mariner 5 (1967) Mariner 10 (1974) Poineer Venus (1978)
More informationASTR 380 Possibilities for Life in the Inner Solar System
ASTR 380 Possibilities for Life in the Inner Solar System ASTR 380 Midterm Test Results Generally people did well: 100-90 = A = 19 people 89 80 = B = 19 people 79 70 = C = 9 people 69 60 = D = 0 < 60 =
More informationLearning Objectives. they differ in density (composition, core), atmosphere, surface age, size, geological activity, magnetic field?
Mercury and Venus Learning Objectives! Contrast the Earth, the Moon, Venus and Mercury. Do they differ in density (composition, core), atmosphere, surface age, size, geological activity, magnetic field?!
More informationLecture #10: Plan. The Moon Terrestrial Planets
Lecture #10: Plan The Moon Terrestrial Planets Both Sides of the Moon Moon: Direct Exploration Moon: Direct Exploration Moon: Direct Exploration Apollo Landing Sites Moon: Apollo Program Magnificent desolation
More informationMercury and Venus 3/20/07
Announcements Reading Assignment Chapter 13 4 th Homework due today Quiz on Thursday (3/22) Will cover all material since the last exam. This is Chapters 9-12 and the part of 13 covered in the lecture
More informationLunar Geology ASTR 2120 Sarazin
Lunar Geology ASTR 2120 Sarazin Interior of the Moon Density low (3.3 gm/cc), very little iron No iron core Very small heat flow out of interior Little radioactive heating No magnetic field No molten iron
More information2) Elucidate a weakness of two of the lines of evidence you listed in the previous question.
GEO 110 Final Test May 30 2003 Name: IMPORTANT: Please write legibly!!! Short Answer (2 points each) 1) List three of the four lines of evidence that the Johnson Space Center team presented as evidence
More informationImportance of Solar System Objects discussed thus far. Interiors of Terrestrial Planets. The Terrestrial Planets
Importance of Solar System Objects discussed thus far Interiors of Terrestrial Planets Chapter 9 Sun: Major source of heat for the surfaces of planets Asteroids: Provide possible insight to the composition
More informationIntroduction to Astronomy
Introduction to Astronomy AST0111-3 (Astronomía) Semester 2014B Prof. Thomas H. Puzia Venus Venus The atmosphere of Venus is very dense and an opaque layer of clouds covers the planet, such that we cannot
More informationChapter 9. ASTRONOMY 202 Spring 2007: Solar System Exploration. Class 27: Planetary Geology [3/26/07] Announcements.
ASTRONOMY 202 Spring 2007: Solar System Exploration Instructor: Dr. David Alexander Web-site: www.ruf.rice.edu/~dalex/astr202_s07 Class 27: Planetary Geology [3/26/07] Announcements Planetary Geology Planetary
More informationRADAR REMOTE SENSING OF PLANETARY SURFACES
RADAR REMOTE SENSING OF PLANETARY SURFACES BRUCE A. CAMPBELL Smithsonian Institution CAMBRIDGE UNIVERSITY PRESS Contents Acknowledgments page ix 1 Introduction 1 1.1 Radar remote sensing 1 1.2 Historical
More informationAstro 210 Lecture 19 October 8, 2010
Astro 210 Lecture 19 October 8, 2010 Announcements Remember me? HW 5 due HW 6 available, due in class next Friday Night Observing continues next week Last time: The Moon Q: from Earth we only see one side
More informationDetermining Venusian Lithospheric Thickness using Frequency-Length Statistics of Fractures
Determining Venusian Lithospheric Thickness using Frequency-Length Statistics of Fractures Alyssa M. Beach California State University, Fullerton, Department of Geological Sciences May 2005 ABTRACT Frequency-length
More informationNext opportunity to observe the Moon and Venus close together: Dec. 31, Announcements
Announcements Last OWL homework: due 12/15 before midnight Study guide for final exam is up on the class webpage Practice exam up Thursday afternoon Final exam: Monday, Dec. 15, 10:30 AM, Hasbrouck 20
More informationA geologic process An erosional force A chronological tool An influence on biology
Impact Cratering: Physics and Chronology A geologic process An erosional force A chronological tool An influence on biology Impact features are common All solar system bodies with solid surfaces show evidence
More informationLecture Outlines. Chapter 9. Astronomy Today 7th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 9 Astronomy Today 7th Edition Chaisson/McMillan Chapter 9 Venus Units of Chapter 9 9.1 Orbital Properties 9.2 Physical Properties 9.3 Long-Distance Observations of Venus 9.4 The
