DOCSLIB.ORG

Glossary (PDF)

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Glossary (PDF) Section Name –LIZZIE WADE on May 4, 2013 E L Y P M I T A/ S A www.sciencemag.org N ) M TO T BO ( ; A N O Z ARI F O Y T I ERS Downloaded from V I UN / L P J A/ S A N ; L P J / A AS N Gas giants more than 50 times the mass A planet with about two to 10 times the ; W of Earth orbiting too close to their stars to A planet that is less massive than Neptune mass of Earth. Can be hard to distinguish E CR 7 1 be habitable. Make up 42% of confi rmed but shares its characteristic thick atmo- from a mini-Neptune. Example: Kepler-62 O L L planets. Example: 51 Pegasi b. sphere of hydrogen and helium. Current e and f. O detection techniques can have trouble AP A/ telling them from super-Earths. Example: AS N ) Similar to a hot Jupiter in mass and prox- Kepler-11 b-f. A planet about the mass of Earth, but not nec- HT G I imity to a star, but much less dense and essarily within its star’s habitable zone. Exam- R O T T thus larger. Synonym: Infl ated hot Jupiter. ple: Planet orbiting Alpha Centauri Bb. F E L Example: HAT-P-1. S O T HO P A rocky planet with one to 10 times the mass C HI Planets between 10 and 50 Earth masses of Earth, orbiting in the habitable zone of its AP R G ( orbiting close to their stars. Example: star. Possible example: expected any time. : S T Gliese 436 b. Synonyms: Twin Earth, Goldilocks planet, DI E R Earth 2.0, Earth analog, Earth-like planet. C 570 3 MAY 2013 VOL 340 SCIENCE www.sciencemag.org Published by AAAS A planet that does not orbit a star. Astron- omers don’t know whether these wander- ing planets were ejected from star systems or formed by themselves in interstellar space. Rogue planets can be up to 13 times the mass of Jupiter; more-massive bod- ies are classifi ed as brown dwarfs. Without stars to keep them warm, they are always frigid. Synonyms: orphan planet, homeless planet, nomad planet, free-fl oating planet, sub-brown dwarf. Example: CFBDSIR 2149-0403. An exoplanet orbiting a pulsar, a spinning neutron star left behind after a supernova; probably debris from the explosion, trapped by the neutron star’s strong gravity. Only a handful are known. Not habitable. Examples: on May 4, 2013 CL PSR 1257+12 b, c, and d, the fi rst exoplanets ever TS R S discovered back in 1992. O F O S E A/ ÇAD CAL . L / A AS N ; A/ M S www.sciencemag.org U E ; TI L R P J O S A super-Earth covered in water — A/ N S A CO A planet that orbits a binary star in the form of ice, oceans, or a N A; VVV D system and thus has two suns water-vapor atmosphere, depend- / O ÇA T L I instead of one. Examples: ing on the planet’s proximity to the A A S C . L R Kepler-16 b, Tatooine. star. Example: Gliese 1214b. / E/ O RM ES ; O Downloaded from CS I EL S D Y . P H P A/ D TRO ÇA AS AL R A moon orbiting an exoplanet. Some exomoons of C . O L F / gas giants may have molten interiors thanks to tidal With orbits the shape of stretched- R O E S T E N heating, which could keep them warm even outside out ellipses, these planets can C; S CE S / their stars’ habitable zones and make them easy to swoop through drastically different T AN I UR N spot from afar. But so far, no exomoons have been temperature zones in the course of O H . S R H observed. Possible example: Fomalhaut b. a year. Example: HD 80606 b. T H/ I C M E -S T D AL AR -C V L P J HAR A/ / AS AR Sometimes called a failed star, a brown dwarf L N I : ) U T G forms when a cloud of gas collapses but is not The rocky core left behind after F A E L D. P / massive enough to ignite the fusion reactions the gas of a hot Jupiter evaporates O A S T E that fuel fully formed stars. Brown dwarfs can as a result of orbiting so close M A/ O R AS be 13 to 75 times the mass of Jupiter. Less to its star. Synonym: chthonian F N E S I massive bodies are rogue planets; more mas- planet, evaporated remnant core. CH; W E K T C L sive ones can sustain fusion and are thus stars. Example: COROT-7b (suspected); O -CA CL L ( Some brown dwarfs have their own planets. HD 209458 b is in the process P S J T A/ DI Example: 2M1207. of evaporating. E AS R C N www.sciencemag.org SCIENCE VOL 340 3 MAY 2013 571 Published by AAAS.
