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The Doppler Method, or the Radial Velocity Detection of Planets: II. Results Telescope Instrument Wavelength Reference 1-m MJUO Hercules Th-Ar / Iodine cell 1.2-m Euler Telescope CORALIE Th-Ar 1.8-m BOAO BOES Iodine Cell 1.88-m Okayama Obs, HIDES Iodine Cell 1.88-m OHP SOPHIE Th-Ar 2-m TLS Coude Echelle Iodine Cell 2.2m ESO/MPI La Silla FEROS Th-Ar 2.7m McDonald Obs. 2dcoude Iodine cell 3-m Lick Observatory Hamilton Echelle Iodine cell 3.8-m TNG SARG Iodine Cell 3.9-m AAT UCLES Iodine cell 3.6-m ESO La Silla HARPS Th-Ar 8.2-m Subaru Telescope HDS Iodine Cell 8.2-m VLT UVES Iodine cell 9-m Hobby-Eberly HRS Iodine cell 10-m Keck HiRes Iodine cell Campbell & Walker: The Pioneers of RV Planet Searches 1988: 1980-1992 searched for planets around 26 solar-type stars. Even though they found evidence for planets, they were not 100% convinced. If they had looked at 100 stars they certainly would have found convincing evidence for exoplanets. Campbell, Walker, & Yang 1988 „Probable third body variation of 25 m s–1, 2.7 year period, superposed on a large velocity gradient“ The first (?) extrasolar planet around a normal star: HD 114762 with M sin i = 11 MJ discovered by Latham et al. (1989) Filled circles are data taken at McDonald Observatory using the telluric lines at 6300 Ang. The mass was uncomfortably high (remember sin i effect) to regard it unambiguously as an extrasolar planet The Search For Extrasolar Planets At McDonald Observatory Bill Cochran & Artie Hatzes Hobby-Eberly 9 m Telescope Harlan J. Smith Phillip MacQueen, Paul Robertson, 2001 - present 2.7 m Telescope Erik Brugamyer, Diane Paulson, Robert 1988 - present Robert Wittenmyer, Stuart Barnes Michael Endl 51 Pegasi b: the 1st extrasolar planet: P = 4.3 days!!! a = 0.05 AU !!! M sin i = 0.45 M Jupiter Michel Mayor & Didier Queloz 1995 A HOT JUPITER 1997: The first 2.7 m Survey Planet: P = 2.2 yrs a = 1.67 AU M ~ 1.7 M Jupiter More Planets / Brown Dwarfs (co-)discovered with the 2.7 m Telescope: Eps Eri b: Gam Cep: HD 137510 b: HD 13189 b: Beta Gem b: HD 91699 b: And then the discoveries started rolling in: “New Planet Seen Outside Solar System” New York Times April 19, 1996 “10 More Planets Discovered” Washington Post August 6, 2000 “First new solar system discovered” USA TODAY April 16, 1999 Global Properties of Exoplanets: Mass Distribution The Brown Dwarf Desert Planet: M < 13 MJup → no nuclear burning Brown Dwarf: 13 MJup < M < ~80 MJup → only deuterium burning Star: M > ~80 MJup → Hydrogen burning Up-to-date Histograms with all ~ 500 exoplanets: One argument: Because of unknown sin i these are just low mass stars seen with i near 0 i decreasing probability decreasing Semi-Major Axis Distribution Number Semi-major Axis (AU) The lack of long period planets is a selection effect since these take a long time to detect The short period planets are also a selection effect: they are the easiest to find and now transiting surveys are geared to finding these. Updated: Eccentricity distribution Fall off at high eccentricity may be partially due to an observing bias… e=0.4 e=0.6 e=0.8 ω=0 ω=90 ω=180 …high eccentricity orbits are hard to detect! For very eccentric orbits the value of the eccentricity is is often defined by one data point. If you miss the peak you can get the wrong mass! At opposition with Earth would