DOCSLIB.ORG

Exoplanet Trading Cards FOLD FOLD

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Exoplanet Trading Cards FOLD FOLD FOLD How to play 2QHSHUVRQUHDGVWKH³'LG<RX.QRZ"´ DQG³7\SHVRI([RSODQHWV´FDUGVWRthe group. Each person gets a game card. Group members review the information on their cards. The game begins when one player reads aloud the information on their card and asks their game question. The player holding the card with the answer to that question responds, shares the information on their card, and reads aloud their own game learning.org - of Exoplanet question. - The game continues until all cards have Trading Cards been shared aloud with the group. www.universe Exoplanet Trading Cards FOLD FOLD Did you Did you know? know? Scientists are searching for planets similar to Earth and signs of life. A key ingredient for life is liquid water, like Exoplanets are planets outside of our oceans or lakes. solar system that usually orbit another star. They are also known as extrasolar The habitable zone is the area around a planets. star where it is not too hot and not too cold for surrounding planets to have We know of thousands of exoplanets in liquid water. the Milky Way galaxy. Scientists have found water molecules Exoplanets are detected and studied by in the atmospheres of some exoplanets. telescopes on the ground and in space. %XWWKH\KDYHQ¶WIRXQGOLTXLGZDWHU\HW Exoplanets range from rocky (like Earth So far, Earth is the only planet we know and Mars) to gas-rich (like Jupiter and of with life. learning.org Saturn). - of We GRQ¶WKDYHSLFWXUHVRIPDQ\ - Proxima Centauri is the closest star to exoplanets because they are small and our own. It hosts the nearest faint. It is difficult to capture their exoplanets. images with current technology. www.universe Exoplanet Trading Cards FOLD FOLD Types of Exoplanets Rocky Worlds Rocky worlds, also called terrestrial, are mainly composed of rocks, heavier elements, or metals. They have a solid surface and are between 1/2 to two Exoplanets come in a variety of types and WLPHV(DUWK¶VUDGLXVLQVL]H sizes. Gas Giants They range from gas giants larger than Gas giants are similar to Jupiter but Jupiter, to small, rocky worlds about as big much ODUJHU7KH\GRQ¶Whave hard around as Earth or Mars. surfaces. Instead, they have swirling gases (hydrogen and/or helium) around They can be hot enough to boil metal or a solid core. locked in a deep freeze. Neptune-like Worlds Some exoplanets orbit multiple stars. Neptune-like worlds are a subset of gas Others are free-IORDWLQJDQGGRQ¶WRUELWD giants that are similar in size to Neptune star at all. or Uranus. Like gas giants, they have hydrogen and helium atmospheres and While there are many types of exoplanets, cores made of rock and metals. learning.org four types are featured in this card deck« - of Super Earths - Super Earths are larger than Earth and smaller than Neptune. They are not necessarily similar to our home planet. They can be made of gas, rock, or a combination of both. www.universe Exoplanet Trading Cards FOLD FOLD Beta Pictoris b A gas giant discovered in 2008. It is one of two known planets in its system. Approx. star temperature: 7,780 °C Distance from star: 9.10 Orbital period: 21 Earth years Habitable zone: No Earth diameter learning.org Game Question - of - What exoplanet has a year that is 20 Earth days long? www.universe g Ceti Beta Pictoris b Tau Answer: ,PDJH$UWLVW¶Vconcept Exoplanet Trading Cards FOLD FOLD HD 10647 b A gas giant discovered in 2006. It is the only known planet in its system at this time. Approx. star temperature: 5,760 °C Distance from star: 2.02 Orbital period: 2.7 Earth years Habitable zone: Yes Earth diameter