Load more

Recommended publications
  • Giant Planets
    Lyot Conference 5 June 2007 Properties of Exoplanets: from Giants toward Rocky Planets & Informing Coronagraphy Collaborators: Paul Butler, Debra Fischer, Steve Vogt Chris McCarthy, Jason Wright, John Johnson, Katie Peek Chris Tinney, Hugh Jones, Brad Carter Greg Laughlin, Doug Lin, Shigeru Ida, Jack Lissauer, Eugenio Rivera -Stellar Sample - 1330 Nearby FGKM Stars (~2000 stars total with Mayor et al. ) Star Selection Criteria: HipparcosH-R Cat. Diagram d < 100 pc . 1330 Target Stars •Vmag < 10 mag • No Close Binaries • Age > 2 Gyr Lum 1.3 Msun Target List: 0.3 M Published SUN 1 Michel Mayor & Didier Queloz First ExoPlanet 51 Peg Now Stephane Udry plays leadership role also. Doppler Monitering Begun: 1987 Uniform Doppler Precision: 1-3 m s-1 2000 FGKM M.S. Stars Three Telescopes 8 Years 7 Years 19 Years (3.5 AU) (3 AU) (6 AU) Keck Lick Anglo-Aus. Tel. 2 Precision: 1.5 m s-1 3 Years Planets or Brown Dwarfs in Unclosed, Long-Period Orbits: Targets for Coronagraphs 3 Sep ~ 0.3 “ Sep ~ 0.2 “ 4 Sep ~ 0.2” Examples of Jupiter-mass & Saturn mass Planets Detected by RV 5 Jupiter Mass Extrasolar Planets P = 5.3 yr e = 0.47 Jupiter Mass Extrasolar Planets P = 1.3 yr 6 Sub-Saturn Masses: 30 - 100 MEarth Msini = 32 MEarth Msini = 37 MEarth Msini = 57 MEarth Old Doppler Precision: 3 m/s Sub-Saturn Masses: Detectable for P < 2 Month Multiple - Planet Systems 7 HD 12661: Sun-like Star ) (meters/sec Velocity Time (years) 2 - Planet Model 2.5 M J Weak Interactions 1.9 MJ K0V, 1Gy, 16 pc HD 128311 2:1 Resonance Inner Outer Per (d) 458 918 Msini 2.3 3.1 ecc 0.23 0.22 ω 119 212 Pc / Pb = 2.004 Dynamical Resonance (Laughlin) 8 Msini = 1.4 MJ M Dwarfs have distant giant planets.
    [Show full text]
  • EPSC2018-126, 2018 European Planetary Science Congress 2018 Eeuropeapn Planetarsy Science Ccongress C Author(S) 2018
    EPSC Abstracts Vol. 12, EPSC2018-126, 2018 European Planetary Science Congress 2018 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2018 Stellar wind interaction with the expanding atmosphere of Gliese 436b A.G. Berezutskiy (1), I.F. Shaikhislamov (1), M.L. Khodachenko (2,3) and I.B. Miroshnichenko (1,4) (1) Institute of Laser Physics, Siberian Brunch Russian Academy of Science, Novosibirsk, Russia; (2) Space Research Institute, Austrian Academy of Science, Graz, Austria; (3) Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, Russia (4) Novosibirsk State Technical University, Novosibirsk, Russia ([email protected]) Abstract the escaping planetary upper atmospheric material are also taken into account. We study an exosphere of a Neptune-size exoplanet Gliese 436b, orbiting the red dwarf at an extremely 3. Results close distance (0.028 au), taking into account its interaction with the stellar wind plasma flow. It was At the initial state of the simulations, the atmosphere shown that Gliese 436 b has a bowshock region of Gliese 436b is assumed to consist of the molecular between planetary and stellar wind which localized hydrogen and helium atoms at a ratio NHe / NH2 = 1/5 on the distance of ~33 Rp, where density of planetary with the temperature 750 K. We consider the case of -3 atoms slightly dominates over the protons. a weak stellar wind (SW) with nsw=100 cm , Tsw=1 МК, Vsw=70 km/s, which is much less intense than 1. Introduction the solar wind. Because of this fact, , we did not consider generation of Energetic Neutral Atoms The modelled planet Gliese 436b has a mass (ENAs).
