Planetary Formation OUTLINE

Size: px
Start display at page:

Download "Planetary Formation OUTLINE"

Transcription

1 Planetary Formation Reading this week: White p OUTLINE Today 1.Accretion 2.Planetary composition 1

2 11/1/17 Building Earth 2 things are important: Accretion means the assembly of Earth from smaller bits Differentiation means the separation of components within Earth during or after assembly ÞThese probably overlapped Nebula condenses Planets form by condensation of planetesimals Temperatures refer to conditions at initial condensation. 2

3 Formation in steps Condensation of gas->dust Km-sized bodies form quickly (<10 6 yr), some differentiate Moon & Mars sized bodies may also form quickly and differentiate Orbit crossing limits growth of big bodies: ~ yr Last stages in absence of solar nebula (used/blown away) What got included Planets start forming in a game of billiards Large control from Jupiter/Saturn Earth materials come from many different regions Zonation of composition in terrestrial zone unlikely Volatile depletion in the terrestrial planet forming materials Results from Chambers,

4 Simplified Earth s formation Fig. 6.4 From (A) a homogeneous, low-density protoplanet to (B) a dense, differentiated planet Importance of giant impacts Mercury head-on, high velocity, collision Total planetary disruption, silicate mantle gone: planet too dense Earth grazing, low velocity, collision Forms very large Moon Global magma oceans on both bodies Mars grazing, low velocity, collision Forms hemispheric dichotomy A baby magma ocean, no large moon 4

5 Mercury s density? How do we know density? Mercury plots above density-radius relationship For a fully differentiated core and mantle (assuming similar compositions as other planets) Core radius ~75% of the planet Core mass ~60% of the planet Instead expect something between Mars & Moon One explanation is giant impact, blasting silicate mantle into space, and only some of it making it back down Earth and Giant Impacts Simulations: Mars-sized bodies impacted Earth during accretion. Extreme events: Earth will radiate like a lowmass star for 1Ka! A large oblique impact places material in Earth orbit: Origin of the Moon 5

6 Earth-Moon System Things to explain: Earth-Moon same δ 18 O-δ 17 O line (TFL), not other planets/meteorites Both depleted in volatiles, but Moon more so Moon not exactly in Earth s equatorial plane Have to explain angular momentum Mars s moons probably captured, ours is big(ger) and compositionally similar. Wiechert et al., 2001 Krot et al., 2003 Giant impact Giant Impact Simulations *Earth close to final size *Mars-sized impactor *Both bodies already differentiated *Both bodies formed at ~1 AU *Grazing blow to explain current mass distribution of Earth and Moon (cores, silicate parts) 6

7 Post-impact Some of material blasted into space returns to Earth, rest accretes into Moon Exact dynamics of impact affect resulting rotation and orbit of both Byproduct of impact If Earth s temperature rises so it can radiate like a low-mass star, what will happen to the accreting spheroid? Think about the elemental budget, what do you expect to happen? Magma Ocean Ron Hartmann 7

8 Traces of accretion? Overall composition: elemental variations hint at conditions Isotopic compositions allow for timing and fingerprinting (later in the semester) Elemental partitioning = evidence of differentiation (next lecture) Heat flux (accretion +??) Pieces of accretion Meteorites are debris of planetary formation non chondrite meteorites sample... c. metal + silicate (stony/fe) a. silicate (stony) chondrites collide/ metamorphose accreting planetismals growth/radioactive heating 4 phase segregation: metal blobs + silicate b. metal (Fe) differentiated planetismal As accretion proceeds, different meteorites represent different parts of space & time Chondrites: most primitive material (recall similarity to solar composition) Achondrites: broadly basaltic (igneous textures), early silicate mantle(s) Irons: Fe-Ni alloys, broadly similar to our core Stony/Fe: mixtures of metallic and silicate materials, core-mantle boundary Also have pieces from Moon, Mars, Vesta, 8

9 Comparing Earth to Chondrites C1 chondrite» Sun (minus few volatiles) Earth s estimated primitive mantle (core removed) vs. C1: ~3 x refractory elements (Al, Ca, U, Th, Si, Ba, rare earths, ) depletions in other elements (including Mg and Si) Intermission some nomenclature Grouped by affinities of elements: 4 types of material thought to exist during accretion: Siderophile: iron- liking elements (liking zero-valent Fe; i.e., metal) Chalcophile: sulfide-liking (S 2- ) Lithophile: silicate-liking ([SiO 4 ] n, also O-loving in practice) Atmophile: gas-phase-liking 9