learning.org Game Question - of - What rocky world has a year that is 18.8 Earth days long? www.universe 1 h 1 - HD 10647 b TRAPPIST Answer: ,PDJH$UWLVW¶Vconcept Exoplanet Trading Cards FOLD FOLD HD 40307 c A Neptune-like world discovered in 2009. It is one of five known planets in its system. Approx. star temperature: 4,700 °C Distance from star: 0.08 Orbital period: 9.6 Earth days Habitable zone: No Earth diameter learning.org Game Question - of - What gas giant was discovered in 2006? www.universe HD 40307 c b 10647 HD Answer: ,PDJH$UWLVW¶Vconcept Exoplanet Trading Cards FOLD FOLD KELT-6 b A gas giant discovered in 2014. It is one of two known planets in its system, the other being KELT-6 c. Approx. star temperature: 6,000 °C Distance from star: 0.08 Orbital period: 7.8 Earth days Habitable zone: No Earth diameter learning.org Game Question - of - What exoplanet is 0.3 away from its star? www.universe 1229 b 1229 - KELT-6 b Kepler Answer: ,PDJH$UWLVW¶Vconcept Exoplanet Trading Cards FOLD FOLD KELT-6 c A gas giant discovered in 2015. It is one of two known planets in its system, the other being KELT-6 b. Approx. star temperature: 6,000 °C Distance from star: 2.39 Orbital period: 3.5 Earth years Habitable zone: Yes Earth diameter learning.org Game Question - of - What exoplanet has a year that is 3.5 Earth days long? www.universe 20 b 20 - KELT-6 c KELT Answer: ,PDJH$UWLVW¶VFRQFHSW Exoplanet Trading Cards FOLD FOLD KELT-19 A b A gas giant discovered in 2017. It is the only known planet in its system at this time. Approx. star temperature: 7,230 °C Distance from star: 0.06 Orbital period: 4.6 Earth days Habitable zone: No Earth diameter learning.org Game Question - of - What exoplanet has an orbital period of 1.7 Earth years? www.universe f Ceti Tau KELT-19 A b Answer: ,PDJH$UWLVW¶Vconcept Exoplanet Trading Cards FOLD FOLD KELT-20 b A gas giant discovered in 2017. It is the only known planet in its system at this time. Approx. star temperature: 8,700 °C Distance from star: 0.05 Orbital period: 3.5 Earth days Habitable zone: No Earth diameter learning.org Game Question - of - What TRAPPIST planet is in the habitable zone? www.universe 1 e 1 - KELT-20 b TRAPPIST Answer: ,PDJH$UWLVW¶Vconcept Exoplanet Trading Cards FOLD FOLD Kepler-62 f A super Earth discovered in 2013. It is one of five known planets in its system. Approx. star temperature: 4,650 °C Distance from star: 0.72 Orbital period: 267.3 Earth days Habitable zone: Yes Earth diameter learning.org Game Question - of - What gas giant was discovered in 2015? www.universe 6 c 6 - Kepler-62 f KELT Answer: ,PDJH$UWLVW¶Vconcept Exoplanet Trading Cards FOLD FOLD Kepler-1229 b A super Earth discovered in 2016. It is the only known planet in its system at this time. Approx. star temperature: 3,450 °C Distance from star: 0.3 Orbital period: 86.8 Earth days Habitable zone: Yes Earth diameter learning.org Game Question - of - What gas giant was discovered in 2008? www.universe b Pictoris Kepler-1229 b Beta Answer: ,PDJH$UWLVW¶Vconcept Exoplanet Trading Cards FOLD FOLD Proxima Centauri b A super Earth discovered in 2016. It is one of two confirmed planets in its system. Approx. star temperature: 2,770 °C Distance from star: 0.05 Orbital period: 11.2 Earth days Habitable zone: Yes Earth diameter learning.org Game Question - of - What Neptune-like world Proxima was discovered in 2009? www.universe Centauri b c 40307 HD Answer: ,PDJH$UWLVW¶Vconcept Exoplanet Trading Cards FOLD FOLD Tau Ceti f A super Earth discovered in 2017. Along with Tau Ceti g, it is one of four confirmed planets in its system. Approx. star temperature: 5,070 °C Distance from star: 1.33 Orbital period: 1.7 Earth years Habitable