1 Assembling the puzzle From Earths to Super-Earths Hitran to the rescue... “ Good planets are hard to find ” Bracewell Lisa Kaltenegger Harvard-Smithsonian.

Slides:

Advertisements

Similar presentations

1 Biomarkers in terrestrial planet atmospheres Super-Earths & Life a fascinating cross-disciplinary puzzle Lisa Kaltenegger MPIA/Harvard University IAUS276,

Advertisements

Kaltenegger et al Presented by Craig Malamut December 4, 2012.

Life Sustaining What’s needed of stars? Stablility.

Colors of Alien Worlds from Direct-Imaging Exoplanet Missions Renyu Hu Hubble Fellow Jet Propulsion Laboratory California Institute of Technology With.

Biomarkers in Super Earth Atmospheres: Photochemical Responses John Lee Grenfell Zentrum für Astronomie und Astrophysik, Technische Universität (TU) Berlin.

Chapter 19: Future climate evolution/Habitable planets around other stars.

Venus. Venus Data Guiding Questions 1.What makes Venus such a brilliant “morning star” or “evening star”? 2.What is strange about the rotation of Venus?

Click to listen Early atmosphere ~4.5 billion years ago Mostly Hydrogen and Helium Escaped into space Outgassing of water vapor and CO2 created a secondary.

Greenhouse Gases and Energy Budget LP 3 1. What are the greenhouse gases? Where do they come from? How do they work? 2.

Earth Astronomy 311 Professor Lee Carkner Lecture 12.

I’m very HOT! Keep out! It’s very cold here! Ha! Ha! I’m not too cold or too hot! It’s OK here! What makes Earth‘s climate so moderate?

Greenhouse Gases and Energy Budget LP 3 1. What are the greenhouse gases? Where do they come from? How do they work? 2.

Atmosphere The atmosphere is a very thin layer of gases wrapped around the earth.

Astronomy190 - Topics in Astronomy

Earth Astronomy 311 Professor Lee Carkner Lecture 12.

Detecting molecules in the atmospheres of transit Exoplanets Giovanna Tinetti University College London Mao-Chang Liang Academia Sinica, Taiwan.

1 Lecture 17: How to Find Life on Exoplanets: Biosignatures.

Dr. David Crisp (Jet Propulsion Laboratory/California Institute of Technology Dr. Victoria Meadows (California Institute of Technology) Understanding the.

Searching for Life Beyond The Solar System Dr. Victoria Meadows NASA Astrobiology Institute Spitzer Science Center/California Institute of Technology.

The Solar System.

Biosignatures: Alien’s View of Earth ASTR 1420 Lecture : 18 Section: Not from the textbook.

Lecture 34. Extrasolar Planets. reading: Chapter 9.

Planet Formation and the solar system REVIEW. The raw materials to form planets come most directly from what source?

Earth’s Atmosphere Chapter 3, Section 2

1 Atmospheric Radiation – Lecture 11 PHY Lecture 20 Comparative atmospheres: Mars, Earth & Venus.

Earth Astronomy 311 Professor Lee Carkner Lecture 12.

Energy from the Sun Radiation is the transfer of energy by electromagnetic waves. Ninety-nine percent of the radiation from the Sun consists of visible.

Earth Astronomy 311 Professor Lee Carkner Lecture 12.

Nigel J Mason Physics & Astronomy The Open University, UK.

Chapter 7e Earth is a living planet. 7.5 Earth as a Living Planet Our Goals for Learning What unique features on Earth are important for human life? How.

Cole Nachman. Symbol Why the name Neptune? ❏ Urbain Le Verrier discovered planet. ❏ Claimed right to name discovery.

Lecture 16: Super-Earths: a New Type of Planet Planets vs. Stars Internal structure Geochemical cycles Habitability.

Inhabited exomoon by artist Dan Durda. Imagine a terrestrial-type exomoon orbiting a Jovian-type planet within the habitable zone of a star. This exomoon.

Lecture 6 6/11/07 Ast Earth’s Atmosphere The Earth’s atmosphere has several very important properties: –Just enough warmth –Just enough pressure.

Lecture 35. Habitable Zones. reading: Chapters 9, 10.

