Exo planets media John Bally - Laboratory for Atmospheric ......The Search for Exo-planets: • The...

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John Bally 1 1 Center for Astrophysics and Space Astronomy Department of Astrophysical and Planetary Sciences University of Colorado, Boulder Searching for Searching for Other Worlds: Other Worlds: The context The context

Transcript of Exo planets media John Bally - Laboratory for Atmospheric ......The Search for Exo-planets: • The...

Page 1: Exo planets media John Bally - Laboratory for Atmospheric ......The Search for Exo-planets: • The Context: The Age of Discovery - Our generation is charting the Universe! - Origns

John Bally1

1Center for Astrophysics and Space Astronomy

Department of Astrophysical and Planetary Sciences

University of Colorado, Boulder

Searching forSearching for Other Worlds:Other Worlds:

The contextThe context

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The Search for The Search for Exo-planetsExo-planets::

• The Context: The Age of Discovery

- Our generation is charting the Universe!

- Origns of the cosmos, stars, planets, and life

• How common are terrestrial (habitable) planets?

- History

- Astrobiology: The origins of life on Earth

In-situ searches in the Solar System

Remote-sensing biosignatures

• Methods of Discovery: Past, present, future (Saturday talk).

- Astrometry

- Radial velocity

- Transits

- gravitational lensing

- Direct detection, imaging, characterization

• Mission Development: From Concept to Flight to Science

- COROT, Kepler, SIM, TPF, Darwin , Starshade, Planet Imager, ….

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The Age of Astronomical DiscoveryThe Age of Astronomical Discovery

• Access to all wavelengths of the spectrum

- Silicon technology

=> sensors at most wavelengths

- Large telescopes

• Powerful computers

• Access to space

- No atmosphere

=> Sharp images (Hubble Space Telescope)

=> Access to all wavelengths (Spitzer)

• Connections to Physics

- Scales: 1028 to 10-33 cm, 1017 to 10-43 sec

- 4 forces: gravity, electro-magnetism, weak, strong

- Matter (4%), Dark matter (24%), Dark energy (72%)

= blXa

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Mauna Kea Observatory: Wei-Hao Wang

Subaru Keck

NASA IRTF

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Gemini N

8 meter on

Mauna Kea

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Hubble Space Telescope

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3 Million years ago: M51 grand design spiral

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Wei-Hao Wang

Summer Milky Way

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Our Milky Way @ visual wavelengths

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Our Milky Way @ near infrared wavelengths

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Our Milky Way @ far infrared wavelengths

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Cosmic Microwave Background:

Snapshot of 3,000 K plasma when Universe was 300,000 yrs old

Redshifted by Expansion of the Universe x1,000 => 3 K

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Dark Energy: Expansion is accelerating!

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The Evolution ofThe Evolution of the Universe:the Universe:• Cosmology: Baryons = 4% 13.7 Gyr

Dark Matter = 26% (1 Gyr = 109 years)

Dark Energy = 70%

• Cosmic Microwave Background:

The young Universe 400,000 years

Hot, ionized plasma 3,000 Kelvin

(1/2 temperature of Sun)

Smooth to 1:105

• The Cosmic Dark Ages: 0.0004 – 0.6 Gyr

• The First Stars: Massive 0.6 – 1 Gyr

• Formation of Galaxies > 1 Gyr

• Solar System Formation: 9.1 Gyr

• Star & Planet Formation today

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Stars Stars

Stars: The fundamental building blocks of the Universe

High mass: (8 - 100 times Mass of Sun)

Short lived: < 30 million years

Source of energy in interstellar medium

Explode as supernovae

Long Lived: > Billion years

(Lock up mass for long time)

Luminous: Thousand => million times Sun

Faint:

Planets: Abodes of life

Sources of light, chemical elements

Low Mass: (< 2 times Mass of Sun)

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16

4 million

Year-old

Cluster

+

Ionized

Nebula

+

Surviving

cloud

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16

(HST)

Surviving

cloud

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Where planets also form

• Giant Molecular Cloud Core

• Gravitational Collapse & Fragmentation

• Rotation & Magnetic Fields

Raw material for star birth

Proto-stars, proto-binaries, proto-clusters

Accretion disks, jets, & outflows

Shrink size by 107; increase density by x 1021 !

Star FormationStar Formation

• Planets

C. LadaMost may form in clusters!

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[S ] [O ]

Class I Outflow: HH 46/47

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Spitzer IRAC: 3 – 8 μm

Class I Outflow: HH 46/47

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HH 46/47

(Hartigan et al. 05, AJ

BR06)

HST 1994

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HST 1997

HH 46/47

(Hartigan et al. 05, AJ

BR06)

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The Orion

Star Forming

Complex

Wei-Hao Wang

Pleiades

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Infrared view of winter sky (10 - 120 μm)

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Orion NebulaOrion Nebula

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d253-535 in M43 Smith et al. 05

Planets in Formation?

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Young Proto-planetary Disk

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Evolution of

A Star:

• Birth

• Main-sequence

life

- fusion: H=>He

• Death

> 60 M:

black hole

8 – 60 M:

neutron star

< 8 M:

white dwarf

The Sun ….

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Death of a low-mass star: Death of a low-mass star: Core collapses to for white dwarf

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Eta Eta Carina nebulaCarina nebula

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Eta-CarinaEta-Carina: Massive star about to die: Massive star about to die

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Remnant of the Supernova of 1054 (Crab Nebula)

Page 37: Exo planets media John Bally - Laboratory for Atmospheric ......The Search for Exo-planets: • The Context: The Age of Discovery - Our generation is charting the Universe! - Origns

• Stellar Reflex Motion:

- Periodic Doppler variation

- Periodic Position change

• Transits (planet blocks light)

• Gravitational Lensing

• Direct detection in images

The Search Extra-Solar PlanetsThe Search Extra-Solar Planets

Hard: Earth 1010 (10 billion) x fainter than Sun!

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Direct imaging of Direct imaging of exo-planets exo-planets is Hard:is Hard:

10 10 Sun

Earth

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>> 200 planets:200 planets:

Most located

inside Earth’s orbit

Goeff Marcy

Paul Butler

Earth

radial velocity method

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> 200 planets: Gas Giants like Jupiter200 planets: Gas Giants like Jupiter

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Orbit eccentricity

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The Metallicity Effect:

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The End