be 1/5 diameter of full moon, 12x brighter than Venus ε Eri 2 ´´ Comparison of some eccentric orbit planets to our solar system Mass versusEccentricities Orbital Distance There is a relative lack of massive close-in planets Classes of planets: 51 Peg Planets: Jupiter mass planets in short period orbits Discovered by Mayor & Queloz 1995 Classes of planets: 51 Peg Planets • ~35% of known extrasolar planets are 51 Peg planets (selection effect) • 0.5–1% of solar type stars have giant planets in short period orbits • 5–10% of solar type stars have a giant planet (longer periods) Somehow these giant planets ended up very close to the star! => orbital migration Classes of planets: Hot Neptunes Santos et al. 2004 Butler et al. 2004 M sin i = 14-20 MEarth If there are „hot Jupiters“ and „hot Neptunes“ it makes sense that there are „hot Superearths“ CoRoT-7b Mass = 7.4 ME P = 0.85 d Classes: The Massive Eccentrics • Masses between 7–20 MJupiter • Eccentricities, e > 0.3 • Prototype: HD 114762 discovered in 1989! m sini = 11 MJup Classes: The Massive Eccentrics There are no massive planets in circular orbits Planet-Planet Interactions Initially you have two giant planets in circular orbits These interact gravitationally. One is ejected and the remaining planet is in an eccentric orbit Lin & Ida, 1997, Astrophysical Journal, 477, 781L Red: Planets with masses < 4 MJup Blue: Planets with masses > 4 MJup Planets in Binary Systems Why should we care about binary stars? • Most stars are found in binary systems • Does binary star formation prevent planet formation? • Do planets in binaries have different characteristics? • For what range of binary periods are planets found? • What conditions make it conducive to form planets? (Nurture versus Nature?) • Are there circumbinary planets? Some Planets in known Binary Systems: Star a (AU) 16 Cyg B 800 55 CnC 540 HD 46375 300 τ Boo 155 υ And 1540 HD 222582 4740 HD 195019 3300 There are very few planets in close binaries. One exception is the γ Cep system. The first extra-solar Planet may have been found by Walker et al. in 1992 in a binary system: Ca II is a measure of stellar activity (spots) γ Cephei Binary Period 56.8 ± 5 Years Msini ~ 0,4 ± 0,1 MSun e 0,42 ± 0,04 a 18.5 AU K 1,98 ± 0,08 km/s Planet Period 2,47 Years Msini 1,76 MJupiter e 0,2 a 2,13 AU K 26,2 m/s γ Cephei Primary star (A) Secondary Star (B) Planet (b) The planet around γ Cep is difficult to form and on the borderline of being impossible. Standard planet formation theory: Giant planets form beyond the snowline where the solid core can form. Once the core is formed the protoplanet accretes gas. It then migrates inwards. In binary systems the companion truncates the disk. In the case of γ Cep this disk is truncated just at the ice line. No ice line, no solid core, no giant planet to migrate inward. γ Cep can just be formed, a giant planet in a shorter period orbit would be problems for planet formation theory. The interesting Case of 16 Cyg B These stars are identical and are „solar twins“. 