More information10/24/2010. Venus Roman goddess of love. Bulk Properties. Summary. Venus is easier to observe than Mercury! Venus and Earth
Venus Roman goddess of love Birth of Venus Botticelli (1485) Bulk Properties Summary 1. Venus is 28% closer to the Sun having an orbital period of 225 Earth days 2. Venus is roughly 95% the size, 82% the
More informationKEY. Planetary Sciences Section 2 Midterm Examination #2 9:30-10:45 a.m., Tuesday, October 8, 2013
KEY Planetary Sciences 206 -- Section 2 Midterm Examination #2 9:30-10:45 a.m., Tuesday, October 8, 2013 INSTRUCTIONS: There are 35 multiple-choice questions, which are worth 2 points each. The last two
More informationGEOLOGY 12 CHAPTER 22 WORKSHEET COMPARATIVE PLANETOLOGY INTRODUCTION (VIDEO) Name
GEOLOGY 12 CHAPTER 22 WORKSHEET COMPARATIVE PLANETOLOGY Name References: Video: Overview of the Solar System (Standard Deviants 30 minutes) Text: pages 165-167 and 475-501 CDROM (Library): Exploring the
More informationTectonics. Planets, Moons & Rings 9/11/13 movements of the planet s crust
Tectonics Planets, Moons & Rings 9/11/13 movements of the planet s crust Planetary History Planets formed HOT Denser materials fall to center Planet cools by conduction, convection, radiation to space
More informationIntroduction. Background
Introduction In introducing our research on mars we have asked the question: Is there a correlation between the width of an impact crater and the depth of that crater? This will lead to answering the question:
More informationMapping the Surface of Mars Prelab. 1. Explain in your own words what you think a "geologic history" for a planet or moon is?
Prelab 1. Explain in your own words what you think a "geologic history" for a planet or moon is? 2. Describe some of the major features seen on the Martian surface by various spacecraft missions over the
More information3. The name of a particularly large member of the asteroid belt is A) Halley B) Charon C) Eris D) Ceres E) Triton
Summer 2013 Astronomy - Test 2 Test form A Name Do not forget to write your name and fill in the bubbles with your student number, and fill in test form A on the answer sheet. Write your name above as
More informationThe Moon. Tides. Tides. Mass = 7.4 x 1025 g = MEarth. = 0.27 REarth. (Earth 5.5 g/cm3) Gravity = 1/6 that of Earth
The Moon Mass = 7.4 x 1025 g = 0.012 MEarth Radius = 1738 km = 0.27 REarth Density = 3.3 g/cm3 (Earth 5.5 g/cm3) Gravity = 1/6 that of Earth Dark side of the moon We always see the same face of the Moon.
More informationGeologic history of the Mead impact basin, Venus
Geologic history of the Mead impact basin, Venus Robert R. Herrick Virgil L. Sharpton Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas 77058 ABSTRACT The geologic history of the Mead
More informationThe Tectonics of Venus and Creation
In A. A. Snelling (Ed.) (28). Proceedings of the Sixth International Conference on Creationism (pp. 25 212). Pittsburgh, PA: Creation Science Fellowship and Dallas, TX: Institute for Creation Research.
More informationMULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Chapter 4 - Group Homework Name MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) Density is defined as A) mass times weight. B) mass per unit volume.
More informationImpact Craters and Venus Resurfacing History
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 97, NO. El0, PAGES 15,923-15,948, OCTOBER 25, 1992 Impact Craters and Venus Resurfacing History ROGER J. PHILLIPS, 1'2 RICHARD F. RAUBERTAS, 3 RAYMOND E. ARVIDSON,
More informationVenus: Key Ideas: A Warm Up Exercise. Venus at a Glance -- Orbit. Venus at a Glance Planetary Data
Venus A Warm Up Exercise Because Mercury has a high average density despite its relatively low mass, it is thought to a) Have a subsurface ocean b) Have a large iron core c) Be made largely of lead d)
More informationLecture #11: Plan. Terrestrial Planets (cont d) Jovian Planets
Lecture #11: Plan Terrestrial Planets (cont d) Jovian Planets Mercury (review) Density = 5.4 kg / liter.. ~ Earth s Rocky mantle + iron/nickel core Slow spin: 59 days (orbital period = 88 days) No satellites
More informationName Class Date. Chapter 29. The Solar System. Review Choose the best response. Write the letter of that choice in the space provided.