10 Close but not quite: CI Chondrite 101 Earth is Volatile-Depleted Where did they go? Bulk Silicate Earth Abundances Normalized by CI Chondrites Earth s Mantle is Siderophile Depleted Why? Bulk Silicate Earth Abundances Normalized by CI Chondrites Mo H Be N Al S K Ti MnNiGaSeRbZrRhCdSb LaNdGdHoYbTaOsAuPb U B O Na Si Cl Ca V FeCuGeBr SrNbPd In TeCsCeSmTb ErLu W Ir Hg Bi Li C F Mg P ScCrCoZnAs YRuAgSn I BaPr EuDyTmHfRe Pt Tl Th Elements in Order of Atomic Mass 10-4 Be Al Ti Ni ZrRh LaNdGdHoYbTaOsAu U O Si CaVFe SrNbPd CeSmTbErLu W Ir Li Mg P ScCrCo As YRu BaPr EuDyTmHfRe Pt Th Elements in Order of Atomic Mass Bulk Earth from McDonough and CI from Palme and O Neill, 2003 A Chondritic Earth Geochemist common assumption: Earth accreted from material with chondritic ratios of the non-volatile elements ÞRefractory isotope systems should look chondritic ÞThis recently became challenged (142Nd next slide) Elements also grouped based on their behavior (=amount vs. C1) (later slides) GG325 L30, F

11 Chondrites vs. Earth Short-lived isotope system: 146 Sm -> 142 Nd (T 1/2 = 103 Ma) After ~5xT 1/2 no 146 Sm left Þ 142 Nd differences made in ~ 500 Ma Earth is different from meteorites, leaves 2 options: 1)Major differentiation event on Earth before this time (hides complement) 2)Earth was never perfectly chondritic More and more people accept #2, but differences are small chondritic Earth OK for 1 st order understanding Boyet and Carlson Goldschmidt s Classification and the Geochemical Periodic Chart This classification was proposed in the 1920s by geochemist Goldschmidt. Qualitatively useful for describing the origin of the Earth from materials present in the early solar system Goldschmidt based his groups on the distributions of elements in silicate, metal-rich and gas phases in 1. metal-ore smelter materials 2. meteorites, 3. the modern Earth. 11

12 Goldschmidt Classification/Geochemical Periodic Chart Elements can be assigned to more than one group depending on the situation, so this scheme provides only generalities. Siderophile iron liking (zero-valent Fe) Chalcophile sulfide liking (S 2- ) Lithophile silicate liking ([SiO 4 ] n, also O loving in practice) Atmophile gas phase liking Where do these groups reside? GG325 L31, F2013 Goldschmidt Classification/Geochemical Periodic Chart The groups have a general relationship to the periodic chart, reflecting an underlying relationship to the electronic configurations of the elements in their common forms. GG325 L31, F

13 Major elements in mantle compared to meteorites Primitive Upper Mantle (PUM) composition is determined from intersection of chondritic meteorite array with mantle xenolith array PUM is not equal to any class of meteorites, Mg/Si higher in Earth; Ca/Si, Al/Si show solar system refractory vs. silicate phases Element Relationships: Earth and C1 Chondrites Most important siderophile and lithophile elements: BULK Earth has higher Fe/Si and Mg/Si than the chondrites (Sun) => if bulk earth» CI chondrite: lower mantle / core must host Si, or we got < chondrite 13

14 Volatiles Earth is variably depleted in volatile elements (e.g., K, Rb, Cs, etc.) relative to chondrites 14

Lecture 31. Planetary Accretion the raw materials and the final compositions

Lecture 31. Planetary Accretion the raw materials and the final compositions Lecture 31 Planetary Accretion the raw materials and the final compositions Reading this week: White Ch 11 (sections 11.1-11.4) Today 1. Boundary conditions for Planetary Accretion Growth and Differentiation

More information

Differentiation 1: core formation OUTLINE

Differentiation 1: core formation OUTLINE Differentiation 1: core formation Reading this week: White Ch 12 OUTLINE Today 1.Finish some slides 2.Layers 3.Core formation 1 Goldschmidt Classification/Geochemical Periodic Chart Elements can be assigned

More information

Meteorites free samples from the solar system

Meteorites free samples from the solar system Meteorites free samples from the solar system It is easier to believe that Yankee professors would lie, than that stones would fall from heaven [Thomas Jefferson, 3rd president of the USA] 2.1 Collection

More information

Differentiation 2: mantle, crust OUTLINE

Differentiation 2: mantle, crust OUTLINE Differentiation 2: mantle, crust OUTLINE Reading this week: Should have been White Ch 10 and 11!! 7- Nov Differentiation of the Earth, Core formation W 10.6.6, 11.4 9- Nov Moon, crust, mantle, atmosphere

More information

Composition and the Early History of the Earth

Composition and the Early History of the Earth Composition and the Early History of the Earth Sujoy Mukhopadhyay CIDER 2006 What we will cover in this lecture Composition of Earth Short lived nuclides and differentiation of the Earth Atmosphere and

More information

Cosmic Building Blocks: From What is Earth Made?

Cosmic Building Blocks: From What is Earth Made? Cosmic Building Blocks: From What is Earth Made? The Sun constitutes 99.87% of the mass of the Solar system. Earth is big and important, so its composition should be similar to that of the average Solar

More information

A non-traditional stable isotope perspective

A non-traditional stable isotope perspective The origins of the Moon: A non-traditional stable isotope perspective Fang-Zhen Teng Department of Earth and Space Sciences From the beginning: The Universe: 13.8 Ga The Milky Way Galaxy The Solar System

More information

General Introduction. The Earth as an evolving geologic body

General Introduction. The Earth as an evolving geologic body General Introduction The Earth as an evolving geologic body Unique/important attributes of Planet Earth 1. Rocky planet w/ strong magnetic field Mercury has a weak field, Mars has a dead field 1 Unique/important

More information

Figure of rare earth elemental abundances removed due to copyright restrictions.

