News• Global Warming: Northern hemisphere warms faster,

affecting rainfall patterns. http://www.sciencedaily.com/releases/2013/04/130402162559.htm

• Hungry black hole wakes up for a planet-sized

snack

• Supernova Remnant 1987A Reveals Its Secrets

• New Insights on How Spiral Galaxies Get Their Arms

• Monkeys Show Why Middle Managers Get Stressed

AST101 Lecture 18

Extra Solar Planets

Finding Planets1. Direct Imaging

HR 8799

Direct Searches

Direct searches are difficult because stars are so bright.

How Bright are Planets?

Planets shine by reflected light.

The amount reflected is the amount received (the solar constant)

- Times the area of the planet

- Times the albedo (reflected), or - Times (1-albedo) (emitted)

Lp = L*/4πd2 a πRp2 ~ L* (Rp/d)2

For the Earth, (Rp/d)2 ~5 x 108

For Jupiter, (Rp/d)2 ~108

How Bright are Planets?

You gain by going to long wavelengths,where the Sun is relatively faint, and the planet is relatively bright.

How Far are Planets from Stars?

By parallax, 1 AU = 1“ at 1 pc•1 pc (parsec) = 3.26 light years•1“ (arcsec) = 1/3600 degree

As seen from α Centauri (4.3 LY):•Earth is 0.75 arcsec from Sol•Jupiter is 4 arcsec from Sol

Can we see this? Yes, but it takes special techniques, and is not easy.

HR 8799(A5V)

Finding Planets

2. Transits

Finding Planets

2. Transits

Transits

Transits requires an edge-on orbit.•Jupiter blocks 2% of the Sun's light•the Earth blocks about 0.01%.

Artist’s ConceptionVenus, 8 June 2004

Finding Planets

3. Astrometric Wobble

Finding Planets

4. Doppler Wobble

OrbitsPlanets do not orbit the Sun - they both orbit the center of mass.

The radius of the orbit is inversely proportional to the massThe radius of the Sun’s orbit with respect to the Earth is 1/300,000 AU, or 500 km

R1 M1 = R2 M2; a = R1 + R2

This is Newton’s law of equal and opposite reactions.

Orbital Velocity V = 2πr/P• r is the radius of the orbit• P is the orbital period• V is the orbital velocity

How fast does the star “wobble”?

Kepler’s 3rd law: P2 = a3 a ~ rp (M* >> Mp)r* = mp/m* rp (center of mass)

V* = 2π mp/m* /(rp)1/2

V⊕ = 2 cm/s; VJ = 3 m/s

51 Pegasi b

Doppler Wobble: Gliese 876

The three planets of Gl 876: masses = 2.5 MJ, 0.8 MJ, and 7.5 M⊕

Gliese 876

M4V star3 planets, including the least massive known (0.75 M⊕)

Extrasolar Planetary Systems

55 Cancri (G5V): 5 planets•1 MU 0.4 AU•1 MJ 0.15 AU•1 Ms 0.25 AU•0.5 MJ 0.8 AU•4 MJ 5 AU

Biases and Limits

Extrasolar Planets

Planets are preferentially found around metal-rich stars

- mostly younger than the Sun.

Habitable Zones

Refer back to our discussion of the Greenhouse Effect.

Tp ~ (L*/D2)0.25

The habitable zone is the region where the temperatureis between 0 and 100 C (273 and 373 K), and water canbe liquid.

Tp depends on both the solar luminosity L* and thedistance D.D does not change, but L* does, as the star evolves.

Faint Young Sun Problem