The Solar System Review Choose the best response. Write the letter of that choice in the space provided. 1. Ptolemy modified Aristotle s model of the universe to include a. Oort clouds. b. retrograde motion.
More informationVenus - Overview. Exploration of Venus. Admin. 9/26/17. Second planet from Sun Earth s sister planet
Admin. 9/26/17 1. Class website http://www.astro.ufl.edu/~jt/teaching/ast1002/ 2. Optional Discussion sections: Tue. ~11.30am (period 5), Bryant 3; Thur. ~12.35pm (end of period 5 and period 6), start
More informationLecture Outlines. Chapter 6. Astronomy Today 7th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 6 Astronomy Today 7th Edition Chaisson/McMillan Chapter 6 The Solar System Units of Chapter 6 6.1 An Inventory of the Solar System 6.2 Measuring the Planets 6.3 The Overall Layout
More informationSUPPLEMENTARY INFORMATION
doi:10.1038/nature12280 Figure S1. The map shows the crater density (for craters larger than 25 km in diameter, N(25), per 10 6 km 2 ) on Mercury calculated in a moving neighborhood of radius 500 km, updated
More informationPart 1: the terrestrial planets
Mercury close up Part 1: the terrestrial planets The weird day on Mercury Weirdness is due to the fact that the rota:on period is comparable to period of revolu:on, and that they are related by the ra:o
More informationVenus: Analysis of the degree of impact crater deposit degradation and assessment of its use for dating geological units and features
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 107, NO. E8, 10.1029/2001JE001584, 2002 Venus: Analysis of the degree of impact crater deposit degradation and assessment of its use for dating geological units and
More informationSOLAR SYSTEM EXAMPLE EXAM B DIVISION
SOLAR SYSTEM EXAMPLE EXAM B DIVISION 2017-2018 TEAM NUMBER: TEAM NAME: STUDENT NAMES: Do not open the test packet until instructed by the event supervisor. Ensure that you have all 6 pages of the test,
More informationPresentation given to computer science undergraduate students at the University of Houston July 2007
Presentation given to computer science undergraduate students at the University of Houston July 2007 Machine Learning and Data Mining in Mars Tomasz F. Stepinski Lunar and Planetary Institute MARS/EARTH
More informationOur Created Solar System Video
Our Created Solar System Video After the first segment of the video (0:00 8:54 min.) is played, the video will be stopped. Then, answer the following questions: 1) In short, what is the solar system? 2)
More informationInner Planets (Part II)
Inner Planets (Part II) Sept. 18, 2002 1) Atmospheres 2) Greenhouse Effect 3) Mercury 4) Venus 5) Mars 6) Moon Announcements Due to technical difficulties, Monday s quiz doesn t count An extra credit problem
More informationof equilibrium radionuclides : Is out of 69 marks total transit on Wednesday Nov 8.
Lab Announcements 4 starts next week Assignment 3 due Wednesday Nov. 8 Office hours: Tomorrow 2:30 3:30 in my office Tuesday: (see web page). Henn 312 (back room) Discussion Midterm of equilibrium radionuclides
More informationModule 2 Educator s Guide Investigation 3. Figure 3. Figure 4
Figure 3 Figure 4 4 Figure 5 Figure 6 5 Figure 7 Figure 8 6 Figure 9 Figure 10 7 Figure 11 Figure 12 8 Module 2, Investigation 3: Briefing What similar physical processes occur on both Earth and Mars?
