Between a Rock and a Hard Place: Can Garnet Planets Be Habitable?

Slides:

Advertisements

Similar presentations

The nebular hypothesis

Advertisements

Mantle composition 1800s meteorites contain similar minerals to terrestrial rocks Hypothesis that meteorites come from asteroid belt and originate from.

Mercury’s origin and evolution:- Likely evidence from surface composition David A Rothery 1, J Carpenter 2, G Fraser 2 & the MIXS team 1 Dept of Earth.

Chemical Models of Protoplanetary Disks for Extrasolar Planetary Systems J. C. Bond and D. S. Lauretta, Lunar and Planetary Laboratory, University of Arizona.

Plate tectonics Image from

Astr The origin and early evolution of the solar system.

Earth Astronomy 311 Professor Lee Carkner Lecture 12.

PY4A01 Solar System Science Lecture 2 - Minimum mass model of solar nebula oTopics to be covered: oComposition and condensation oSurface density profile.

Mercury. Mercury’s Orbit Mercury has a short year. –88 Earth days = 1/4 Earth year –0.4 AU from the Sun This is predictable from Kepler’s third law. –The.

The Solar System.

Essentials to Life A description of factors that have allowed complex life to evolve on Earth as noted in Rare Earth: Why Complex Life is Uncommon in the.

The Diversity of Extrasolar Terrestrial Planets J. Bond, D. Lauretta & D. O’Brien IAU Symposium th August 2009.

Astro 101 Slide Set: Kepler’s Exoplanet Discoveries Exceed 1,000 0 Topic: Exoplanets Concepts: Transit Detection, Exoplanet Statistics Mission: Kepler.

Geochemical data. All electromagnetic waves travel at the speed of light (3 x 10 8 ms -1 ) and are discussed in terms of wavelength and frequency The.

The Chemistry of Extrasolar Planetary Systems J. Bond, D. O’Brien and D. Lauretta.

Chapter 22 ISCI 2001 Structure of the Earth Tectonics.

Earth By: Ethan Saffier. Earth’s Symbol How did earth get its name? Earth means “The planet inhabited by humans”

The Diversity of Extrasolar Terrestrial Planets J. Carter-Bond, D. O’Brien & C. Tinney RSAA Colloquium 12 April 2012.

The Sun & The Solar System. Structure of the Sun The Sun has layers which can be compared to the Earth’s core, mantle, crust, and atmosphere All of these.

Solid Earth System. The Earth is like an onion, it is made up of many layers. Although we have not been to the center of the Earth, Earthquakes, and volcanoes.

Geologist A scientist who studies the Earth as well as the processes and history that have shaped it.

Structure of the Earth and Mineralogy Environmental Science Earth Science Unit Environmental Science Earth Science Unit.

Our Earth & Moon (Chapter 16). Student Learning Objectives Compare and contrast interior structures of the Earth & Moon Describe surface features for.

Atmosphere: Jupiter’s atmosphere has two basic features. 1) Changing parallel bands aligned with the equator, and 2) the Great Red Spot.

The Core and Mantle: future prospects for understanding the Deep Earth

Formation of Earth Birth of the Solar System Nebular Theory

Magma Oceans in the Inner Solar System Linda T. Elkins-Tanton.

The Chemistry of Extrasolar Planetary Systems Jade Bond PhD Defense 31 st October 2008.

Earth Astronomy 311 Professor Lee Carkner Lecture 12.

1 - EARTH STRUCTURE & DIMENSIONS 2 - LAYERS OF THE EARTH 3 - ELEMENTS OF THE EARTH EARTH’S INTERNAL STRUCTURE.

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.

Unique Properties of the Earth. 1. Due to the location in the solar system the Earth is not too hot and not too cold… it’s just right for life.

Goal: To understand life in our universe. Objectives: 1)To understand the Basic building blocks for life in general 2)To learn about the basics of climate.

EART 160: Planetary Science 11 February Last Time Paper Discussion: Stevenson (2001) –Mars Magnetic Field Planetary Interiors –Pressure inside Planets.

Layers of the Earth These notes go on p. 5 of your INB.

Magmatism on Super-Earths: What do we expect to see?

The Earth’s Interior and how it works..

Atmosphere: Jupiter’s atmosphere has two basic features

Image of the day.

Section 1: Earth: A Unique Planet

Asteroseismology of Kepler

Visualizing Earth Science

Solid Earth System.

Astronomy 340 Fall September 2005 Class #7.

Chapter 3 Introducing Earth

Theme: Earth Class: Sciences Name: Alexa Gabriela Montoya Alvarez Teacher: Mrs. López Date: 05/03/2018.

Earth’s Interior.

Earth’s Interior Structure

EARTH’S INTERNAL STRUCTURE

• Sun’s ignition clears the solar system

Class 8. Mantle Melting and Phase Diagrams William Wilcock

Frontiers in Exoplanet Research

So Hot! Why? Early Earth 4.6bya.