    [Show full text]
  • Estudio Numérico De La Dinámica De Planetas
    UNIVERSIDAD PEDAGOGICA´ NACIONAL FACULTAD DE CIENCIA Y TECNOLOG´IA ESTUDIO NUMERICO´ DE LA DINAMICA´ DE PLANETAS EXTRASOLARES Tesis presentada por Eduardo Antonio Mafla Mejia dirigida por: Camilo Delgado Correal Nestor Mendez Hincapie para obtener el grado de Licenciado en F´ısica 2015 Departamento de F´ısica I Dedico este trabajo a mi mam´a, quien me apoyo en mi deseo de seguir el camino de la educaci´on. Sin su apoyo este deseo no lograr´ıa ser hoy una realidad. RESUMEN ANALÍTICO EN EDUCACIÓN - RAE 1. Información General Tipo de documento Trabajo de Grado Acceso al documento Universidad Pedagógica Nacional. Biblioteca Central ESTUDIO NUMÉRICO DE LA DINÁMICA DE PLANETAS Título del documento EXTRASOLARES Autor(es) Mafla Mejia, Eduardo Antonio Director Méndez Hincapié, Néstor; Delgado Correal, Camilo Publicación Bogotá. Universidad Pedagógica Nacional, 2015. 61 p. Unidad Patrocinante Universidad Pedagógica Nacional DINÁMICA DE EXOPLANETAS, LEY GRAVITACIONAL DE NEWTON, Palabras Claves ESTUDIO NUMÉRICO. 2. Descripción Trabajo de grado que se propone evidenciar si el modelo matemático clásico newtoniano, y en consecuencia las tres leyes de Kepler, se puede generalizar a cualquier sistema planetario, o solo es válido para determinados casos particulares. Para lograr esto de comparar numéricamente los efectos de las diferentes correcciones que puede adoptar la ley de gravitación de Newton para modelar la dinámica de planetas extrasolares aplicándolos en los sistemas extrasolares Gliese 876 d, Gliese 436 b y el sistema Mercurio – Sol. En los exoplanetas examinados se encontró, que en un buen grado de aproximación, la dinámica de los exoplanetas se logran describir con el modelo newtoniano, y en consecuencia, modelar su movimiento usando las leyes de Kepler.
    [Show full text]
  • How to Detect Exoplanets Exoplanets: an Exoplanet Or Extrasolar Planet Is a Planet Outside the Solar System
    Exoplanets Matthew Sparks, Sobya Shaikh, Joseph Bayley, Nafiseh Essmaeilzadeh How to detect exoplanets Exoplanets: An exoplanet or extrasolar planet is a planet outside the Solar System. Transit Method: When a planet crosses in front of its star as viewed by an observer, the event is called a transit. Transits by terrestrial planets produce a small change in a star's brightness of about 1/10,000 (100 parts per million, ppm), lasting for 2 to 16 hours. This change must be absolutely periodic if it is caused by a planet. In addition, all transits produced by the same planet must be of the same change in brightness and last the same amount of time, thus providing a highly repeatable signal and robust detection method. Astrometry: Astrometry is the area of study that focuses on precise measurements of the positions and movements of stars and other celestial bodies, as well as explaining these movements. In this method, the gravitational pull of a planet causes a star to change its orbit over time. Careful analysis of the changes in a star's orbit can provide an indication that there exists a massive exoplanet in orbit around the star. The astrometry technique has benefits over other exoplanet search techniques because it can locate planets that orbit far out from the star Radial Velocity method: The radial velocity method to detect exoplanet is based on the detection of variations in the velocity of the central star, due to the changing direction of the gravitational pull from an (unseen) exoplanet as it orbits the star.