More informationWelcome to Class 12: Mars Geology & History. Remember: sit only in the first 10 rows of the room
Welcome to Class 12: Mars Geology & History Remember: sit only in the first 10 rows of the room What are we going to discuss today? How easily could humans live on Mars? Is there water on Mars? PRS: If
More informationAsteroids, Comets and NEOs. (Answers) Solar System Impacts. Author: Sarah Roberts
Asteroids, Comets and NEOs (Answers) Author: Sarah Roberts Asteroids, Comets and NEOs - Impact craters on the Earth 1. Using the data given below for real impact craters on the Earth, investigate the effect
More informationAstronomy Test Review. 3 rd Grade
Astronomy Test Review 3 rd Grade Match the vocabulary word to its definition. Outer Planets The path a planet takes around the sun. Inner Planets Orbit Sun The center of our solar system. Small, rocky
More informationProblem Set 3: Crater Counting
Problem Set 3: Crater Counting Introduction Impact craters are the dominant landforms on most of the solid surfaces in our solar system. These impact craters have formed on the surfaces over the 4.6 billion
More informationA Computational Model of Mars Craters-Size Frequency Distribution
Proceeding of The National Conference On Undergraduate Research (NCUR) 2006 The University of North Carolina at Asheville Asheville, North Carolina April 6 8, 2006 A Computational Model of Mars Craters-Size
More informationIn-situ geochronology General overview
In-situ geochronology General overview Timothy D. Swindle, University of Arizona, Tucson AZ F. Scott Anderson, Southwest Research Institute, Boulder CO October 26, 2009 Decadal Survey Inner Planets Panel
More informationExamining the Terrestrial Planets (Chapter 20)
GEOLOGY 306 Laboratory Instructor: TERRY J. BOROUGHS NAME: Examining the Terrestrial Planets (Chapter 20) For this assignment you will require: a calculator, colored pencils, a metric ruler, and your geology
More informationImpact craters on regional plains on Venus: Age relations with wrinkle ridges and implications for the geological evolution of Venus
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 111,, doi:10.1029/2005je002473, 2006 Impact craters on regional plains on Venus: Age relations with wrinkle ridges and implications for the geological evolution of
More informationChapter 9 Planetary Geology: Earth and the Other Terrestrial Worlds
Chapter 9 Planetary Geology: Earth and the Other Terrestrial Worlds 9.1 Connecting Planetary Interiors and Surfaces Our goals for learning What are terrestrial planets like on the inside? What causes geological
More information9. Moon, Mercury, Venus
9. Moon, Mercury, Venus All the heavier elements were manufactured by stars later, either by thermonuclear fusion reactions deep in their interiors or by the violent explosions that mark the end of massive
More informationOverview of Solar System
Overview of Solar System The solar system is a disk Rotation of sun, orbits of planets all in same direction. Most planets rotate in this same sense. (Venus, Uranus, Pluto are exceptions). Angular momentum
More informationIn so many and such important. ways, then, do the planets bear witness to the earth's mobility. Nicholas Copernicus
In so many and such important ways, then, do the planets bear witness to the earth's mobility Nicholas Copernicus What We Will Learn Today What did it take to revise an age old belief? What is the Copernican
More informationYes, inner planets tend to be and outer planets tend to be.
1. Planet Density Make some general comments about inner and outer planets density Inner Planets Density Outer Planets Density Is there a pattern or a trend in planet density? Yes, inner planets tend to
More informationClass Exercise. Today s Class. Overview of Mercury. Terrestrial Planet Interiors. Today s Class: Mercury & Venus
Today s Class: Mercury & Venus Homework: Further reading on Venus for next class Sections 10.1 and 10.5 in Cosmic Perspective. Space in the News: 'Frankenstein' Galaxy Surprises Astronomers Presenter:
More informationOn the Origin of the Rocky Planets, Fugue in Venus Megacollision
On the Origin of the Rocky Planets, Fugue in Venus Megacollision Simon Porter October 30, 2009 And art thou, then, a world like ours, Flung from the orb that whirled our own A molten pebble from its zone?
More informationGeologic Features of Mars
Name Purpose Geologic Features of Mars To learn to identify landforms on the surface of Mars and the geological processes that produced them. Introduction In many ways, Mars is similar to Earth. The same
More informationWhere we are now. The Moon Chapters 8.2, 9. Topography. Outline
Where we are now Introduction Little things - comets, asteroids, KBOs Slightly larger things - Moon Larger still - Terrestrial planets Really large - Jovian planets Jovian moons + Pluto Extrasolar Planets
More informationASTRO 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
More informationHow can solid rock be bent, squished, stretched, and cracked?
AST 105 Intro Astronomy The Solar System MIDTERM II: Tuesday, April 5 4 Processes that Shape Surfaces Volcanism Eruption of molten rock onto surface Impact cratering Impacts by asteroids or comets Tectonics
More informationReading. 1 Read the extract from a book about the Solar System. Then complete the sentences with the words from the box. Earth.