Figure of rare earth elemental abundances removed due to copyright restrictions. Figure of rare earth elemental abundances removed due to copyright restrictions. See figure 3.1 on page 26 of Tolstikhin, Igor and Jan Kramers. The Evolution of Matter: From the Big Bang to the Present

More information

Formation of the Earth and Solar System

Formation of the Earth and Solar System Formation of the Earth and Solar System a. Supernova and formation of primordial dust cloud. NEBULAR HYPOTHESIS b. Condensation of primordial dust. Forms disk-shaped nubular cloud rotating counterclockwise.

More information

Volatiles in the terrestrial planets. Sujoy Mukhopadhyay University of California, Davis CIDER, 2014

Volatiles in the terrestrial planets. Sujoy Mukhopadhyay University of California, Davis CIDER, 2014 Volatiles in the terrestrial planets Sujoy Mukhopadhyay University of California, Davis CIDER, 2014 Atmophiles: Elements I will talk about rock-loving iron-loving sulfur-loving Temperatures in Protoplanetary

More information

2/24/2014. Early Earth (Hadean) Early Earth. Terms. Chondrule Chondrite Hadean Big Bang Nucleosynthesis Fusion Supernova

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

More information

Lab 5: An Investigation of Meteorites Geology 202: Earth s Interior

Lab 5: An Investigation of Meteorites Geology 202: Earth s Interior Lab 5: An Investigation of Meteorites Geology 202: Earth s Interior Asteroids and Meteorites: What is the difference between asteroids and meteorites? Asteroids are rocky and metallic objects that orbit

More information

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)

More information

OCN 201: Origin of the Earth and Oceans. Waimea Bay, Jan 2002

OCN 201: Origin of the Earth and Oceans. Waimea Bay, Jan 2002 OCN 201: Origin of the Earth and Oceans Waimea Bay, Jan 2002 Periodic Table of the Elements Noble IA IIA IIIA IVA VA VIA VIIA VIIIA IB IIB IIIB IVB VB VIB VIIB gases H He Li Be B C N O F Ne Na Mg Al Si

More information

Radioactive Dating. U238>Pb206. Halflife: Oldest earth rocks. Meteors and Moon rocks. 4.5 billion years billion years

Radioactive Dating. U238>Pb206. Halflife: Oldest earth rocks. Meteors and Moon rocks. 4.5 billion years billion years U238>Pb206 Halflife: 4.5 billion years Oldest earth rocks 3.96 billion years Meteors and Moon rocks 4.6 billion years This is the time they solidified The solar system is older than this. Radioactive Dating

More information

Differentiation & Thermal Evolution

Differentiation & Thermal Evolution Differentiation & Thermal Evolution 1 1 Meteorite Classification: Iron Meteorites 2 Meteorite Classification: Iron Meteorites 2 Meteorite Classification Basic Types of Meteorites: - Stony (93% of falls)

More information

Wed. Aug. 30, 2017 Reading:

Wed. Aug. 30, 2017 Reading: Wed. Aug. 30, 2017 Reading: Reading for Fri.: Wood Ch. 1 (solar system overview) Reading for Wed. Wed. Wood Ch. 6 & 8 (Asteroids & Meteorites, Solar Nebula) Reading for Fri. Sept. 8. Rozel et al. (link

More information

Composition of the Earth and its reservoirs: Geochemical observables

Composition of the Earth and its reservoirs: Geochemical observables Composition of the Earth and its reservoirs: Geochemical observables Cin-Ty A. Lee Rice University MYRES-I 2004 The Earth is dynamic and heterogeneous Atmosphere Midocean Ridge Plume Ocean Crust Oceanic

More information

Today: Collect homework Hand out new homework Exam Friday Sept. 20. Carrick Eggleston begins lectures on Wednesday

Today: Collect homework Hand out new homework Exam Friday Sept. 20. Carrick Eggleston begins lectures on Wednesday Geol 2000 Mon. Sep. 09, 2013 Today: Collect homework Hand out new homework Exam Friday Sept. 20 Review session THIS Friday Sept. 13 10AM? Geol. 216? (Discuss with class if this time works for students.

More information

Lecture 9 : Meteorites and the Early Solar System

Lecture 9 : Meteorites and the Early Solar System Lecture 9 : Meteorites and the Early Solar System 1 Announcements Reminder: HW 3 handed out this week, due next week. HW 1 will be returned Wednesday and solutions posted. Midterm exam Monday Oct 22, in

More information

(4) Meteorites: Remnants of Creation

(4) Meteorites: Remnants of Creation (4) Meteorites: Remnants of Creation Meteoroid: small piece of debris in space Meteor: space debris heated by friction as it plunges into the Earth s atmosphere Meteorite: Space debris that has reached

More information

Solar System Forma-on

Solar System Forma-on Solar System Forma-on The processes by which stars and planets form are ac-ve areas of research in modern astrophysics The forma-on of our own solar system is central to the first half of our course, and

More information

At the beginning. Matter + antimatter. Matter has the advantage. baryons quarks, leptons, electrons, photons (no protons or neutrons)

At the beginning. Matter + antimatter. Matter has the advantage. baryons quarks, leptons, electrons, photons (no protons or neutrons) At the beginning Matter + antimatter Matter has the advantage baryons quarks, leptons, electrons, photons (no protons or neutrons) Hadrons protons, neutrons Hydrogen, helium (:0 H:He) Origin of the Universe

More information

Initial Conditions: The temperature varies with distance from the protosun.