zone: Yes Earth diameter learning.org Game Question - of - What super Earth is in a five planet system? www.universe 62 f 62 - Tau Ceti f Kepler Answer: ,PDJH$UWLVW¶Vconcept Exoplanet Trading Cards FOLD FOLD Tau Ceti g A super Earth discovered in 2017. Along with Tau Ceti f, it is one of four confirmed planets in its system. Approx. star temperature: 5,070 °C Distance from star: 0.13 Orbital period: 20 Earth days Habitable zone: No Earth diameter learning.org Game Question - of - :KDWH[RSODQHW¶VVWDUKDV a temperature of 2,770 °C? www.universe Centauri b Centauri Proxima Tau Ceti g Answer: ,PDJH$UWLVW¶Vconcept Exoplanet Trading Cards FOLD FOLD TRAPPIST-1 e A rocky world discovered in 2017. It is one of seven known planets in the TRAPPIST-1 system. Approx. star temperature: 2,270 °C Distance from star: 0.03 Orbital period: 6.1 Earth days Habitable zone: Yes Earth diameter learning.org Game Question - of - :KDWH[RSODQHW¶V\HDULV 7.8 Earth days long? www.universe 6 b 6 - TRAPPIST-1 e KELT Answer: ,PDJH$UWLVW¶Vconcept Exoplanet Trading Cards FOLD FOLD TRAPPIST-1 h A rocky world discovered in 2017. It is one of seven known planets in the TRAPPIST-1 system. Approx. star temperature: 2,270 °C Distance from star: 0.06 Orbital period: 18.8 Earth days Habitable zone: No Earth diameter learning.org Game Question - of - :KDWH[RSODQHW¶VVWDUKDVD temperature of 7,230 °C? www.universe 19 A b A 19 - TRAPPIST-1 h KELT Answer: ,PDJH$UWLVW¶Vconcept Exoplanet Trading Cards FOLD FOLD GJ 179 b A gas giant discovered in 2009. It is the only known planet in its system at this time. Approx. star temperature: 3,150 °C Distance from star: 0.05 Orbital period: 6.3 Earth years Earth diameter Habitable zone: No learning.org - of - Bonus Card GJ 179 b www.universe ,PDJH$UWLVW¶Vconcept Exoplanet Trading Cards FOLD FOLD HD 40307 b A super Earth discovered in 2009.
Load more

Recommended publications
  • RADIAL VELOCITIES in the ZODIACAL DUST CLOUD
    A SURVEY OF RADIAL VELOCITIES in the ZODIACAL DUST CLOUD Brian Harold May Astrophysics Group Department of Physics Imperial College London Thesis submitted for the Degree of Doctor of Philosophy to Imperial College of Science, Technology and Medicine London · 2007 · 2 Abstract This thesis documents the building of a pressure-scanned Fabry-Perot Spectrometer, equipped with a photomultiplier and pulse-counting electronics, and its deployment at the Observatorio del Teide at Izaña in Tenerife, at an altitude of 7,700 feet (2567 m), for the purpose of recording high-resolution spectra of the Zodiacal Light. The aim was to achieve the first systematic mapping of the MgI absorption line in the Night Sky, as a function of position in heliocentric coordinates, covering especially the plane of the ecliptic, for a wide variety of elongations from the Sun. More than 250 scans of both morning and evening Zodiacal Light were obtained, in two observing periods – September-October 1971, and April 1972. The scans, as expected, showed profiles modified by components variously Doppler-shifted with respect to the unshifted shape seen in daylight. Unexpectedly, MgI emission was also discovered. These observations covered for the first time a span of elongations from 25º East, through 180º (the Gegenschein), to 27º West, and recorded average shifts of up to six tenths of an angstrom, corresponding to a maximum radial velocity relative to the Earth of about 40 km/s. The set of spectra obtained is in this thesis compared with predictions made from a number of different models of a dust cloud, assuming various distributions of dust density as a function of position and particle size, and differing assumptions about their speed and direction.
