1 “A Post Galileo view of Io’s Interior” Keszthelyi et al. Icarus 169 (2004) Raquel Fraga-Encinas Dec 7, 2004UMD TERPS Conference.

Slides:

Advertisements

Similar presentations

The Earth’s Interior Glencoe Ch Pages

Advertisements

Earth Structure & Plate Tectonics Notes

Warm up Write the questions!! 1.Describe the interior (Underground) of the Earth. 2.About how deep is the Earth going from one end to the other? Use page.

Interior of the Earth. I. Morphology of Earth's Interior.

Journey to the Center of Earth

Inside Edition The Earth’s Interior: A Hot Topic.

Digging Deep Into The Earth (C) Copyright all rights reserved

Europa Scenarios: Physical Models Ice-cracks on surface consistent with either “warm-ice” or water beneath the surface Near infrared mapping consistent.

Reading: Chapter 8 Lecture 29. Jupiter and the Galilean Moons; Tides and Friction.

b. a. Moons of Jupiter – total of 63 confirmed! Inner moons closer to Jupiter than Io.

Layers of the Earth.

EARTH`S LAYERS INNER CORE

Heat and Plate Tectonics

Section 13-1 Review Page #324:1-8.

The Layers of the Earth © Copyright 2006. M. J. Krech. All rights reserved.

1 SGES 1302 INTRODUCTION TO EARTH SYSTEM LECTURE 14: Rock Cycle & Magmatism.

Classification of Igneous Rocks

Igneous Rocks. The Nature of Igneous Rocks All igneous rocks are made of interlocking crystals of minerals that cool and crystallize our of magma. All.

Bellwork Obj: SWBAT describe the layers within the earth. 1.What happens to the temperature as you move from the crust to the core of the earth?

Earth on the Move Earth Structure & Plate Tectonics Notes.

Layers of the Earth Notes 10 Starter Layers of the Earth Notes 8/31/15 Application/Connection/Exit: Start Foldable Practice: Discussion: 9 Describe what.

Earth’s Interior (What’s down there below us?)

Chapter 5: Igneous rocks

Chapter 8: Terrestrial interiors. Interiors How might we learn about the interior structure of the Earth, or other planets?  What observations can you.

Igneous Rocks. The Rock Cycle The continuous and reversible processes that illustrates how one rock changes to another. “ One rock is the raw material.

STRUCTURE OF THE EARTH. Differentiation of Earth Earth is divided into layers based on density and composition Solid Layers – Core (iron-nickel) – Mantle.

Earth’s Interior Chapter 5 Section 1.

Earth’s Interior Structure

EQ: What are the names and locations of the main structural layers of the Earth? Layers of the Earth Notes 12 Starter Layers of the Earth Notes 9/1/15.

The Layers of the Earth!. Earth Layers The Earth is divided into 4 main layers.  Inner Core  Outer Core  Mantle  Crust.

Inside the Earth Planet Earth All objects on or near Earth are pulled toward Earth’s center by gravity. Earth formed as gravity pulled small particles.

Chapter 12: Earth’s Interior

Chapter 12 Section 4 - Volcanoes.  Movement along a fault causes a decrease in pressure – decompression  A decrease in pressure causes a decrease in.

CHAPTER 10 Section 1 Objectives  Describe the movement and formation of magma.  Define volcanism  List the three locations where volcanism occurs.

Convection Current in the Mantle SAYRO PAW. The Four Layers of Earth Inner Core Outer Core Mantle Crust The inner core is the hottest layer in the Earth.

Layers of the Earth.

Today’s Learning Target: We will be able to describe structures and layers of the earth and explain how we know about the structure.

The Earth’s Interior.

TEKS: 6.10A. Inner Core  Thickness:  Composition:  Temperature:  Interesting Fact(s): 1,250 km Solid Fe 6,000°C The deepest, most dense layer in.

Earth’s Layered Structure. PHENOMENON: What did you observe? What evidence do you have? OBJECTS: Define the system. What objects are interacting? MOTION:

Terminology Volcanoes Wildcard I Wildcard II Wildcard.

Earth’s Layers. The Layers: Lower mantle Transition region.

Volcanoes A volcano is a mountain that forms when magma reaches the surface. Magma rises because it is less dense than the solid rock around and above.

TEMPERATURE  The deeper you go, the hotter it gets. & Celsius 4,000° C 4,000 km 2,000 km & kilometers 5,000° C 6,000 km F F mi.

Igneous Rocks December 7-8,   Melted rock that cools & crystallizes at or below the surface Igneous Rocks.

Earth’s Layered Structure

The Giant Planets Jovian Planets.

Thursday, 1/29/2015 Objectives: Describe Earth’s interior.

Earth’s Layers.

Digging Deep Layers of the Earth Day 2

Schedule for Today Greetings Expectations Rules are the same Homework

Imagine a journey to the centre of the Earth…

Crust and mantle are solid rock not liquid

Earth’s Layers.

Earth’s Structure.

The Layers of the Earth!.

Structure of the Earth.

6.E.2.1 Structure of the Earth Vocabulary

Earth: Systems, Structures and Processes

5.1 Lecture Igneous Rocks.

Today’s Plan Warm Up: Journey to the Center of the Earth Writing

Layers of the Earth.

Earth’s History Flip book

Earth’s Internal Heat.

Igneous Rocks Chapter 5.

5% of all known volcanoes in the world are not located close to a plate margin. These are known as intraplate volcanoes and occur as a result of mantle.

Earth’s Interior Chapter 5 Section 1.

Layers of the Earth.

Presentation transcript:

1 “A Post Galileo view of Io’s Interior” Keszthelyi et al. Icarus 169 (2004) Raquel Fraga-Encinas Dec 7, 2004UMD TERPS Conference

2 View right after Voyager flybys Completely molten interior (Peale 1979) Thin lithosphere flexed by tidal forces causes tidal heating Underlying basaltic magmas drive up sulfur eruptions

3 View right before Galileo flybys Thick cold lithosphere (> 30km) Aesthenospheric heating model ( Ross et al. 1990) Io’s interior considered largely solid (Nash et al. 1986)

4 Galileo Mission Observations SSI (0.4–1 um), NIMS ( um), PPR (visible-100 um) Timeline: Pillan Patera eruption T = /- 25 K SSI color data – hottest spots were darkest near 1 micron : presence of “enstatite” Limits: superheating due to rapid ascent or tidal heating of materials

5 Modeling MELTS numerical thermodynamic model from published data Assume Pressure ~ 100Mbar Upper mantle ~ 50% molten, core boundary 10-20%

6 Post-Galileo View Io & Implications Core: molten Fe-S mix, size = km Mantle: molten ~ 10% base to ~ 50% upper (enstatite composition) Crust: at least 13km thick (continually recycled into mantle) Can explain features like paterae & plumes

7 Concluding remarks This latter model is closer to what was proposed on the 70’s than prior to the Galileo mission Uncertainties on lava temperatures? Need more data

8 RIGHT: Si magma (red) rises thru rock, not buoyant enough to reach volatiles (navy). Heat melts S (yellow) and SO2 (light blue) when it vaporizes erupts into surface. Depression forms and can be unroofed forming the patera. LEFT: Orange (warm S) black spot (Si unroofed)

9 L/LL-chondrites have low Fe content, have olivine & pyroxene IO INFO Mass = 8.94E25 g Radius = 1821 km Av. Density = 3.53 g/cc

10