Initial Conditions: The temperature varies with distance from the protosun. Initial Conditions: The temperature varies with distance from the protosun. In the outer disk it is cold enough for ice to condense onto dust to form large icy grains. In the inner solar system ice can

More information

Recap: Element Segregation

Recap: Element Segregation Recap: Earth is Structured A) Metal Core and Silicate mantle and Crust B) Deduced by: -Observation of crust and mantle derived rocks -Seismic structure (P and S waves) -Knowledge of Earth mass deduced

More information

http://eps.mcgill.ca/~courses/c220/ Nucleosynthesis neutron electron + proton = é + H + t 1/2 = 12 minutes H + + neutron Deuterium (D) 2 H + + neutrons Helium (He) 3 H + + neutrons Lithium (Li) From: W.S.

More information

Announcements. Reminder: HW 3 is due Thursday, 5 PM. HW 2 can still be turned in (with the late penalty) today before 5 PM.

Announcements. Reminder: HW 3 is due Thursday, 5 PM. HW 2 can still be turned in (with the late penalty) today before 5 PM. Announcements Reminder: HW 3 is due Thursday, 5 PM HW 2 can still be turned in (with the late penalty) today before 5 PM. 1 Lecture 9 : Meteorites and the Early Solar System 2 Meteorite terminology Meteoroid:

More information

Question 1 (1 point) Question 2 (1 point) Question 3 (1 point)

Question 1 (1 point) Question 2 (1 point) Question 3 (1 point) Question 1 (1 point) If the Earth accreted relatively slowly, the heat obtained from the gravitational potential energy would have had time to escape during its accretion. We know that the Earth was already

More information

B.S., 1970, Geology, Michigan State University. M.A., 1972, Geology, Princeton University. Post-doctoral fellow, , Stanford University

B.S., 1970, Geology, Michigan State University. M.A., 1972, Geology, Princeton University. Post-doctoral fellow, , Stanford University B.S., 1970, Geology, Michigan State University M.A., 1972, Geology, Princeton University Ph.D., 1976, Geology, Harvard University Post-doctoral fellow, 1976-77, Stanford University Scientist, 1977-86,

More information

Accretionary Disk Model

Accretionary Disk Model Accretionary Disk Model SOLAR NEBULAR THEORY a large cloud of gas began eventually forming the Sun at its center while the outer, cooler, parts created the planets. SOLAR NEBULA A cloud of gasses and

More information

Formation of the Solar System. What We Know. What We Know

Formation of the Solar System. What We Know. What We Know Formation of the Solar System Many of the characteristics of the planets we discussed last week are a direct result of how the Solar System formed Until recently, theories for solar system formation were

More information

Lecture 16. How did it happen? How long did it take? Where did it occur? Was there more than 1 process?

Lecture 16. How did it happen? How long did it take? Where did it occur? Was there more than 1 process? Planet formation in the Solar System Lecture 16 How did it happen? How long did it take? Where did it occur? Was there more than 1 process? Planet formation How do planets form?? By what mechanism? Planet

More information

Today. Solar System Formation. a few more bits and pieces. Homework due

Today. Solar System Formation. a few more bits and pieces. Homework due Today Solar System Formation a few more bits and pieces Homework due Pluto Charon 3000 km Asteroids small irregular rocky bodies Comets icy bodies Formation of the Solar System How did these things come

More information

In class, Wednesday Oct 25. Please wait outside AT BACK until told to enter the room. Must write IN PEN. Non programming calculators allowed (and

In class, Wednesday Oct 25. Please wait outside AT BACK until told to enter the room. Must write IN PEN. Non programming calculators allowed (and Midterm material In class, Wednesday Oct 25. Please wait outside AT BACK until told to enter the room. Must write IN PEN. Non programming calculators allowed (and required) No notes or hats. Formulae provided

More information

AMHERST COLLEGE Department of Geology Geology 41: Environmental and Solid Earth Geophysics

AMHERST COLLEGE Department of Geology Geology 41: Environmental and Solid Earth Geophysics AMHERST COLLEGE Department of Geology Geology 41: Environmental and Solid Earth Geophysics Lab 1: Meteorites EQUIPMENT: notebook and pen only In this lab, we will examine thin sections and hand samples

More information

Isotopic record of the atmosphere and hydrosphere

Isotopic record of the atmosphere and hydrosphere Isotopic record of the atmosphere and hydrosphere W. F. McDonough 1 1 Department of Earth Sciences and Research Center for Neutrino Science, Tohoku University, Sendai 980-8578, Japan (Dated: March 7, 2018)