    [Show full text]
  • AST413 Gezegen Sistemleri Ve Oluşumu Ders 1 : Tarihçe Ve Temel Yasalar Kozmogoni
    AST413 Gezegen Sistemleri ve Oluşumu Ders 1 : Tarihçe ve Temel Yasalar Kozmogoni Milton'ın Evreni Evren nedir, nasıl bir yerdir ve biz nasıl oluştuk? → DinlerveFelsefe! Dinler ve Felsefe! Stonehenge M.Ö. 3000-2000 @ Wiltshire, İngiltere Kozmoloji Evren nasıl oluştu ve nasıl çalışıyor? → DinlerveFelsefe! Nedenselleştirme ve Bilim! Yer Merkezli Evren Modeli: Merkezinde hareketsiz Yer'in bulunduğu, hepsi Yer'e aynı uzaklıktaki yıldızların üstünde bulunduğu bir küre! 1. Yer'in küresel olduğu, 2. Yer'in büyüklüğü, 3. Tutulmalar bu modelle açıklanabilmiştir. Ancak, 1. Hızı diğer cisimlerden farklı olanlar? 2. Sabit hızla hareket etmeyenler? 3. Geri yönlü (retrograd) hareket yapanlar? “The School of Athens”, Raphael, 1509-1511 Dış Çemberlerle Retrograd Hareketi Açıklama Çabası Appolonius, dış çember kullanarak geri yönlü (retrograd) hareketi, Yer'i merkezden alıp, dış çemberin merkezinin hareketini diğer odağa göre sabit yaparak sabit hızla gerçekleşmeyen hareketi de başarıyla açıklamış oldu. Ama teorisi hala gezegen gözlemlerinde ulaşılan bazı gözlemsel sonuçları açıklayamıyordu. Batlamyus (Ptolemy) (90 – 168) bu problemi iki dış çember kullanarak gidermeye çalıştı. Perge'li Appolonius (MÖ 262 - 190) Güneş Merkezli Evren Modeli Böylece Mars ve Güneş'in konumlarını daha hassas ve çok daha basit bir modelle açıklamak mümkün oldu! Nicolas Copernicus (1473 - 1543) Tycho Brahé (1546 - 1601) Melez Yer-Güneş Merkezli Evren Modeli Tycho gelmiş geçmiş en iyi gözlemcilerden biri (belki de birincisi olduğu halde) Dünya'nın Güneş çevresinde dolanması durumunda yıldızların paralaktik hareket göstermesini beklediği halde bunu gözleyemediği için melez bir modele yöneldi. Eksik olan onun gözlemleri değil, paralaktik hareketi ölçecek teknolojiye (teleskop!) henüz ulaşılamamış olmasıydı... YÖRÜNGE DÖNEMİ – KAVUŞUM DÖNEMİ Kavuşum Dönemi (S): Gök cisminin aynı konfigürasyonda arka arkaya iki dizilişi arasındaki süre.