Greenhouse Gases and Energy Budget LP 3 1. What are greenhouse gases? Where do they come from? How do they work? 2.

The role of climate Ecology unit 3 lecture 1. What is climate? Climate: average, year-round conditions in a region Weather: the day-to-day conditions.

Origin, Evolution, and Composition of the Atmosphere

The Greenhouse Effect What is the greenhouse effect? Interaction between planet’s atmosphere, star’s light Results in heating of planet What causes the.

Biosignatures: Alien’s View of Earth ASTR 1420 Lecture : 19 Section: Not from the textbook.

HOW DID WE GET HERE?? EARTH AND THE ORIGIN OF LIFE.

Life in the Milky Way: Panel Discussion Wesley A. Traub Chief Scientist, NASA’s Exoplanet Exploration Program Jet Propulsion Laboratory, California Institute.

Habitable Zones and the Occurrence of Potentially Habitable Planets James Kasting, Ravi Kopparapu, Ramses Ramirez *, and Sonny Harman Department of Geosciences.

Homework 8 Due: Monday, Nov. 28, 9:00 pm, Exam 2: Weds., Nov. 30.

Planetary atmospheres

Characterizing Habitable Worlds... From the Moon Margaret Turnbull - STScI / Carnegie.

Chapter 7d Hothouse Venus. Venus Orbital distance: – km (0.72 AU) –NOT Eccentric Year: –224.7 d Day: – d –Retrograde rotation Temperature:

The Origin of the Atmosphere

PLANETARY GEOLOGY. Discuss the factors that affected the geologic processes and formations of the planets Outline the information in the 6 slides Use.

The Atmosphere.  Nitrogen (78%)  Oxygen (21%)  Water Vapor (less than 4%)  Carbon Dioxide (less than 1%)  Methane (less than 1%)  Nitrous Oxide.

National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Navigator Program Exploring New Worlds Exoplanet.

Earth Astronomy 311 Professor Lee Carkner Lecture 12.

Habitability: Making a habitable planet 26 January 2016.

Planets of the Solar System Section 1 Section 1: Formation of the Solar System Preview Key Ideas The Nebular Hypothesis Formation of the Planets Formation.

Greenhouse Effect Sun Earth’s Temperature Solar Energy Solar Energy Solar Energy Solar Energy.

27-1OBJECTIVES Explain the nebular hypothesis of the origin of the solar system Describe how the planets formed Describe the formation of the land, the.

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.

WEATHER Texas 2012 Texas 2012 what is happening in the air, right here, right now Climate- long term weather patterns.

Climate & Biomes. Weather Short term day to day changes in temperature, air pressure, humidity, precipitation, cloud cover, & wind speed Result of uneven.

The Greenhouse Effect. Natural heating of earth’s surface caused by greenhouse gases –CO 2 (Carbon Dioxide) –CH 3 (Methane) –N 2 O (Nitrous Oxide) –H.

The Dynamic EarthSection 2 Objectives Diagram the % composition of Earth’s atmospheric gasses. Label the layers of Earth’s atmosphere. Identify three mechanisms.

National Aeronautics and Space Administration Wesley A. Traub Jet Propulsion Laboratory, California Institute of Technology Advantages and Strategies for.

Atmospheric Heating.

Goal: To find life in our universe.

Terrestrial Planet Finder - Coronagraph

Image of the day.

Advantages and Strategies for Direct Imaging and Characterization of Exoplanets: 5-minute Summary Wesley A. Traub Jet Propulsion Laboratory, California.

Habitability: Making a habitable planet

Section 1: Formation of the Solar System

What is a Habitable Zone?