More information

GEOL212 Due 10/9/17 Homework VI

GEOL212 Due 10/9/17 Homework VI GEOL212 Due 10/9/17 Homework VI General instructions: Although you are allowed to discuss homework questions with your classmates, your work must be uniquely your own. Thus, please answer all questions

More information

Chapter 11. The Archean Era of Precambrian Time

Chapter 11. The Archean Era of Precambrian Time Chapter 11 The Archean Era of Precambrian Time 1 Guiding Questions When and how did Earth and its moon come into being? How did the core, mantle, crust form? Where did Archean rocks form, and what is their

More information

Mercury. Why is Mercury important? Background from Mariner 10 to MESSENGER. An unusual geochemistry. Pre-MESSENGER models

Mercury. Why is Mercury important? Background from Mariner 10 to MESSENGER. An unusual geochemistry. Pre-MESSENGER models Mercury TJ McCoy and LR Nittler 2014 (2003) Why is Mercury important? Background from Mariner 10 to MESSENGER An unusual geochemistry Pre-MESSENGER models Re-evaluation of models + discussion Mariner 10

More information

Formation of the Solar System Chapter 8

Formation of the Solar System Chapter 8 Formation of the Solar System Chapter 8 To understand the formation of the solar system one has to apply concepts such as: Conservation of angular momentum Conservation of energy The theory of the formation

More information

Nebular Hypothesis and Origin of Earth s Water

Nebular Hypothesis and Origin of Earth s Water Nebular Hypothesis and Origin of Earth s Water What is the shape of our solar system? A. Spherical: the Sun is in the center, the planets orbit in spherical shells. B. Disc shaped: fat in the center, tapering

More information

5. How did Copernicus s model solve the problem of some planets moving backwards?

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

More information

Origin of heavier elements, origin of universe

Origin of heavier elements, origin of universe Origin of heavier elements, origin of universe Like we said earlier It takes higher and higher temperatures to make larger and larger nuclei fuse together What happens when a star cannot maintain fusion

More information

Models of the Earth: thermal evolution and Geoneutrino studies

Models of the Earth: thermal evolution and Geoneutrino studies Models of the Earth: thermal evolution and Geoneutrino studies Bill McDonough, Yu Huang and Ondřej Šrámek Geology, U Maryland Steve Dye, Natural Science, Hawaii Pacific U and Physics, U Hawaii Shijie Zhong,

More information

Nebular Hypothesis and Origin of Earth s Water

Nebular Hypothesis and Origin of Earth s Water Nebular Hypothesis and Origin of Earth s Water What is the shape of our solar system? A. Spherical: the Sun is in the center, the planets orbit in spherical shells. B. Disc shaped: fat in the center, tapering

More information

Comparative Planetology II: The Origin of Our Solar System. Chapter Eight

Comparative Planetology II: The Origin of Our Solar System. Chapter Eight Comparative Planetology II: The Origin of Our Solar System Chapter Eight ASTR 111 003 Fall 2007 Lecture 07 Oct. 15, 2007 Introduction To Modern Astronomy I: Solar System Introducing Astronomy (chap. 1-6)

More information

Astronomy 405 Solar System and ISM

Astronomy 405 Solar System and ISM Astronomy 405 Solar System and ISM Lecture 17 Planetary System Formation and Evolution February 22, 2013 grav collapse opposed by turbulence, B field, thermal Cartoon of Star Formation isolated, quasi-static,

More information

Constructing the Moon

Constructing the Moon Constructing the Solar System: A Smashing Success Constructing the Moon Thomas M. Davison Department of the Geophysical Sciences Compton Lecture Series Autumn 2012 T. M. Davison Constructing the Solar

More information

Origin of the Solar System

Origin of the Solar System Origin of the Solar System Look for General Properties Dynamical Regularities Orbits in plane, nearly circular Orbit sun in same direction (CCW from N.P.) Rotation Axes to orbit plane (Sun & most planets;

More information

-Melissa Greenberg, Arielle Hoffman, Zachary Feldmann, Ryan Pozin, Elizabeth Weeks, Christopher Pesota, & Sara Pilcher

-Melissa Greenberg, Arielle Hoffman, Zachary Feldmann, Ryan Pozin, Elizabeth Weeks, Christopher Pesota, & Sara Pilcher -Melissa Greenberg, Arielle Hoffman, Zachary Feldmann, Ryan Pozin, Elizabeth Weeks, Christopher Pesota, & Sara Pilcher Formation Overview All explanations as to how the solar system was formed are only

More information

Remote Sensing of the Earth s Interior

Remote Sensing of the Earth s Interior Remote Sensing of the Earth s Interior Earth s interior is largely inaccessible Origin and Layering of the Earth: Geochemical Perspectives Composition of Earth cannot be understood in isolation Sun and

More information

Compositional relationships between meteorites and planets I. Kevin Righter NASA Johnson Space Center

Compositional relationships between meteorites and planets I. Kevin Righter NASA Johnson Space Center Compositional relationships between meteorites and planets I Kevin Righter NASA Johnson Space Center Accretion models for terrestrial planets Can we make planets from meteorites? What are the outstanding

More information

Chapter Outline. Earth and Other Planets. The Formation of the Solar System. Clue #1: Planetary Orbits. Clues to the Origin of the Solar System

Chapter Outline. Earth and Other Planets. The Formation of the Solar System. Clue #1: Planetary Orbits. Clues to the Origin of the Solar System Chapter Outline Earth and Other Planets The Formation of the Solar System Exploring the Solar System Chapter 16 Great Idea: Earth, one of the planets that orbit the Sun, formed 4.5 billion years ago from

More information

Wed. Oct. 04, Makeup lecture time? Will Friday noon work for everyone? No class Oct. 16, 18, 20?