    [Show full text]
  • The Universe Contents 3 HD 149026 B
    History . 64 Antarctica . 136 Utopia Planitia . 209 Umbriel . 286 Comets . 338 In Popular Culture . 66 Great Barrier Reef . 138 Vastitas Borealis . 210 Oberon . 287 Borrelly . 340 The Amazon Rainforest . 140 Titania . 288 C/1861 G1 Thatcher . 341 Universe Mercury . 68 Ngorongoro Conservation Jupiter . 212 Shepherd Moons . 289 Churyamov- Orientation . 72 Area . 142 Orientation . 216 Gerasimenko . 342 Contents Magnetosphere . 73 Great Wall of China . 144 Atmosphere . .217 Neptune . 290 Hale-Bopp . 343 History . 74 History . 218 Orientation . 294 y Halle . 344 BepiColombo Mission . 76 The Moon . 146 Great Red Spot . 222 Magnetosphere . 295 Hartley 2 . 345 In Popular Culture . 77 Orientation . 150 Ring System . 224 History . 296 ONIS . 346 Caloris Planitia . 79 History . 152 Surface . 225 In Popular Culture . 299 ’Oumuamua . 347 In Popular Culture . 156 Shoemaker-Levy 9 . 348 Foreword . 6 Pantheon Fossae . 80 Clouds . 226 Surface/Atmosphere 301 Raditladi Basin . 81 Apollo 11 . 158 Oceans . 227 s Ring . 302 Swift-Tuttle . 349 Orbital Gateway . 160 Tempel 1 . 350 Introduction to the Rachmaninoff Crater . 82 Magnetosphere . 228 Proteus . 303 Universe . 8 Caloris Montes . 83 Lunar Eclipses . .161 Juno Mission . 230 Triton . 304 Tempel-Tuttle . 351 Scale of the Universe . 10 Sea of Tranquility . 163 Io . 232 Nereid . 306 Wild 2 . 352 Modern Observing Venus . 84 South Pole-Aitken Europa . 234 Other Moons . 308 Crater . 164 Methods . .12 Orientation . 88 Ganymede . 236 Oort Cloud . 353 Copernicus Crater . 165 Today’s Telescopes . 14. Atmosphere . 90 Callisto . 238 Non-Planetary Solar System Montes Apenninus . 166 How to Use This Book 16 History . 91 Objects . 310 Exoplanets . 354 Oceanus Procellarum .167 Naming Conventions . 18 In Popular Culture .
    [Show full text]
  • The Echo Design Reference Mission
    ESA UNCLASSIFIED – For Official Use estec European Space Research and Technology Centre Keplerlaan 1 2201 AZ Noordwijk The Netherlands Tel. (31) 71 5656565 Fax (31) 71 5656040 www.esa.int The EChO Design Reference Mission Prepared by The EChO Study Science Team Reference ECHO-SRE-SA-PHASEA-010 Issue 2 Revision 0 Date of Issue 18th December, 2013 Status Document Type Distribution ESA UNCLASSIFIED – For Official Use ESA UNCLASSIFIED – For Official Use Title The EChO Design Reference Mission Issue 2 Revision 0 Author EChO Study Science Team Date 18th December, 2013 Approved by Date Reason for change Issue Revision Date Edits to section 6.1 to clarify language 1 1 2/10/2013 Edits for discussion 1 2 (not issued) Edits for clarity, references and section 5.3 added 1 3 3/10/2013 Additional details on exoplanet radii 1 4 15/10/2013 Explicit planet parameters given 1 5 21/10/20013 Editing and updating 1 6 4/12/2013 Update, including comments from the PRR 1 7 10/12/2013 Further update of text describing modelling tools 2 0 16/12/2013 Issue 1.0 Revision 4+5+6+7 Reason for change Date Pages Paragraph(s) General update of text 10/12/2013 All Update of figures/appendix to reflect targets known as 18/12/2013 of December 2013 (tables 2 and 3 remain as of Sept 2013) Page 2/24 ESA Standard Document Date 18th December 2013 Issue 2 Rev 0 ESA UNCLASSIFIED – For Official Use ESA UNCLASSIFIED – For Official Use Table of contents: 1 Executive Summary ...........................................................................................................................