Reading 1 Read the extract from a book about the Solar System. Then complete the sentences with the words from the box. Earth The third planet from the Sun is Earth, our home. Earth does not get as hot
More informationStar groups 88 recognized Stars names by brightness in them. Bright star to. Orion is Sirius
Star groups 88 recognized Stars names by brightness in them Orion: Greek Hunter White Tiger: Chinese http://borghetto.astrofili.org/costellazioni/costellazioni.htm Bright star to lower left of Orion is
More informationcrater density: number of craters per unit area on a surface
Reading for this week: Chap. 9, Sect. 9.4-9.5, Chap. 10, Sect. 10.1-10.5 Homework 6: due in recitation Friday/Monday (Oct. 13, 16) Midterm grade estimates posted on Blackboard this week Astro 120 Fall
More informationTopHat quizzes for astro How would you represent in scientific notation? A 2.7 x 10 2 B 2.7 x 10 3 C 2.7 x 10 4 D 2.
TopHat quizzes for astro 111 Lecture week 1 1. If you multiply 2 x 10 4 by itself, what do you get? A. 4 x 10 4 B. 4 x 10 8 C. 2 x 10 4 D. 4 x 10 16 2. Jupiter's maximum distance from the sun is approximately
More informationPhysics Homework Set 3 Fall 2015
1) Mercury presents the same side to the Sun 1) A) every third orbit. B) every 12 hours. C) all the time, just like our Moon. D) every other orbit. E) Twice every orbit. 2) Both the Moon and Mercury are
More informationGravity Tectonics Volcanism Atmosphere Water Winds Chemistry. Planetary Surfaces
Gravity Tectonics Volcanism Atmosphere Water Winds Chemistry Planetary Surfaces Gravity & Rotation Polar flattening caused by rotation is the largest deviation from a sphere for a planet sized object (as
More informationVenus s evolution: A synthesis
Geological Society of America Special Paper 419 2007 Venus s evolution: A synthesis V.L. Hansen Department of Geological Sciences, University of Minnesota, Duluth, Minnesota 55812, USA D.A. Young Department
More informationChapter 9 Lecture. The Cosmic Perspective Seventh Edition. Planetary Geology: Earth and the Other Terrestrial Worlds Pearson Education, Inc.
Chapter 9 Lecture The Cosmic Perspective Seventh Edition Planetary Geology: Earth and the Other Terrestrial Worlds Planetary Geology: Earth and the Other Terrestrial Worlds 9.1 Connecting Planetary Interiors
More informationMULTIPLE 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
More informationOutline. Planetary Atmospheres. General Comments about the Atmospheres of Terrestrial Planets. General Comments, continued
Outline Planetary Atmospheres Chapter 10 General comments about terrestrial planet atmospheres Atmospheric structure & the generic atmosphere Greenhouse effect Magnetosphere & the aurora Weather & climate
More informationIntro to Earth Science Chapter 23 Study Guide
Name _ Date _ Period _ Intro to Earth Science Chapter 23 Study Guide 1. is the planet that cannot be classified as either a terrestrial or a Jovian planet. 2. The densities of the planets are about five
More informationThe inner solar system cratering record and the evolution of
Research in Astronomy and Astrophysics manuscript no. (L A TEX: cratering paper raa v3.tex; printed on July 10, 2014; 16:34) The inner solar system cratering record and the evolution of impactor populations
More informationAstronomy November, 2016 Introduction to Astronomy: The Solar System. Mid-term Exam 3. Practice Version. Name (written legibly):
Astronomy 101 16 November, 2016 Introduction to Astronomy: The Solar System Mid-term Exam 3 Practice Version Name (written legibly): Honor Pledge: On my honor, I have neither given nor received unauthorized
More informationASTR 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
More informationSolar System B UT Regional 2018
Solar System B UT Regional 2018 Competitors: School Name: Team Number: This test contains 5 parts, worth 150 points in total. As always, you ll have 50 minutes to complete the test. You may separate the
More informationarxiv: v1 [astro-ph.ep] 16 Jul 2014
Research in Astronomy and Astrophysics manuscript no. (L A TEX: preprint.tex; printed on July 18, 2014; 0:47) The inner solar system cratering record and the evolution of arxiv:1407.4521v1 [astro-ph.ep]
More informationThe Planets and Scale
The Planets and Scale Elementary grades Lesson Summary Students practice reading data about the planets from a table and making numerical comparisons. Prior Knowledge & Skills Comparing numbers Reading
More informationName Class Date. For each pair of terms, explain how the meanings of the terms differ.