Wed. Oct. 04, Makeup lecture time? Will Friday noon work for everyone? No class Oct. 16, 18, 20? Wed. Oct. 04, 2017 Reading: For Friday: Bugiolacchi et al. 2008 Laurence et al. 1998" Makeup lecture time? Will Friday noon work for everyone? No class Oct. 16, 18, 20? Today: Finish Lunar overview (from

More information

Geochemical constraints on the core formation and composition

Geochemical constraints on the core formation and composition Geochemical constraints on the core formation and composition Bernard Bourdon ENS Lyon with: Mathieu Touboul, Caroline Fitoussi, John Rudge and Thorsten Kleine Collège de France November 25 th Core formation

More information

Astronomy 101 The Solar System Tuesday, Thursday 2:30-3:45 pm Hasbrouck 20. Tom Burbine

Astronomy 101 The Solar System Tuesday, Thursday 2:30-3:45 pm Hasbrouck 20. Tom Burbine Astronomy 101 The Solar System Tuesday, Thursday 2:30-3:45 pm Hasbrouck 20 Tom Burbine tomburbine@astro.umass.edu Course Course Website: http://blogs.umass.edu/astron101-tburbine/ Textbook: Pathways to

More information

AST 248. Is Pluto a Planet?

AST 248. Is Pluto a Planet? AST 248 Is Pluto a Planet? And what is a planet, anyways? N = N * f s f p n h f l f i f c L/T What is a Star? A star supports stable Hydrogen fusion Upper mass limit: about 120 M above that radiation pressure

More information

The History of the Earth

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

More information

Astr 1050 Fri., Feb. 24, 2017

Astr 1050 Fri., Feb. 24, 2017 Astr 1050 Fri., Feb. 24, 2017 Chapter 7 & 8: Overview & Formation of the Solar System Reading: Chapters 7 on Solar System Chapter 8: Earth & Terrestrial Planets Reminders: New homework on MA up this afternoon,

More information

Analyzing the Chemical Composition and Classification of Miller Range 07273

Analyzing the Chemical Composition and Classification of Miller Range 07273 Alyssa Dolan Analyzing the Chemical Composition and Classification of Miller Range 07273 When small grains and debris that were present in the early solar system combine, they form meteoroids. Meteoroids

More information

HNRS 227 Fall 2006 Chapter 13. What is Pluto? What is a Planet? There are two broad categories of planets: Terrestrial and Jovian

HNRS 227 Fall 2006 Chapter 13. What is Pluto? What is a Planet? There are two broad categories of planets: Terrestrial and Jovian Key Points of Chapter 13 HNRS 227 Fall 2006 Chapter 13 The Solar System presented by Prof. Geller 24 October 2006 Planets Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune Dwarf Planets Pluto,

More information

Meteoritics clues to the origin of the Solar System. Dr Alex Bevan

Meteoritics clues to the origin of the Solar System. Dr Alex Bevan Meteoritics clues to the origin of the Solar System Dr Alex Bevan Monday 15th June 2009, ninety people (RSWA members, their families, interested scientists, and members of the public) attended the fourth

More information

Chapter 19 The Origin of the Solar System

Chapter 19 The Origin of the Solar System Chapter 19 The Origin of the Solar System Early Hypotheses catastrophic hypotheses, e.g., passing star hypothesis: Star passing closely to the the sun tore material out of the sun, from which planets could

More information

Chapter 8 Lecture. The Cosmic Perspective Seventh Edition. Formation of the Solar System

Chapter 8 Lecture. The Cosmic Perspective Seventh Edition. Formation of the Solar System Chapter 8 Lecture The Cosmic Perspective Seventh Edition Formation of the Solar System Formation of the Solar System 8.1 The Search for Origins Our goals for learning: Develop a theory of solar system

More information

Evidence of Earth s Interior Direct and Indirect Evidence

Evidence of Earth s Interior Direct and Indirect Evidence Into Which Layer Have We Drilled? Evidence of Earth s Interior Direct and Indirect Evidence 1. Crust 2. Mantle 3. Outer Core 4. Inner Core Why?? How Many Types of Crust Exist? Which of the following is

More information

Astronomy A BEGINNER S GUIDE TO THE UNIVERSE EIGHTH EDITION

Astronomy A BEGINNER S GUIDE TO THE UNIVERSE EIGHTH EDITION Astronomy A BEGINNER S GUIDE TO THE UNIVERSE EIGHTH EDITION CHAPTER 4 The Solar System Lecture Presentation 4.0 What can be seen with the naked eye? Early astronomers knew about the Sun, Moon, stars, Mercury,