    [Show full text]
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • Cosmological Aspects of Planetary Habitability
    Cosmological aspects of planetary habitability Yu. A. Shchekinov Department of Space Physics, SFU, Rostov on Don, Russia [email protected] M. Safonova, J. Murthy Indian Institute of Astrophysics, Bangalore, India [email protected], [email protected] ABSTRACT The habitable zone (HZ) is defined as the region around a star where a planet can support liquid water on its surface, which, together with an oxygen atmo- sphere, is presumed to be necessary (and sufficient) to develop and sustain life on the planet. Currently, about twenty potentially habitable planets are listed. The most intriguing question driving all these studies is whether planets within habitable zones host extraterrestrial life. It is implicitly assumed that a planet in the habitable zone bears biota. How- ever along with the two usual indicators of habitability, an oxygen atmosphere and liquid water on the surface, an additional one – the age — has to be taken into account when the question of the existence of life (or even a simple biota) on a planet is addressed. The importance of planetary age for the existence of life as we know it follows from the fact that the primary process, the photosynthesis, is endothermic with an activation energy higher than temperatures in habitable zones. Therefore on planets in habitable zones, due to variations in their albedo, orbits, diameters and other crucial parameters, the onset of photosynthesis may arXiv:1404.0641v1 [astro-ph.EP] 2 Apr 2014 take much longer time than the planetary age. Recently, several exoplanets orbiting Population II stars with ages of 12–13 Gyr were discovered.
    [Show full text]
  • Geodynamics and Rate of Volcanism on Massive Earth-Like Planets
    The Astrophysical Journal, 700:1732–1749, 2009 August 1 doi:10.1088/0004-637X/700/2/1732 C 2009. The American Astronomical Society. All rights reserved. Printed in the U.S.A. GEODYNAMICS AND RATE OF VOLCANISM ON MASSIVE EARTH-LIKE PLANETS E. S. Kite1,3, M. Manga1,3, and E. Gaidos2 1 Department of Earth and Planetary Science, University of California at Berkeley, Berkeley, CA 94720, USA; [email protected] 2 Department of Geology and Geophysics, University of Hawaii at Manoa, Honolulu, HI 96822, USA Received 2008 September 12; accepted 2009 May 29; published 2009 July 16 ABSTRACT We provide estimates of volcanism versus time for planets with Earth-like composition and masses 0.25–25 M⊕, as a step toward predicting atmospheric mass on extrasolar rocky planets. Volcanism requires melting of the silicate mantle. We use a thermal evolution model, calibrated against Earth, in combination with standard melting models, to explore the dependence of convection-driven decompression mantle melting on planet mass. We show that (1) volcanism is likely to proceed on massive planets with plate tectonics over the main-sequence lifetime of the parent star; (2) crustal thickness (and melting rate normalized to planet mass) is weakly dependent on planet mass; (3) stagnant lid planets live fast (they have higher rates of melting than their plate tectonic counterparts early in their thermal evolution), but die young (melting shuts down after a few Gyr); (4) plate tectonics may not operate on high-mass planets because of the production of buoyant crust which is difficult to subduct; and (5) melting is necessary but insufficient for efficient volcanic degassing—volatiles partition into the earliest, deepest melts, which may be denser than the residue and sink to the base of the mantle on young, massive planets.
    [Show full text]
  • Correlations Between the Stellar, Planetary, and Debris Components of Exoplanet Systems Observed by Herschel⋆
    A&A 565, A15 (2014) Astronomy DOI: 10.1051/0004-6361/201323058 & c ESO 2014 Astrophysics Correlations between the stellar, planetary, and debris components of exoplanet systems observed by Herschel J. P. Marshall1,2, A. Moro-Martín3,4, C. Eiroa1, G. Kennedy5,A.Mora6, B. Sibthorpe7, J.-F. Lestrade8, J. Maldonado1,9, J. Sanz-Forcada10,M.C.Wyatt5,B.Matthews11,12,J.Horner2,13,14, B. Montesinos10,G.Bryden15, C. del Burgo16,J.S.Greaves17,R.J.Ivison18,19, G. Meeus1, G. Olofsson20, G. L. Pilbratt21, and G. J. White22,23 (Affiliations can be found after the references) Received 15 November 2013 / Accepted 6 March 2014 ABSTRACT Context. Stars form surrounded by gas- and dust-rich protoplanetary discs. Generally, these discs dissipate over a few (3–10) Myr, leaving a faint tenuous debris disc composed of second-generation dust produced by the attrition of larger bodies formed in the protoplanetary disc. Giant planets detected in radial velocity and transit surveys of main-sequence stars also form within the protoplanetary disc, whilst super-Earths now detectable may form once the gas has dissipated. Our own solar system, with its eight planets and two debris belts, is a prime example of an end state of this process. Aims. The Herschel DEBRIS, DUNES, and GT programmes observed 37 exoplanet host stars within 25 pc at 70, 100, and 160 μm with the sensitiv- ity to detect far-infrared excess emission at flux density levels only an order of magnitude greater than that of the solar system’s Edgeworth-Kuiper belt. Here we present an analysis of that sample, using it to more accurately determine the (possible) level of dust emission from these exoplanet host stars and thereafter determine the links between the various components of these exoplanetary systems through statistical analysis.