Earth Layers Powerpoint for day 1 of Earth Model activity. 5 slide powerpoint meant to be shown at beginning (and maybe end) of class. Should last 5-10.

A good review… Use this PowerPoint to review the concepts that include all the layers of the Earth. This will be one helpful source to prepare for the.

Geology and Earth’s Structure

Section 1: Earth: A Unique Planet

We have been talking about minerals primarily in the earth’s crust

So Hot! Why? Early Earth 4.6bya.

So Hot! Why? Early Earth 4.6bya.

Exploring Our Beloved Earth

1-2. FORMATION & EVOLUTION OF The Earth

Warm-Up List one example of something that exists in each of the different spheres.

We have been talking about minerals primarily in the earth’s crust

Layers of the Earth.

Planets of the Solar System

Crust mantle Outer core Inner core.

Presentation transcript:

Between a Rock and a Hard Place: Can Garnet Planets Be Habitable? Presenter: Johanna Teske Carnegie Institution for Science Wendy Panero Jennifer Johnson Cayman Unterborn Scott Hull

How do we determine exoplanet compositions? Atmosphere spectroscopy, direct imaging Planet mass and radius Host star composition Degenerate; multiple possible compositions Possible only for a small # of planets Initial planet-forming ingredients help place constraints In fact, this conclusion is further complicated studies that have shown that there is considerable degeneracy in these mass-radius relations (e.g., Dorn et al., 2015), with multiple compositions, core mass fractions, and mantle mineralogies producing planets of similar density. Fortunately, the degeneracy in these models is greatly reduced when the composition of the host star is assumed to be a proxy for that of the exoplanet, acting as a powerful third constraint.

How is exoplanet composition related to habitability? Flowchart representing the concept of whole planet coupling. Climate influences tectonics through the role of surface temperature in a planet's tectonic regime (i.e., stagnant lid versus plate tectonics), while the tectonic regime in turn affects climate through volatile cycling between the surface and interior. The tectonic regime also influences whether a magnetic field can be generated by dictating the core cooling rate. Finally, the strength of the magnetic field influences atmospheric escape, and therefore long‐term climate evolution.

How is exoplanet composition related to habitability? Earth-likeness? Sustained surface liquid H2O Atmosphere & Climate atmospheric escape surface temperature rock weathering volatile recycling Magnetic Field Tectonics Flowchart representing the concept of whole planet coupling. Climate influences tectonics through the role of surface temperature in a planet's tectonic regime (i.e., stagnant lid versus plate tectonics), while the tectonic regime in turn affects climate through volatile cycling between the surface and interior. The tectonic regime also influences whether a magnetic field can be generated by dictating the core cooling rate. Finally, the strength of the magnetic field influences atmospheric escape, and therefore long‐term climate evolution. core cooling Based on Foley & Driscoll 2016, Fig. 1

Different composition From Star to Planet Solar composition condensation of elements from nebula differentiation into core, mantle, crust evolution over time Host star abundances from SDSS/APOGEE How Earth-like? Different composition Planet is Kepler-22b Orbits G5 star Less metals than sun Not to scale Image credits: NASA/Ames/JPL-Caltech

Olivine vs. Garnet X3Y2(SiO4)3 (Mg,Fe)2(SiO4) X=Ca, Mg, Fe, or Mn Y=Al, Fe, Cr Si-rich (Mg,Fe)2(SiO4) Mg-rich Olivine less stiff than garnet -- helps plate tectonics

Different abundance patterns result in drastically different planets. Kepler 102 Olive Kepler 407 Janet Image credit: Robin Dienel, Carnegie/DTM Different abundance patterns result in drastically different planets. Mg/Si for Kepler-102 = 1.23, Mg/Si for Kepler-407 = 0.78 Mg/Si for Sun = 1.04 cpx - clinopyroxene (commonly augite/diopside): Ca(Mg,Fe)Si2O6 - bright green.opx - orthopyroxene (commonly enstatite): (Mg,Fe)SiO3 - dark green/brown ol - olivine, with three phases that vary by pressure, alpha (just olivine - olive green), beta (also called wadsleyite- blue green), gamma (also called ringwoodite - brilliant blue). gt - garnet here, composition is (Mg,Fe)3Al2Si4O12 (pyrope, deep red/red wine)

Different abundance patterns result in drastically different planets.

Between a Rock and a Hard Place: Can Garnet Planets Be Habitable? The host star abundances from SDSS/APOGEE give us important constraints on exoplanet interior composition and structure. Our results point to a wide variety in known rocky planets. We can use this new information to assess how Earth-like exoplanets are. @johannateske @APOGEEsurvey @sdsssurveys @CarnegiePlanets @CarnegieAstro @CarnegieScience