More information

SUPPLEMENTARY INFORMATION

SUPPLEMENTARY INFORMATION doi:10.1038/nature10326 Supplementary Discussion All known modern terrestrial mantle reservoirs evolved from a primitive precursor with superchondritic 143 Nd/ 144 Nd. What is this reservoir? The terms

More information

Minimum Radii of Super-Earths: Constraints from Giant Impacts

Minimum Radii of Super-Earths: Constraints from Giant Impacts Minimum Radii of Super-Earths: Constraints from Giant Impacts Robert A. Marcus 1,a, Dimitar Sasselov 1, Lars Hernquist 1, Sarah T. Stewart 2 1 Astronomy Department, Harvard University, Cambridge, MA 02138

More information

For thought: Excess volatiles

For thought: Excess volatiles For thought: Excess volatiles Term coined by William Rubey (circa 1955) Definition: Compounds present at Earth s surface that were not derived from converting igneous rock to sedimentary rock Rubey and

More information

Topic 1. Relative abundances

Topic 1. Relative abundances Topic 1 Observational evidence for relative abundances Relative abundances The plot to the right shows the relative abundances of atomic species as a function of atomic mass number. Note that it is a logarithmic

More information

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

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---

More information

AN OXYGEN ISOTOPE MIXING MODEL FOR THE ACCRETION AND COMPOSITION OF ROCKY PLANETS. 1. Introduction

AN OXYGEN ISOTOPE MIXING MODEL FOR THE ACCRETION AND COMPOSITION OF ROCKY PLANETS. 1. Introduction AN OXYGEN ISOTOPE MIXING MODEL FOR THE ACCRETION AND COMPOSITION OF ROCKY PLANETS KATHARINA LODDERS Planetary Chemistry Laboratory, Department of Earth and Planetary Sciences, Washington University, St.

More information

Origin of the Solar System

Origin of the Solar System Origin of the Solar System and Solar System Debris 1 Debris comets meteoroids asteroids gas dust 2 Asteroids irregular, rocky hunks small in mass and size Ceres - largest, 1000 km in diameter (1/3 Moon)

More information

Meteorite Ages & Timing of Solar System Processes

Meteorite Ages & Timing of Solar System Processes Meteorite Ages & Timing of Solar System Processes 1 Isotope Systematics Object 0 CHUR 26 Mg 24 Mg 26 Mg 24 Mg 26 Mg 24 Mg Chemical fractionation 26 Al decay ( 26 Al/ 27 Al) t0 ( 26 Mg/ 24 Mg) t0 ( 26 Mg/

More information

Class Exercise. Today s Class: The Origin & Evolution of the Moon. Space in the News: NASA and Russia Partner Up for Crewed Deep-Space Missions

Class Exercise. Today s Class: The Origin & Evolution of the Moon. Space in the News: NASA and Russia Partner Up for Crewed Deep-Space Missions Today s Class: The Origin & Evolution of the Moon 1. 2. 3. 4. Homework. Read: Sections 9.2-9.3 in Cosmic Perspective. Next class is at Fiske Planetarium! Need volunteers for Space in the News. Exam #2

More information

SIO 103 Origin and composition of the Earth

SIO 103 Origin and composition of the Earth SIO 103 Origin and composition of the Earth In this chapter we briefly review the origin of the Earth, from the Big Bang 14 billion years ago to the accretion of the Earth from the solar nebula some 4.56

More information

Earth s Formation Unit [Astronomy] Student Success Sheets (SSS)

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

More information

Comparative Planetology II: The Origin of Our Solar System. Chapter Eight

Comparative Planetology II: The Origin of Our Solar System. Chapter Eight Comparative Planetology II: The Origin of Our Solar System Chapter Eight ASTR 111 003 Fall 2007 Lecture 06 Oct. 09, 2007 Introduction To Modern Astronomy I: Solar System Introducing Astronomy (chap. 1-6)

More information

Solar System Formation

Solar System Formation Solar System Formation Solar System Formation Question: How did our solar system and other planetary systems form? Comparative planetology has helped us understand Compare the differences and similarities

More information

1 The Earth as a Planet

1 The Earth as a Planet General Astronomy (29:61) Fall 2012 Lecture 27 Notes, November 5, 2012 1 The Earth as a Planet As we start studying the planets, we begin with Earth. To begin with, it gives us a different perspective

More information

The Solar Nebula Theory

The Solar Nebula Theory Reading: Chap. 21, Sect.21.1, 21.3 Final Exam: Tuesday, December 12; 4:30-6:30PM Homework 10: Due in recitation Dec. 1,4 Astro 120 Fall 2017: Lecture 25 page 1 Astro 120 Fall 2017: Lecture 25 page 2 The

More information

Comparative Planetology I: Our Solar System

Comparative Planetology I: Our Solar System Comparative Planetology I: Our Solar System Guiding Questions 1. Are all the other planets similar to Earth, or are they very different? 2. Do other planets have moons like Earth s Moon? 3. How do astronomers