    [Show full text]
  • 1 Director's Message
    1 Director’s Message Markus Kissler-Patig 3 Weighing the Black Hole in M101 ULX-1 Stephen Justham and Jifeng Liu 8 World’s Most Powerful Planet Finder Turns its Eye to the Sky: First Light with the Gemini Planet Imager Bruce Macintosh and Peter Michaud 12 Science Highlights Nancy A. Levenson 15 Operations Corner: Update and 2013 Review Andy Adamson 20 Instrumentation Development: Update and 2013 Review Scot Kleinman ON THE COVER: GeminiFocus January 2014 The cover of this issue GeminiFocus is a quarterly publication of Gemini Observatory features first light images from the Gemini 670 N. A‘ohoku Place, Hilo, Hawai‘i 96720 USA Planet Imager that Phone: (808) 974-2500 Fax: (808) 974-2589 were released at the Online viewing address: January 2014 meeting www.gemini.edu/geminifocus of the American Managing Editor: Peter Michaud Astronomical Society Science Editor: Nancy A. Levenson held in Washington, D.C. Associate Editor: Stephen James O’Meara See the press release Designer: Eve Furchgott / Blue Heron Multimedia that accompanied the images starting on Any opinions, findings, and conclusions or recommendations page 8 of this issue. expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation. Markus Kissler-Patig Director’s Message 2013: A Successful Year for Gemini! As 2013 comes to an end, we can look back at 12 very successful months for Gemini despite strong budget constraints. Indeed, 2013 was the first stage of our three-year transition to a reduced opera- tions budget, and it was marked by a roughly 20 percent cut in contributions from Gemini’s partner countries.
    [Show full text]
  • Disks in Nearby Planetary Systems with JWST and ALMA
    Disks in Nearby Planetary Systems with JWST and ALMA Meredith A. MacGregor NSF Postdoctoral Fellow Carnegie Department of Terrestrial Magnetism 233rd AAS Meeting ExoPAG 19 January 6, 2019 MacGregor Circumstellar Disk Evolution molecular cloud 0 Myr main sequence star + planets (?) + debris disk (?) Star Formation > 10 Myr pre-main sequence star + protoplanetary disk Planet Formation 1-10 Myr MacGregor Debris Disks: Observables First extrasolar debris disk detected as “excess” infrared emission by IRAS (Aumann et al. 1984) SPHERE/VLT Herschel ALMA VLA Boccaletti et al (2015), Matthews et al. (2015), MacGregor et al. (2013), MacGregor et al. (2016a) Now, resolved at wavelengthsfrom from Herschel optical DUNES (scattered light) to millimeter and radio (thermal emission) MacGregor Planet-Disk Interactions Planets orbiting a star can gravitationally perturb an outer debris disk Expect to see a variety of structures: warps, clumps, eccentricities, central offsets, sharp edges, etc. Goal: Probe for wide separation planets using debris disk structure HD 15115 β Pictoris Kuiper Belt Asymmetry Warp Resonance Kalas et al. (2007) Lagrange et al. (2010) Jewitt et al. (2009) MacGregor Debris Disks Before ALMA Epsilon Eridani HD 95086 Tau Ceti Beta PictorisHR 4796A HD 107146 AU Mic Greaves+ (2014) Su+ (2015) Lawler+ (2014) Vandenbussche+ (2010) Koerner+ (1998) Hughes+ (2011) Matthews+ (2015) 49 Ceti HD 181327 HD 21997 Fomalhaut HD 10647 (q1 Eri) Eta Corvi HR 8799 Roberge+ (2013) Lebreton+ (2012) Moor+ (2015) Acke+ (2012) Liseau+ (2010) Lebreton+ (2016)
    [Show full text]
  • The HARPS Search for Earth-Like Planets in the Habitable Zone I
    A&A 534, A58 (2011) Astronomy DOI: 10.1051/0004-6361/201117055 & c ESO 2011 Astrophysics The HARPS search for Earth-like planets in the habitable zone I. Very low-mass planets around HD 20794, HD 85512, and HD 192310, F. Pepe1,C.Lovis1, D. Ségransan1,W.Benz2, F. Bouchy3,4, X. Dumusque1, M. Mayor1,D.Queloz1, N. C. Santos5,6,andS.Udry1 1 Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Versoix, Switzerland e-mail: [email protected] 2 Physikalisches Institut Universität Bern, Sidlerstrasse 5, 3012 Bern, Switzerland 3 Institut d’Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis Bd Arago, 75014 Paris, France 4 Observatoire de Haute-Provence/CNRS, 04870 St. Michel l’Observatoire, France 5 Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 6 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Portugal Received 8 April 2011 / Accepted 15 