Skills Worksheet Chapter Review USING KEY TERMS For each pair of terms, explain how the meanings of the terms differ. 1. terrestrial planet and gas giant 2. asteroid and comet 3. meteor and meteorite Complete
More informationAfter you read this section, you should be able to answer these questions:
CHAPTER 16 4 Moons SECTION Our Solar System California Science Standards 8.2.g, 8.4.d, 8.4.e BEFORE YOU READ After you read this section, you should be able to answer these questions: How did Earth s moon
More informationMULTIPLE 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 B of the exam. Please fill in (B). A) This
More informationModule 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
More informationWhat's Up In Space? In the Center. Around the Sun. Around Earth. Space Facts! Places in Space
Non-fiction: What's Up In Space? What's Up In Space? Places in Space Space is an exciting place! Our solar system is in space. It is made up of the sun and the eight planets that travel around the sun.
More informationGeology of the terrestrial planets Pearson Education, Inc.
Geology of the terrestrial planets 2014 Pearson Education, Inc. Earth s Bulk Properties Earth s Bulk Properties albedo - A = 0.39 A = 0 planet absorbs all sunlight that hits it A =1 planet reflects all
More informationMAPPING THE SURFACE OF MARS
MAPPING THE SURFACE OF MARS What will you learn in this lab? How can we determine the geologic history of a planet or satellite without travelling to the planetary body? In this lab you will create a simple
More information7. 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
More informationMercury = Hermes Mythology. Planet Mercury, Element, Mercredi God of Commerce, Messenger God, guide to Hades Winged sandals and staff
Mercury = Hermes Mythology Planet Mercury, Element, Mercredi God of Commerce, Messenger God, guide to Hades Winged sandals and staff Mercury s Orbit Mercury never seen more than 28 from the sun Revolves/orbits
More informationEarth Science 11 Learning Guide Unit Complete the following table with information about the sun:
Earth Science 11 Learning Guide Unit 2 Name: 2-1 The sun 1. Complete the following table with information about the sun: a. Mass compare to the Earth: b. Temperature of the gases: c. The light and heat
More informationUnit 3 Lesson 4 The Terrestrial Planets. Copyright Houghton Mifflin Harcourt Publishing Company
Florida Benchmarks SC.8.N.1.5 Analyze the methods used to develop a scientific explanation as seen in different fields of science. SC.8.E.5.3 Distinguish the hierarchical relationships between planets
More informationI always wanted to be somebody, but I should have been more specific. Lilly Tomlin Reading has been updated. (All of Chaps. 9& 10) Friday, first sit
I always wanted to be somebody, but I should have been more specific. Lilly Tomlin Reading has been updated. (All of Chaps. 9& 10) Friday, first sit for passing back HW, then with chart. Water on the Moon?
More informationThe Inner Planets. Chapter 3 Lesson 1. Pages Workbook pages 51-52
The Inner Planets Chapter 3 Lesson 1 Pages 152-159 Workbook pages 51-52 Create the Foldable on pg 159 The solar The planets system The four inner planets Compare and Contrast Question What are planets?
More informationFor the next few weeks: Terrestrial Planets, their Moons, and the Sun. Planetary Surfaces and Interiors 2/20/07
For the next few weeks: Terrestrial Planets, their Moons, and the Sun Announcements Reading Assignment Section 9-1 (pp 186-189), 9-5 and 9-6 (pp 199-203) 3 rd Homework is now posted on the course website
More informationASTRONOMY 340 FALL September 2007 Class #6-#7
ASTRONOMY 340 FALL 2007 25 September 2007 Class #6-#7 Review Physical basis of spectroscopy Einstein A,B coefficients probabilities of transistions Absorption/emission coefficients are functions of ρ,
More information4 A(n) is a small, rocky object that orbits the sun; many of these objects are located in a band between the orbits of Mars and Jupiter.
Name Vocabulary Fill in the blank with the term that best completes the sentence., 6.11B 1 is the process in which energy is released as the nuclei of small atoms combine to form a larger nucleus., 6.11B
More informationLesson 2 The Inner Planets
Lesson 2 Student Labs and Activities Page Launch Lab 25 Content Vocabulary 26 Lesson Outline 27 MiniLab 29 Content Practice A 30 Content Practice B 31 School to Home 32 Key Concept Builders 33 Enrichment
More information