    [Show full text]
  • STUDY of EXTRA SOLAR EXOPLANET SYSTEMS by METHOD of the GEO-SPACE UNIVERSAL X – STRUCTURE A. G. Syromyatnikov1 Saint-Petersbur
    British Journal of Earth Sciences Research Vol.4, No.2, pp.16-21, April 2015 ___Published by European Centre for Research Training and Development UK (www.eajournals.org) STUDY OF EXTRA SOLAR EXOPLANET SYSTEMS BY METHOD OF THE GEO-SPACE UNIVERSAL X – STRUCTURE A. G. Syromyatnikov1 Saint-Petersburg State University, department of Physics, Ulyanovskaya ul. d. 1, 198504, Saint Petersburg, Petrodvoretz, Russia ABSTRACT: For some exoplanets within 50 light-years (15 pc) of the Earth by a method of the Geo-space universal X – structu re it is studied questions of the definition of the exoplanets parameters: density – diameter etc. I give also the Universal Geo – space X – structure theoretical Levels of the similarity of natural satellites of Solar system planets. From the theory in particularly follows the mystery similarity between the Mercury and the Earth’s Moon. KEYWORDS: Geo-Space, Universal, X-Structure, INTRODUCTION There is a Galactic Winter on the Earth at present [1]. It's pretty quiet time when nobody when no major geological events does not occur except in the local area as it was 10,000 years ago with the isthmus connecting Asia with America (Bering Strait), in the formation of the Straits separating New Zealand, off the East coast of North America, etc. But sometimes comets fall into Jupiter. The attention of researchers of an outer space has attracted discovering exoplanets outside the Solar system [2]. For centuries philosophers and scientists supposed that extrasolar planets existed, but there was no way of detecting them or of knowing their frequency or how similar they might be to the planets of the Solar system.
    [Show full text]
  • Extrasolar Planets Dimitar D
    Vol 451|3 January 2008 Q&A ESA/C. CARREAU ESA/C. ASTRONOMY Extrasolar planets Dimitar D. Sasselov Hundreds of planets are known to orbit stars other than the Sun, and unprecedented observations of their atmospheres and structures are being made. It’s an invaluable opening for understanding the planets’ diverse natures, the formation of our Solar System, and the possibility of habitable planets beyond our home. 2 How many planets outside our Solar for at least one complete orbit of the planet. A will dim the star’s light by a fraction (Rp/Rs) , System have we found so far? wobble can also be detected directly by care- where Rp and Rs are the respective radii of the The number is going up week by week, but at fully observing the position of the star with planet and star. For a planet the size of Jupiter the moment there are about 270 confirmed respect to other stars (a technique known as and a star the size of the Sun, this dimming extrasolar planets — exoplanets, as they’re astrometry), but this is technically even more effect would be roughly 1%, which is easily known in the jargon. Not bad, considering the demanding. detectable even with amateur equipment. The first one was discovered just 13 years ago, and catch is that a transit requires the planet’s orbit they’re not that easy to spot. What other ways are there of finding to be almost exactly edge-on as we look at the exoplanets, besides the Doppler effect? star, which is extremely unlikely.
    [Show full text]
  • The Stellar Disintegration Zone
    The Stellar Disintegration Zone Jeffrey J. Wolynski September 29, 2018 Rockledge, FL 32955 Abstract: The stellar disintegration zone is the area that separates hot Jupiters from their more evolved and evolving counterparts. It shows that hot Jupiters lose their thick helium/hydrogen atmospheres faster if they orbit close to a much hotter host star, which is predicted by the General Theory of Stellar Metamorphosis. The SDZ on this graph is between 5-9 Earth Radii, with a period shorter than 10 days. As well, the SDZ's can be different for different stars, this graph is only a generalization. Data is taken from various telescopes including the Kepler, and 2,504 evolving/dead stars are on the graph. The periods of the dead/evolving stars on the graph do not include the ones beyond 50 days, and objects beyond a radius of 23 Earths. Data for the points on the graph is included, as well as the objects' names. What this graph shows us in the orange box is that there really is a gap in stellar evolution. This is due to atmospheric escape as a hot Jupiter (already very evolved star) does not have a large enough gravitational field to hold on to its helium and hydrogen. We should expect this gap to become more pronounced as the data comes in from the Transiting Exoplanet Survey Satellite (TESS). It is suggested for astronomers to realize that not all stars pass through this gap, the only purpose of this paper is to show quite clearly that Hot Jupiters in fact do lose their mass due to physical changes (changing orbits/adoption per the adoption principle of stellar metamorphosis) that were not predicted by Big Bang or the Nebular Hypothesis.
