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## PowerPoint Slideshow about ' Extra Solar Planets' - asa

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### The first—51 Pegasi b (Bellerophon )

### 51 Pegasi B

### How do we know this

### Problem: not all systems are edge on! We don’t always know the tilt!Thus the mass measured is a minimum mass

### Limits of Radial velocity measurements

### Hot Jupiters!

The planet

Star51 Pegasi

ConstellationPegasus

Distance50.9 ± 0.3 ly(15.61 ± 0.09 pc)

Spectral typeG2.5IVa or G4-5Va

Mass(m)1.06 x Mass of Sun

Radius(r)1.237 ± 0.047 Rsun

Temperature(T)5571 ± 102 K

Metallicity[Fe/H]0.20 ± 0.0

Age6.1-8.1 Gyr

Radial velocity of Star

It move toward and away from us with period of 4.2 days.

Here mp = 0, we can can know exact mass.

Here I = 90..can’t determine mp

In General, mass listed is really: M sin i

where i is inclination of orbit

Then a bit of algebra….and

Astronomers know star masses from their spectra and lots of work from predecessors over the years!

Vstar and p are obtained from the radial velocity graph!

Star surfaces move up and down about 1 m/s, so this is smallest practical speed for star.

Big Planet close to small star creates the biggest wobble, so we can see these most easily.

To see a complete wobble, we need to watch for one period—hard to do for planets more distant than a few AU’s.

Earth Makes sun move about 1 cm/s, so this would be lost in the Noise of the sun if someone was trying to detect us!

So guess what we found around sun like stars ?

Here are the first nine planets discovered (as of 1997)

So where are we know (2010)

Note 20 multiple planet systems!

So how are they finding smaller or more distant planets?

Use Astrometry (motion of stars in photographs)

Watch for longer time periods! (its been 12 years now!)

- Improve precision of methods (techology continues to improve)
- Gets lots more people doing it!
- Search around smaller stars!
- Use Transit Photometry for edge on systems (finds smaller planets?)
- Lets see how these methods are working!

Zoom in…

Check out: http://www.esnips.com/doc/868644b5-3d2d-46f7-8497-90255b80e3d7

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