August 2011 ABSTRACT Context. In 2009 we started an intense radial-velocity monitoring of a few nearby, slowly-rotating and quiet solar-type stars within the dedicated HARPS-Upgrade GTO program. Aims. The goal of this campaign is to gather very-precise radial-velocity data with high cadence and continuity to detect tiny signatures of very-low-mass stars that are potentially present in the habitable zone of their parent stars. Methods. Ten stars were selected among the most stable stars of the original HARPS high-precision program that are uniformly spread in hour angle, such that three to four of them are observable at any time of the year.
    [Show full text]
  • AMD-Stability and the Classification of Planetary Systems
    A&A 605, A72 (2017) DOI: 10.1051/0004-6361/201630022 Astronomy c ESO 2017 Astrophysics& AMD-stability and the classification of planetary systems? J. Laskar and A. C. Petit ASD/IMCCE, CNRS-UMR 8028, Observatoire de Paris, PSL, UPMC, 77 Avenue Denfert-Rochereau, 75014 Paris, France e-mail: [email protected] Received 7 November 2016 / Accepted 23 January 2017 ABSTRACT We present here in full detail the evolution of the angular momentum deficit (AMD) during collisions as it was described in Laskar (2000, Phys. Rev. Lett., 84, 3240). Since then, the AMD has been revealed to be a key parameter for the understanding of the outcome of planetary formation models. We define here the AMD-stability criterion that can be easily verified on a newly discovered planetary system. We show how AMD-stability can be used to establish a classification of the multiplanet systems in order to exhibit the planetary systems that are long-term stable because they are AMD-stable, and those that are AMD-unstable which then require some additional dynamical studies to conclude on their stability. The AMD-stability classification is applied to the 131 multiplanet systems from The Extrasolar Planet Encyclopaedia database for which the orbital elements are sufficiently well known. Key words. chaos – celestial mechanics – planets and satellites: dynamical evolution and stability – planets and satellites: formation – planets and satellites: general 1. Introduction motion resonances (MMR, Wisdom 1980; Deck et al. 2013; Ramos et al. 2015) could justify the Hill-type criteria, but the The increasing number of planetary systems has made it nec- results on the overlap of the MMR island are valid only for close essary to search for a possible classification of these planetary orbits and for short-term stability.
    [Show full text]
  • The Hd 40307 Planetary System: Super-Earths Or Mini-Neptunes?
    The Astrophysical Journal, 695:1006–1011, 2009 April 20 doi:10.1088/0004-637X/695/2/1006 C 2009. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE HD 40307 PLANETARY SYSTEM: SUPER-EARTHS OR MINI-NEPTUNES? Rory Barnes1, Brian Jackson1, Sean N. Raymond2,4, Andrew A. West3, and Richard Greenberg1 1 Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA 2 Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309, USA 3 Astronomy Department, University of California, 601 Campbell Hall, Berkeley, CA 94720-3411, USA Received 2008 July 9; accepted 2009 January 15; published 2009 April 6 ABSTRACT Three planets with minimum masses less than 10 M⊕ orbit the star HD 40307, suggesting these planets may be rocky. However, with only radial velocity data, it is impossible to determine if these planets are rocky or gaseous. Here we exploit various dynamical features of the system in order to assess the physical properties of the planets. Observations allow for circular orbits, but a numerical integration shows that the eccentricities must be at least 10−4. Also, planets b and c are so close to the star that tidal effects are significant. If planet b has tidal parameters similar to the terrestrial planets in the solar system and a remnant eccentricity larger than 10−3, then, going back in time, the system would have been unstable within the lifetime of the star (which we estimate to be 6.1 ± 1.6 Gyr). Moreover, if the eccentricities are that large and the inner planet is rocky, then its tidal heating may be an order of magnitude greater than extremely volcanic Io, on a per unit surface area basis.