Presentation transcript:

1 Assembling the puzzle From Earths to Super-Earths Hitran to the rescue... “ Good planets are hard to find ” Bracewell Lisa Kaltenegger Harvard-Smithsonian Center for Astrophysics HITRAN Conf, June 22th 2008

2 Planets... The story so far...

3 New worlds in our sky shadows of weird worlds... What can we tell?

4 The KEY... Transiting planets Torres 2008 Fortney, 2007 Sasselov 2007

5 Weather forecast on Giant exoplanets? Atmosphere by transits... HD189733b Tinetti et al 2007

6 WHY ?

7 The Pale Blue Dot Voyager image, 400 billion km away

8 Earth IR-emission TES data; Christensen 2004 Kaltenegger, Traub, Jucks 2007 (ApJ)

9 Line of Evidence WHAT KIND INTERIOR ATMOSPHERE LIFE ? Density ? (radius/mass) Plate tectonics? Ocean/land? What chemistry? What star ? HZ ? What biota? FORMATION Formation Models

10 Line of Evidence FIND INTERIOR ATMOSPHERE LIFE ? SPECTRAL FINGERPRINT

11 add OUTLINE CODES Climate (Kasting, Segura, Pavlov) Photochemistry (Segura, Kasting) Radiative Transfer (Traub, Jucks) Planet interior & outgassing Cloud physics (CO 2 & H 2 O) add Kaltenegger et al 2007

12 Signs Of Life On An Earth-like Planet Vegetation Plant product Plant life Bacteria observed Water Oxygen Carbon dioxide Methane Nitrous oxide Ozone Needed for life Primordial; & bacteria product

13 Selsis 2007

14 Spectral features IR & Is there Take out ? Traub & Jucks, AGU, 2002; Des Marais et al. 2002, Selsis 2003, Kaltenegger 2007

15 Atmospheric escape Outgassing Early or continuous Geochemical recycling e. g. carbonate silicate cycle Biological processing photochemistry

16 LIFE

17 Selsis (data Kasting et al 93) Update Kaltenegger & Segura (prep) The Test...The possibilities...Characterizing planets

18 Habitable Zone... Goldilocks Zone Selsis, Kasting et al 2007; Kaltenegger & Selsis 2007

19 Paillet et al., in prep TPF-C New World Finder CIS for Exoplanets: Spectral Fingerprints

20 Earth part of the puzzle... & a universe full of possibilities Sontin et al 2007 Leger et al 2004

21 How to make water from a H 2 -rich atmosphere ? Reduction of Fe-bearing silicates by H 2 (Sasaki, 1990) For f O 2 ≤ core formation H 2 0/H 2 ~ 0.1 (Solar nebula : 6 x Delivery?) H 2 O vapor promotes greenhouse: Earth’s temp. as high as 4800 K

22 Earth Evolution over geological time Kaltenegger et al 2007 ApJ

23 Continuous habitable zone Goldilocks Zone Gl 581c... HOT, Gl581d COLD Selsis et al 2007, Kaltenegger et al 2008, Seager et al 2008, Miller-Ricci et al 2008,...

24 Super Earth around M star 3400K Tidally locked planet 1: day (60%) night side (40%) 2: day (75%) night side (25%) 3: day (85%) night side (15%) Kaltenegger et al 2008 (in prep)

25 Super Earth around M star 3400K Tidally locked planet (rapidely rotating planet comparison line (shown in grey)) Scenario 3: high heat transport from day (85%) to night side (15%) Kaltenegger et al 2008 (in prep) CO 2 O3O3 CH 4 H2OH2O H2OH2O

26

27 Transits... Pushing the limits Kaltenegger, Traub, Jucks 2008 (sub) Radius +/- ~ 0.06%

28 Transits... Detecting habitable atmospheres Kaltenegger, Traub, Jucks 2008 (sub)

29 Hitran Shopping list Near-IR lines (CH 4 ) Line profile (especially wings - Transits) Self broadening... Line broadening High atm pressure (< 3 bar) –(= high gravity on Super-Earths) Transits probe upper Earth atmosphere mainly Warming and cooling of atmosphere –e.g. dense and early Earth atmospheres –…

30 LIFE SUPER EARTHS... opportunity & challenge

31 Habitabitity of Super Earths Gl581d Gl 581d: Earth Amtosphere, 2.63 bar, 1.8x Earth gravity. M star 3200K Scenario 1: no heat transfer day & night side (freeze out on dark side) Scenario 2: Planet rapidely rotating like Earth (same temperature day and night side) Scenario 3: Low heat transfer between day (75%) & night side (25%), no freeze out Kaltenegger et al (in prep)