Definition of “fossil” A fossil is defined as any remains, trace or imprint of a plant or animal that has been preserved by natural processes in the Earth’s.

Slides:



Advertisements
Similar presentations
Topic: Absolute Dating Absolute Dating is the real, true age of the rock.
Advertisements

Other clues to the formation of the Solar System Inner planets are small and dense Outer planets are large and have low density Satellites of the outer.
WHAT IS THE CURRENT SCIENTIFIC THEORY FOR THE FORMATION OF THE UNIVERSE?
The origin of the Solar System. Small planets beyond Pluto – Sedna, ~1,300 – 1750 km dia.
Oxygen Isotopes Anomalies of the Sun and the Original Environment of the Solar System Jeong-Eun Lee UCLA.
Vagabonds of the Solar System Chapter 17. A search for a planet between Mars and Jupiter led to the discovery of asteroids Astronomers first discovered.
Trace Element Abundances in Single Presolar SiC Stardust Grains by Synchrotron X-Ray Fluorescence (SXRF) Zhonghu Cai (XOR) Barry Lai (XOR) Steve Sutton.
New Science from new Technology: NanoSIMS and RIMS Peter Hoppe Max-Planck-Institute for Chemistry IAU Meeting 2006 Prague August 21, 2006.
8-1 The key characteristics of the solar system that must be explained by any theory of its origins 8-2 How the abundances of chemical elements in the.
The Nebular Hypothesis
Radiometric Dating and Half Life Over time a radioactive sample becomes less radioactive as unstable atoms decay to stable forms. The decay is a random.
Meteorites II: Differentiated Meteorites; Ages Lecture 41.
History of the Earth Chapter 1: Formation of the Earth From the Big Bang to Early Planets.
How did the Earth form? What processes were involved? When did it happen? How long did it take? How do we know?
Dynamic Earth Class 4 19 January Any Questions?
History of the Earth Chapter 1: Formation of the Earth From the Big Bang to Early Planets.
1 Chapter 2 Origins  Formation of Universe, Solar System and Earth  Creation of Oceans.
1 Chapter 2 Creation of Oceans. 2 Supporting Evidence for the Big Bang Edwin Hubble discovered spreading of galaxies. Cosmic background radiation (the.
Asteroids Astronomy 311 Professor Lee Carkner Lecture 15.
Astronomy 1 – Winter 2011 Lecture 11; January
1 Lecture #02 - Earth History. 2 The Fine Structure of The Universe : The Elements Elements are a basic building block of molecules, and only 92 natural.
Chapter 8 Welcome to the Solar System. 8.1 The Search for Origins Our goals for learning What properties of our solar system must a formation theory explain?
Meteorites: Rocks from space. Leonid meteor shower, 1998 European Fireball Network image Meteoroid Meteor (fireball) Meteorite.
How did the Solar System form? 3. What are the broad general characteristics or physical features of our Solar System and how do they illuminate Solar.
Comparative Planetology: Our Solar System Chapter Seven & Eight.
How our Solar System (and Moon) came to be…. Learning Objectives Be able to explain – How our solar system and moon came to be.
Comparative Planetology II: The Origin of Our Solar System
Origin of the Solar System. Stars spew out 1/2 their mass as gas & dust as they die.
Our Solar System and Its Origin. What does the solar system look like?
Origin of the Solar System. Stars spew out 1/2 their mass as gas & dust as they die.
Comparative Planetology II: The Origin of Our Solar System.
Copyright © 2014 All rights reserved, Government of Newfoundland and Labrador Earth Systems 3209 Unit: 1 Introduction to Earth Science – The Evolution.
Radial Mixing in the Early Solar System: Meteoritic and Cometary Evidence Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen.
Survey of the Solar System
Astronomy 1 – Fall 2014 Lecture 7: October 23, 2014.
Sample return from C-type asteroids: What will we bring back? Paula Lindgren School of Geographical and Earth Sciences University of Glasgow SPACE Glasgow.
Hadean Eon & the formation of Earth
The Origin of Our Solar System Part 2
Meteors Updated july 19, Meteors – Comet dust particles entering our atmosphere and burning up from the friction. Every year about Nov. 18 the Earth.
Vagabonds of the Solar System Chapter 17. Guiding Questions 1.How and why were the asteroids first discovered? 2.Why didn’t the asteroids coalesce to.
Survey of the Solar System. Introduction The Solar System is occupied by a variety of objects, all maintaining order around the sun The Solar System is.
Meteorites I: Chondrites & Their Components Lecture 40.
Reading: Chapter 4 Lecture 6. Formation of the Moon, Absolute Ages, Radiometric Dating.
1. Amor asteroid -an asteroid whose orbit crosses the orbit of Mars.
Most meteorites that fall on Earth are fragments of broken-up asteroids which orbit the Sun mostly between the orbits of Mars and Jupiter. This is indicated.
Solar System Formation And the Stuff that was Left Over.
Asteroids (in space) and Meteorites (once they have entered the atmosphere) Meteorites hit the atmosphere with speeds from 12 to 72 km/s. Earth’s orbital.
Formation of Our Solar System
永島一秀, 小林幸雄, 坂本直哉, 殿谷梓, 圦本尚義 東工大・地球惑星科学 Presolar Silicates in meteorites Presolar Silicates in Primitive Chondrites Mar. 02, 2005 K. Nagashima, S. Kobayashi,
Chapter 19: Origin of the Solar System
Isotope chronology of meteorites and oxygen isotopes Part I: Radiometric dating methods Esa Vilenius Outline Introduction Rubidium-Strontium.
Comparative Planetology II: The Origin of Our Solar System Chapter Eight.
© 2010 Pearson Education, Inc. Chapter 8 Formation of the Solar System.
Lecture 32: The Origin of the Solar System Astronomy 161 – Winter 2004.
What makes up the Solar System and what force is holding it in place? The Force of Gravity hold our Solar System in Place. Things that make up our Solar.
Brief history of the universe. Atoms Atoms – consist of a dense nucleus of positively charged protons and uncharged neutrons surrounded by a cloud of.
Nucleosynthetic processes: Fusion: Hydrogen Helium Carbon Oxygen After Fe, neutron addition takes place (rapid and slow processes)
Nebula Charged ion stream Blew lighter gases to the outer solar system Provides evidence that they were formed at the same time as the Solar Nebula Light.
1B11 Foundations of Astronomy Meteorites Liz Puchnarewicz
Presolar Grains & Meteorites
Survey of the Solar System
Presolar Grains Bulk of material in the solar system is a mixture from a large number of stellar source---mixing in interstellar medium or during solar.
Pt. II: Oxygen Isotopes in Meteorites
Meteoroids, Asteroids Dwarf Planets
New View of Gas and Dust in the Solar Nebula
Meteoroids, Asteroids Dwarf Planets
Comparative Planetology II: The Origin of Our Solar System
SATISH PRADHAN DNYANASADHANA COLLEGE,THANE
Origin of 17,18O-rich materials from Acfer 094
Meteoroids, Asteroids Dwarf Planets
Presentation transcript:

Definition of “fossil” A fossil is defined as any remains, trace or imprint of a plant or animal that has been preserved by natural processes in the Earth’s crust from some distant geologic time and provides a record of Earth’s history from that time

Stromatolites, one of the oldest “fossils” of life on Earth

Meteorites as “fossils” of the earliest history of our Solar System Meteorites are also “fossils”, because they have preserved within them a record of the most ancient history of solar system material, a record not preserved in any other rocks. For example, dating of meteorites allows the determination of the time of formation of solid materials during the dawn of our Solar System, and of the mineralogic and isotopic composition of “Star dust”, material that formed in stars prior to the formation of our Solar System.

Chondrites are meteorites from broken-up primitive, undifferentiated asteroids that never melted. Thus, the properties of their constituents [calcium-aluminum-rich inclusions (CAIs), chondrules, matrix, and metallic Fe,Ni] are today as they were when the Solar System formed Chondrite NWA 5028

Radioactive parent isotopes, and stable daughter isotopes (decay products of the parent) and their half-lifes of common elements used in the dating of meteorites and other rocks

A classical and one of the earliest determinations of the age of an ordinary chondrite by Wasserburg and co-workers, using the Rb-Sr techniques. This primitive chondrite is 4.56 billion years old and, by inference, so is our Solar System!

When did the Solar System form: Ages of formation of the first solid materials in our Solar System Age of CAIs from CV chondrites: 4,567.4 ± 0.5 Ma Age of chondrules from CR chondrites: 4,564.7 ± 0.6 Ma (Amelin and Krot, 2002) Thus, chondrules formed 2.7 Ma after the formation of CAIs Sahara 192

The discovery of oxygen nuclear isotopic anomalies in carbonaceous chondrites In 1977, Clayton and co-workers discovered isotopic anomalies in the oxygen compositions of carbonaceous chondrites. They concluded that the origin of these anomalies can only be explained by nucleosynthesis, i.e., formation of the carriers of the anomalies in other stars, such as a supernova outside of, and prior to, formation of our Solar System

A grain of “stardust” a few microns in size of silicon carbide, SiC, whose isotopic composition indicates that it must have formed outside of, and prior to, the formation of the Solar System, most likely in a so-called AGB star

Raw materials for making stars and planets: Presolar grains and stellar nucleosynthesis Elements are made in the interiors of stars and returned to interstellar space Circumstellar (presolar) grains carry record of nucleosynthesis in a star Typical presolar grains are diamond, graphite, SiC, corundum (Al 2 O 3 ), spinel (MgAl 2 O 4 ), TiC. Sources: Supernova, AGB stars, novae, red giants, etc. We determine the structures and isotopic compositions of circumstellar condensates These data provide ground truth for testing theoretical models of star formation Graphite from Murchison CC TiC

The center piece of the W.M. Keck Cosmochemistry Laboratory: The Cameca 1280 Secondary Ion Mass Spectrometer (SIMS; Ion Microprobe)

Cameca 1280 Ion Microprobe and Isotope Scanning Microscope Most elements and their isotopes can be measured in µ- sized objects The precision of, for example, O-isotope ratio measurements approaches that achieved in a conventional gas source mass spectrometer Measurements preserve petrographic context A focussed primary beam of ~ 10 keV cesium or oxygen ions sputters secondary ions off of the surface of a polished thin section, and the secondary ions are analyzed in a magnetic sector mass spectrometer

From gas to dust to planets: Formation of our Solar System: The chemical elements formed in the interiors of stars. Dying stars ejected material into interstellar space, and presolar grains and amorphous material condensed in stellar atmospheres of stars such as Red Giants, AGB stars, and supernovae. These materials survived the long journey from the parent stars through the interstellar medium into cold molecular clouds whose cores collapsed to form new stars (e.g., our Sun), the planets, asteroids and comets. Asteroids broke up due to collisions with other asteroids, and the fragments (the chondritic meteorites) fell on Earth ~ 4.57 Ga after the solar system formed, bringing with them stardust from other stars that formed before formation of the solar system, as well as primitive solar system materials (CAIs, chondrules) that formed at the dawn of the solar system.,