PH709 Extrasolar Planets Professor Michael Smith 1 EXOPLANETS: Prof Michael SMITH ph709-08-part1.doc ph709-08-part2.doc ph709-08-part3.doc http://astro.kent.ac.uk/mds/Modules/modules.htm TOPICS COVERED IN COURSE Intro 1. Measurement and Theory: Dynamics, Binaries 2. Exoplanets 3. Detection Techniques Measurement Derived Physical Information 4. Summary of detection 5. Populations, Distributions, Metallicity, Eccentricity 6. Star and Planet Formation The accretion disk to the debris disc Formation models Evolution: Migration/eccentricity Review of the Latest Status We are still in the early days of a revolution in the field of planetary sciences that was triggered by the discovery of planets around other stars. Candidate exoplanets now number 312, with masses as small as 5–7 ME http://exoplanet.eu/catalog.php . Comparative planetology, which once included only our solar system's planets and moons, now includes sub-Neptune to super-Jupiter-mass planets in other solar systems. PH709 Extrasolar Planets Professor Michael Smith 2 SUPER-EARTHS Thanks to remarkable progress, radial velocity surveys are now able to detect terrestrial planets at habitable distance from low-mass stars. The unexpected diversity of exoplanets includes a growing number of superEarth planets, i.e., exoplanets with masses smaller than 10 Earth masses. Unlike the larger exoplanets previously found, these smaller planets are more likely to have similar chemical and mineralogical composition to the Earth. In April 2007, a team of 11 European scientists announced the discovery of a planet outside our solar system that is potentially habitable, with Earth-like temperatures. The planet was discovered by the European Southern Observatory's telescope in La Silla, Chile, which has a special instrument that splits light to find wobbles in different wave lengths (HARPS). Those wobbles can reveal the existence of other worlds. What they revealed is a planet circling the red dwarf star, Gliese 581. The discovery of the new planet, named Gliese 581c, is sure to fuel studies of planets circling similar dim stars. About 80 percent of the stars near Earth are red dwarfs. The new planet is about five times heavier than Earth, classifying it as a super-earth. Its discoverers aren't certain if it is rocky, like Earth, or if it is a frozen ice ball with liquid water on the surface. If it is rocky like Earth, which is what the prevailing theory proposes, it has a diameter about 1 1/2 times bigger than our planet. If it is an iceball, it would be even bigger. Gliese 581: M star: 3480K, mass: 0.31 solar masses; Luminosity; 0.013 solar Hot Neptune Gl 581b 15.7 ME 0.041 AU Super-earth Gl 581c 5.06ME 0.073 AU Super-earth Gl 581d 8.3 ME 0.25 AU Gl 581c: 20C (albedo = 0.5 assumed) Greenhouse? Tidal locking? However, further research on the potential effects of the planetary atmosphere casts doubt upon the (extremophile life form) habitability of Gliese 581 c and indicates that the third planet in the system, Gliese 581 d, is a better candidate for habitability. !!! An extremophile is an organism that thrives in and may even require physically or geochemically extreme conditions that are detrimental to the majority of life on Earth. Most known extremophiles are microbes. PH709 Extrasolar Planets Professor Michael Smith 3 Currently, Gliese 581d, the third planet of the red dwarf star Gliese 581 (approximately 6.12 parsecs from Earth), appears to be the best example yet discovered of a possible terrestrial exoplanet which orbits close to the habitable zone of space surrounding its star. Going by strict terms, it appears to reside outside the "Goldilocks Zone", but the greenhouse effect may raise the planet's surface temperature to that which would support liquid water. HZ – Habitable Zone: life zone", "Comfort Zone", "Green Belt" or "Goldilocks Zone" (because it's neither too hot nor too cold, but "just right") Sources and sinks of atmospheric carbon dioxide. The photosynthesissustaining habitable zone (pHZ) is determined by the limits of biological productivity on the planetary surface. Although Gliese 581 d orbits outside the theoretical habitable zone of its star, scientists surmise that conditions on the planet may be conducive to supporting life. Scientists originally believed that Gliese 581 d would be too cold for liquid water to exist, and therefore could not support life in forms as existing on Earth. However, since Earth's temperature would be about -19°C without any greenhouse gases, and due to a theorized greenhouse effect of Gliese 581 d, research now suggests that atmospheric conditions