The first—51 Pegasi b (Bellerophon ) Extra Solar Planets 51 Pegasi B The star How do we know this The planet Star51 Pegasi ConstellationPegasus Distance50.9 ± 0.3 ly (15.61 ± 0.09 pc) Spectral typeG2.5IVa or G45Va 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 Semimajor axis (a) 0.0527 ± 0.0030 AU (7.89 Gm) Periastron (q) 0.0520 AU (7.79 Gm) Apastron (Q) 0.0534 AU (7.99 Gm) Eccentricity (e) 0.013 ± 0.012 Orbital period (P) Radial velocity of Star It move toward and away from us with period of 4.2 days. 4.230785 ± 0.000036 d (101.5388 h) Argument of periastron (ω) 58° Time of periastron (T0) 2,450,001.51 ± 0.61 JD Semi-amplitude (K) 55.94 ± 0.69 m/s Physical characteristics Minimum mass (m sin i) 0.472 ± 0.039 MJ (150 M ) How do we know that? In practice…its done with spectra Doppler Effect! Change in wavelength depends on speed! 1 Problem: not all systems are edge on! We don’t always know the tilt! Thus the mass measured is a minimum mass Then there is a bit more physics: I. rp + rstar = d Here mp = 0, we can can know exact mass. M starVstar = m planet v planet p2 = ( (conservation of momentum) 4π 2 +m star planet ) )d 3 p = orbital period d = semi - major axis G = constant of universal gravitation II . Here I = 90..can’t determine mp p2 = ( In General, mass listed is really: M sin i G(M 4π 2 +m star planet ) )d 3 p = orbital period d = semi - major axis p2 = ( G = constant of universal gravitation p2 = ( M star p 2G 4π 2 so you only need M star , Vstar , and p! d =3 G( M 4π 2 )d 3 +m ) star planet p = orbital period d = semi - major axis G = constant of universal gravitation Astronomers know star masses from their spectra and lots of work from predecessors over the years! planet ) )d 3 IV. vstar = 2πrplanet 2πrstar , v planet = p p Limits of Radial velocity measurements Then a bit of algebra….and 2 M star p 2πG 4π 2 +m star G = constant of universal gravitation III. m p + M star ≈ M star the result , is : G( M p = orbital period d = semi - major axis where i is inclination of orbit m p = Vstar 3 G( M 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 ? Vstar and p are obtained from the radial velocity graph! Hot Jupiters! Why search around sun like stars? Here are the first nine planets discovered (as of 1997) 2 A more complete list (2000) A Growth Industry? So where are we going? 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! Note 20 multiple planet systems! • Use Transit Photometry for edge on systems (finds smaller planets?) • Lets see how these methods are working! Astrometry Transit Photmetry 3 Provides lots of info! Not as easy as it looks! Transit of Mercury in 2006 Transit of Venus in 2004 Zoom in… Check out: http://www.esnips.com/doc/868644b5-3d2d-46f7-849790255b80e3d7 4
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