    [Show full text]
  • Report from the Exoplanet Task Force
    THE UNIVERSITY OF ARIZONA ® TUCSON ARIZONA Department of Planetary Sciences Tucson, Arizona 85721-0092 Lunar and Planetary Laboratory Tel: (520) 621-2789 1629 E. University Blvd. Fax: (520) 626-8250 May 18, 2008 Dr. Garth D. Illingworth Chair, Astronomy and Astrophysics Advisory Committee Department of Astronomy and Astrophysics University of California, Santa Cruz Dear Garth, I am pleased to transmit to you the report of the Exoplanet Task Force. The report is a comprehensive study of the search for and study of planets around other stars (exoplanets). The young but maturing field of exoplanets is perhaps one of the most compelling fields of study in science today—both because of the discoveries made to date on giant planets around other stars, and because the detection of planets just like our Earth (“Earth analogs”) is at last within reach technologically. In the Report we outline the need for a vigorous research program in exoplanets to understand our place in the cosmos: whether planets like our home Earth are a common or rare outcome of cosmic evolution. The strategy we developed is intended to address the following fundamental questions, in priority order, within three distinct 5-yr long phases, over a 15 year period: 1. What are the physical characteristics of planets in the habitable zones around bright, nearby stars? 2. What is the architecture of planetary systems? 3. When, how and in what environments are planets formed? The Report recommends a two-pronged strategy for the detection and characterization of planets the size of the Earth. For stars much less massive and cooler than our Sun (M-dwarfs), existing ground-based techniques including radial velocity and transit searches, and space-based facilities both existing and under development such as Spitzer and JWST, are adequate for finding and studying planets close to the mass and size of the Earth.
    [Show full text]
  • Planet Cards
    Space Mission Part 4 Grade 6 – Space Planet Cards 55 Cancri e Gliese 436 b Size: twice the size of Earth Size: 4 times the size of Earth Mass: 8 times the mass of Earth Mass: 22 times the mass of Earth Temperature: 1700 C Temperature: 440 C Liquid water: no Liquid water: ice Type of planet: rocky Type of planet: rocky Length of year: 18 hours! Length of year: 2 days Other Notes: Other Notes: Due to the high This planet could largely be made of surface pressure water could be in carbon, which could be in the form the form of ice there despite the high of a HUGE diamond in its core due temperature. This ice could “burn” to the high pressure. into vapour due to radiation. Sciencenorth.ca/schools Science North is an agency of the Government of Ontario 1 Kepler 62 f HD 209458 b Size: 1.4 times the size of the Earth Size: A bit larger than Jupiter Mass: Maybe 3 times the Earth’s Mass: Almost as massive as Jupiter mass Temperature: 1100 C Temperature: -30 C or greater Liquid water: no Liquid water: possible Type of planet: gas giant Type of planet: rocky Length of year: 3 days Length of year: 267 days Other Notes: Other Notes: An example of a “hot Jupiter”. A Seems too cold, but depending on huge planet that orbits very closely the atmosphere the greenhouse to its star. effect could make this planet habitable. Kepler 296 e Kepler 20 e Size: 1.75 times the size of Earth Size: 87% the size of Earth Mass: unknown, likely larger than Mass: 40% of Earth Earth Temperature: 1000 C Temperature: -6 C or higher Liquid water: no! Liquid lava! Liquid water: possible Type of planet: rocky Type of planet: rocky Length of year: 6 days Length of year: 34 days Other Notes: Other Notes: The same side always faces the Sun, so A bit larger than Earth but very similar.
    [Show full text]