on the planet could create temperatures at which liquid water can exist, and therefore the planet may be capable of supporting life. PH709 Extrasolar Planets Professor Michael Smith 4 Planet “c” receives 30% more energy from its star than Venus from the Sun, with an increased radiative forcing caused by the spectral energy distribution of Gl 581. This planet is thus unlikely to host liquid water, although its habitability cannot be positively ruled out by theoretical models due to uncertainties affecting cloud properties and cloud cover. Highly reflective clouds covering at least 75% of the day side of the planet could indeed prevent the water reservoir from being entirely vaporized. Irradiation conditions of planet “d” are comparable to those of early Mars, which is known to have hosted surface liquid water. Thanks to the greenhouse effect of CO2-ice clouds, also invoked to explain the early Martian climate, planet “d” might be a better candidate for the first exoplanet known to be potentially habitable. TRANSITS Currently the most important class of exoplanets are those that transit the disk of their parent stars, allowing for a determination of planetary radii. The 14 confirmed transiting planets observed to date are all more massive than Saturn, have orbital periods of only a few days, and orbit stars bright enough such that radial velocities can be determined, allowing for a calculation of planetary masses and bulk densities (see Charbonneau et al. 2007a). A planetary mass and radius allows us a window into planetary composition (Guillot 2005). The 51 transiting planets are mainly gas giants although one planet, HD 149026b, appears to be 2/3 heavy elements by mass (Sato et al. 2005; Fortney et al. 2006; Ikoma et al. 2006). Understanding how the transiting planet massradius relations change as a function of orbital distance, stellar mass, stellar metallicity, or UV flux, will provide insight into the fundamentals of planetary formation, migration, and evolution. The transit method of planet detection is biased toward finding planets that orbit relatively close to their parent stars. This means that radial velocity follow-up will be possible for some planets as the stellar "wobble" signal is larger for shorter period orbits. However, for transiting planets that are low mass, or that orbit very distant stars, stellar radial velocity measurements may not be possible. For planets at larger orbital distances, radial velocity observations may take years. Therefore, for the foreseeable future a measurement of planetary radii will be our only window into the structure of these planets. Orbital distances may give some clues as to a likely composition, but our experience over the past decade with Pegasi planets (or "hot Jupiters") has shown us the danger of assuming certain types of planets cannot exist at unexpected orbital distances. PH709 Extrasolar Planets Professor Michael Smith 5 UPCOMING SPACE MISSIONS The French/European COROT mission, launched in 2006 December, and the American Kepler mission, set to launch in 2009 Nmarch 4 will revolutionize the study of exoplanets. COROT will monitor 12,000 stars in each of five different fields, each for 150 continuous days (Bordé et al. 2003). COROT detected its first extrasolar planet, COROT-Exo-1b, in May 2007. Planets as small as RE could be detectable around solar-type stars (Moutou et al 2006). The mission lifetime is expected to be at least 2.5 yr. The Kepler mission (Transit Method) will continuously monitor one patch of sky in the Cygnus region, monitoring over 100,000 main-sequence stars (Basri et al. 2005). The expected mission lifetime is 3-5 years. Detection of sub-Earth size planets is the mission's goal, with detection of planets with radii as small at 1 Mercury radius is possible around M stars. With these missions, perhaps hundreds of planets will be discovered with masses ranging from sub-Mercury to many times that of Jupiter. Of course, while planets close to their parent stars will preferentially be found, due to their shorter orbital periods and greater likelihood to transit, planetary transits will be detected at all orbital separations. In general, the detection of three successive transits will be necessary for a confirmed detection, which will limit confirmed planetary-radius objects to about 1.5 AU. INTERFEROMETRY (mid-IR ? ) There are several potential advantages to the use of interferometry for direct detection of extrasolar planetary emission. Destructive interference can be used to strongly suppress emission from the much brighter primary star. High angular