    [Show full text]
  • Cycle 14 Approved Programs
    Cycle 14 Approved Programs as of 04/05/05 Science First Name Last Name Type Phase II ID Institution Country Title Category Physical Processes in Orion's Veil: A High Resolution Nicholas Abel AR 10636 University of Kentucky USA Star Formation UV Absorption Study of the Line of Sight Towards the Trapezium University of Eric Agol GO 10486 USA Cosmology A Cosmic String Lens Candidate Washington University of Eric Agol AR 10637 USA Cool Stars Finding Terrestrial Planets with HST Washington Space Telescope NGC 4449: a Testbed for Starbursts in the Low- and Alessandra Aloisi GO 10585 Science Institute - USA Galaxies High-Redshift Universe ESA Space Telescope The Rosetta Stone without a Distance: Hunting for Alessandra Aloisi GO 10586 Science Institute - USA Galaxies Cepheids in the "Primordial" Galaxy I Zw 18 ESA University of Timing Studies of the X-ray Binary Populations in Scott Anderson GO 10615 USA Hot Stars Washington Globular Clusters The Johns Hopkins A Search for Debris Disks in the Coeval Beta Pictoris David Ardila GO 10487 USA Star Formation University Moving Group University of Colorado Thomas Ayres AR 10638 USA Cool Stars StarCAT at Boulder Studies of Europa's Plasma Interactions and Gilda Ballester AR 10639 University of Arizona USA Solar System Atmosphere with HST/STIS FUV Images Edward Baltz GO 10543 Stanford University USA Galaxies Microlensing in M87 and the Virgo Cluster University of HST Observations of MilliJansky Radio Sources from the Robert Becker AR 10640 USA Galaxies California - Davis VLA FIRST Survey European Southern
    [Show full text]
  • The HARPS Search for Southern Extra-Solar Planets,
    A&A 493, 639–644 (2009) Astronomy DOI: 10.1051/0004-6361:200810451 & c ESO 2009 Astrophysics The HARPS search for southern extra-solar planets, XIII. A planetary system with 3 super-Earths (4.2, 6.9, and 9.2 M⊕) M. Mayor1,S.Udry1,C.Lovis1,F.Pepe1,D.Queloz1,W.Benz2, J.-L. Bertaux3, F. Bouchy4, C. Mordasini2, and D. Segransan1 1 Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland e-mail: [email protected] 2 Physikalisches Institut, Universität Bern, Silderstrasse 5, 3012 Bern, Switzerland 3 Service d’Aéronomie du CNRS/IPSL, Université de Versailles Saint-Quentin, BP 3, 91371 Verrières-le-Buisson, France 4 Institut d’Astrophysique de Paris, CNRS, Université Pierre et Marie Curie, 98bis Bd Arago, 75014 Paris, France Received 23 June 2008 / Accepted 1 August 2008 ABSTRACT We report the detection of a planetary system with three Super-Earths orbiting HD 40307. HD 40307 is a K2 V metal-deficient star at a distance of only 13 parsec, which is part of the HARPS GTO high-precision planet-search programme. The three planets on circular orbits have very low minimum masses of 4.2, 6.9, and 9.2 Earth masses and periods of 4.3, 9.6, and 20.5 days, respectively. The planet with the shortest period is the lowest mass planet detected to-date orbiting a main sequence star. The detection of the correspondingly low amplitudes of the induced radial-velocity variations is secured completely by the 135 high-quality HARPS observations illustrated by the radial-velocity residuals around the 3-Keplerian solution of only 0.85 ms−1.
    [Show full text]