More information

Evolution of the Atmosphere: The Biological Connection

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

More information

8. Solar System Origins

8. Solar System Origins 8. Solar System Origins Chemical composition of the galaxy The solar nebula Planetary accretion Extrasolar planets Our Galaxy s Chemical Composition es Big Bang produced hydrogen & helium Stellar processes

More information

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

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

More information

arxiv: v1 [astro-ph.ep] 29 Aug 2017

arxiv: v1 [astro-ph.ep] 29 Aug 2017 The Elemental Abundances (with Uncertainties) of the Most Earth-like Planet Haiyang S. Wang a,b,, Charles H. Lineweaver a,b,c, Trevor R. Ireland b,c a Research School of Astronomy and Astrophysics, The

More information

AST 301 Introduction to Astronomy

AST 301 Introduction to Astronomy AST 301 Introduction to Astronomy John Lacy RLM 16.332 471-1469 lacy@astro.as.utexas.edu Myoungwon Jeon RLM 16.216 471-0445 myjeon@astro.as.utexas.edu Bohua Li RLM 16.212 471-8443 bohuali@astro.as.utexas.edu

More information

The Earth-Moon system. Origin of the Moon. Mark Wyatt

The Earth-Moon system. Origin of the Moon. Mark Wyatt Origin of the Moon Mark Wyatt The Earth-Moon system The Moon orbits the Earth at a moon = 385,000 km with an eccentricity of 0.05, inclination to ecliptic of 5 o The Earth orbits the Sun at a earth = 150,000,000

More information

Wed. Sept. 20, Today: For Monday Sept. 25 and following days read Chapter 4 (The Moon) of Christiansen and Hamblin (on reserve).

Wed. Sept. 20, Today: For Monday Sept. 25 and following days read Chapter 4 (The Moon) of Christiansen and Hamblin (on reserve). Wed. Sept. 20, 2017 Reading: For Friday: Connelly et al. 2012, "The Absolute Chronology and Thermal Processing of Solids in the Solar Protoplanetary Disk." 338: 651-665. Simon et al., 2011, "Oxygen Isotope

More information

What is it like? When did it form? How did it form. The Solar System. Fall, 2005 Astronomy 110 1

What is it like? When did it form? How did it form. The Solar System. Fall, 2005 Astronomy 110 1 What is it like? When did it form? How did it form The Solar System Fall, 2005 Astronomy 110 1 Fall, 2005 Astronomy 110 2 The planets all orbit the sun in the same direction. The Sun spins in the same

More information

Class Announcements. Solar System. Objectives for today. Will you read Chap 32 before Wed. class? Chap 32 Beyond the Earth

Class Announcements. Solar System. Objectives for today. Will you read Chap 32 before Wed. class? Chap 32 Beyond the Earth Class Announcements Please fill out an evaluation for this class. If you release your name I ll I give you quiz credit. Will you read Chap 32 before Wed. class? a) Yes b) No Chap 32 Beyond the Earth Objectives

More information

Regular Features of the Solar System

Regular Features of the Solar System 1 Regular Features of the Solar System All of the planets orbit the Sun in the same plane All planetary orbits are nearly circular All planets orbit the Sun in the same direction Most planets rotate in

More information

The Earth-Moon system. Origin of the Moon. Mark Wyatt

The Earth-Moon system. Origin of the Moon. Mark Wyatt Origin of the Moon Mark Wyatt The Earth-Moon system The Moon orbits the Earth at a moon = 385,000 km with an eccentricity of 0.05, inclination to ecliptic of 5 o The Earth orbits the Sun at a earth = 150,000,000

More information

Brooks Observatory telescope observing this week

Brooks Observatory telescope observing this week Brooks Observatory telescope observing this week Mon. - Thurs., 7:30 9:15 PM MW, 7:30 8:45 PM TR See the class web page for weather updates. This evening s session is cancelled. Present your blue ticket

More information

Composition of bulk silicate Earth and global geodynamics

Composition of bulk silicate Earth and global geodynamics Composition of bulk silicate Earth and global geodynamics Jun Korenaga Department of Geology and Geophysics Yale University March 23, 2007 @ Hawaii Geoneutrino Workshop Overview Motivation: Thermal evolution

More information

The Solar System consists of

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

More information

From observations of newly formed stars it appears that the

From observations of newly formed stars it appears that the Vol 441 15 June 2006 doi:10.1038/nature04763 Accretion of the Earth and segregation of its core Bernard J. Wood 1, Michael J. Walter 2 & Jonathan Wade 2 The Earth took 30 40 million years to accrete from

More information

Vagabonds of the Solar System

Vagabonds of the Solar System Vagabonds of the Solar System Guiding Questions 1. How and why were the asteroids first discovered? 2. Why didn t the asteroids coalesce to form a single planet? 3. What do asteroids look like? 4. How

More information

12/3/14. Guiding Questions. Vagabonds of the Solar System. A search for a planet between Mars and Jupiter led to the discovery of asteroids

12/3/14. Guiding Questions. Vagabonds of the Solar System. A search for a planet between Mars and Jupiter led to the discovery of asteroids Guiding Questions Vagabonds of the Solar System 1. How and why were the asteroids first discovered? 2. Why didn t the asteroids coalesce to form a single planet? 3. What do asteroids look like? 4. How

More information