16 Cyg B has a giant planet with 1.7 MJup in a 800 d period, but star A shows no evidence for any planet. Why? Planetary Systems: ~50 Multiple Systems Extrasolar Planetary Systems (18 shown) Star P (d) MJsini a (AU) e HD 82943 221 0.9 0.7 0.54 Star P (d) MJsini a (AU) e 444 1.6 1.2 0.41 HD 74156 51.6 1.5 0.3 0.65 GL 876 30 0.6 0.1 0.27 2300 7.5 3.5 0.40 61 2.0 0.2 0.10 HD 169830 229 2.9 0.8 0.31 47 UMa 1095 2.4 2.1 0.06 2102 4.0 3.6 0.33 2594 0.8 3.7 0.00 HD 160691 9.5 0.04 0.09 0 HD 37124 153 0.9 0.5 0.20 637 1.7 1.5 0.31 550 1.0 2.5 0.40 2986 3.1 0.09 0.80 55 CnC 2.8 0.04 0.04 0.17 HD 12661 263 2.3 0.8 0.35 14.6 0.8 0.1 0.0 1444 1.6 2.6 0.20 44.3 0.2 0.2 0.34 HD 168443 58 7.6 0.3 0.53 260 0.14 0.78 0.2 5300 4.3 6.0 0.16 1770 17.0 2.9 0.20 HD 38529 14.31 0.8 0.1 0.28 Ups And 4.6 0.7 0.06 0.01 2207 12.8 3.7 0.33 241.2 2.1 0.8 0.28 1266 4.6 2.5 0.27 HD 190360 17.1 0.06 0.13 0.01 2891 1.5 3.92 0.36 HD 108874 395.4 1.36 1.05 0.07 HD 202206 255.9 17.4 0.83 0.44 1605.8 1.02 2.68 0.25 1383.4 2.4 2.55 0.27 HD 128311 448.6 2.18 1.1 0.25 HD 11964 37.8 0.11 0.23 0.15 919 3.21 1.76 0.17 1940 0.7 3.17 0.3 HD 217107 7.1 1.37 0.07 0.13 3150 2.1 4.3 0.55 The 5-planet System around 55 CnC 0.17MJ 5.77 M J • 0.82M J 0.03M •0.11 MJ • J Red lines: solar system plane orbits The Planetary System around GJ 581 (M dwarf!) 16 ME 7.2 ME 5.5 ME Inner planet M sin i = 1.9 MEarth Resonant Systems Systems Star P (d) MJsini a (AU) e HD 82943 221 0.9 0.7 0.54 → 2:1 444 1.6 1.2 0.41 GL 876 30 0.6 0.1 0.27 → 2:1 61 2.0 0.2 0.10 55 Cnc 14.6 0.8 0.1 0.0 → 3:1 44.3 0.2 0.2 0.34 HD 108874 395.4 1.36 1.05 0.07 → 4:1 1605.8 1.02 2.68 0.25 HD 128311 448.6 2.18 1.1 0.25 → 2:1 919 3.21 1.76 0.17 2:1 → Inner planet makes two orbits for every one of the outer planet Eccentricities • Period (days) Red points: Systems Blue points: single planets Mass versus Orbital Distance Eccentricities Red points: Systems Blue points: single planets On average, giant planets in planetary sytems tend to be lighter than single planets.
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  • Search for Brown-Dwarf Companions of Stars⋆⋆⋆

    Search for Brown-Dwarf Companions of Stars⋆⋆⋆

    A&A 525, A95 (2011) Astronomy DOI: 10.1051/0004-6361/201015427 & c ESO 2010 Astrophysics Search for brown-dwarf companions of stars, J. Sahlmann1,2, D. Ségransan1,D.Queloz1,S.Udry1,N.C.Santos3,4, M. Marmier1,M.Mayor1, D. Naef1,F.Pepe1, and S. Zucker5 1 Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland e-mail: [email protected] 2 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany 3 Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 4 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Portugal 5 Department of Geophysics and Planetary Sciences, Tel Aviv University, Tel Aviv 69978, Israel Received 19 July 2010 / Accepted 23 September 2010 ABSTRACT Context. The frequency of brown-dwarf companions in close orbit around Sun-like stars is low compared to the frequency of plane- tary and stellar companions. There is presently no comprehensive explanation of this lack of brown-dwarf companions. Aims. By combining the orbital solutions obtained from stellar radial-velocity curves and Hipparcos astrometric measurements, we attempt to determine the orbit inclinations and therefore the masses of the orbiting companions. By determining the masses of poten- tial brown-dwarf companions, we improve our knowledge of the companion mass-function. Methods. The radial-velocity solutions revealing potential brown-dwarf companions are obtained for stars from the CORALIE and HARPS planet-search surveys or from the literature. The best Keplerian fit to our radial-velocity measurements is found using the Levenberg-Marquardt method.