resolution, which can be significantly better that the diffraction limit of the individual telescopes, will help to separate the emission from an extrasolar planet and its primary star as well as from sources of background emission. http://exoplanet.eu/ http://en.wikipedia.org/wiki/Extrasolar_planet Book: Chapter 23 of Carroll & Ostlie, Modern Astronomy, second edition Rapidly developing subject - first extrasolar planet around an ordinary star only discovered in 1995 by Mayor & Queloz. PH709 Extrasolar Planets Professor Michael Smith 6 Resources. For observations, a good starting point is Berkeley extrasolar planets search homepage http://exoplanets.org/ Number: There are 228 confirmed planets listed. Of the 312 candidates — there are 31 multiple planet systems, 178 in single planet systems, 5 orbiting pulsars. 3 free floating?, plenty of candidates, retractions, cluster planets,…… Detection method: 293 planets have been detected by radial velocity or doppler method, 51 by transit method, 8 by microlensing, 6 by direct imaging, and 5 by timing method. Mass: The planets are listed with indications of their approximate masses as multiples of Jupiter 's mass (MJ = 1.898 × 1027 kg) or multiples of Earth's mass (ME = 5.9737 × 1024 kg). Neptune = 17.1 ME, Mercury = 0.0553 ME. Orbit/Distance: approximate distances in astronomical units (1) AU = 1.496 108 km, distance between Earth and Sun) from their parent stars. Names: According to astronomical naming conventions, the official designation for a body orbiting a star is the star's catalogue number followed by a letter. The star itself is designated with the letter 'a', and orbiting bodies by 'b', 'c', etc Fusing stars There are currently (2007) 238 planets known in orbit around fusing stars. There are currently 178 known planets in single-planet systems and 60 known planets in 20 multiple-planet systems (14 with two planets, 4 with three and 2 with four). "Single" here means that only one planet has been detected to date. Detection methods are not sensitive to low-mass planets, these stars may have smaller planets that are below the limits of detectability, or are so far from the star that they have not yet been observed over an orbital period. Could ALL stars harbour planets? Pulsars There are currently four known planets orbiting two different pulsars. The planet of PSR B1620−26 is in a circumbinary orbit around a pulsar and a white dwarf star. PH709 Extrasolar Planets Professor Michael Smith 7 Brown dwarfs There is currently one known planet orbiting a brown dwarf. Free floating planets There is currently one suspected free-floating planet, i.e. it doesn't appear to orbit a star. PH709 Extrasolar Planets Professor Michael Smith 8 PH709 Extrasolar Planets Professor Michael Smith 9 PH709 Extrasolar Planets Professor Michael Smith 10 PH709 Extrasolar Planets Professor Michael Smith 11 IN 2008 ……..(wikipedia) 2008, OGLE-2006-BLG-109Lb and OGLE-2006-BLG-109Lc On February 14 the discovery of the, until now, most similar Jupiter-Saturn planetary system constellation was announced, with the ratios of mass, distance to their star and orbiting time PH709 Extrasolar Planets Professor Michael Smith 12 similar to that of Jupiter-Saturn. This can be important for possible life in a solar system as Jupiter and Saturn have a stabilizing effect to the habitable zone by sweeping away large asteroids from the habitable zone.[50] 2008, HD 189733 b On March 20 follow up studies to the first spectral analyses of an extrasolar planet were published in the scientific journal Nature, announcing evidence of an organic molecule found on an extrasolar planet for the first time. In 2007 water vapor was already detected in the spectrum of HD 189733 b, but new analyses showed not only water vapor, but also methane existing in the atmosphere of the giant gas planet. Although conditions on HD 189733 b are too harsh to harbor life, it still is the first time a key molecule for organic life was found on an extrasolar planet.[51] 2008, HD 40307 On June 16, Michel Mayor announced a confirmed planetary system with three super-Earths orbiting this K-type star. Their masses are between 4 to 9 Earth masses and with periods between 4 to 20 days. It is speculated that this may be the first multi-planetary system without any known gas giants. All three terrestrial planets were discovered by the HARPS spectrograph in La Silla, Chile. The discoveries represented a significant increase in the numbers of known super-earths. Based on this, astronomers now suggest that such low-mass planets may outnumber the Jupiter-like planets by 3 to 1.