DOCSLIB.ORG

Candidate Kinematic Groups Among Stars with Planets

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Candidate Kinematic Groups Among Stars with Planets Submitted to ApJ May 18, 2001 Candidate Kinematic Groups Among Stars with Planets Jean-Marc Deltorn1 Space Telescope Science Institute, Baltimore, MD 21218 and Paul Kalas2,3 University of California, Berkeley, CA 94720 [email protected] ABSTRACT We use the Hipparcos catalog to search for stars that share the space velocities of 57 stars with planets. We find 27 stars with planets have at least one “kine- matic companion” in a U, V, W box with size 4, 2 and 6 km s−1, respectively. Thirteen stars with planets have space motions that match those of possible kine- matic groups. A Kolmogorov-Smirnov test on the metallicity distribution of F, G, and K stars shows that the stars with planets and their kinematic companions are likely members of the same, higher metallicity population, and separate from a control sample of stars without planets and their companions. Six stars with planets share similar space velocities with the Hyades moving group. Four stars share the space motions of the Pleiades moving group. HD 19994, HD 160691, and HD 186427 match the space velocities of the IC 2391, Centaurus-Crux, and Wolf 630 moving groups, respectively. HD 27442 and HD 92788 have no com- panions in velocity space except for each other, kinematically appearing as sister stars with planets. Future observational and theoretical tests are required to understand the nature of these candidate kinematic groups. Subject headings: planetary systems—Hipparcos—stellar kinematic groups 1Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 2Astronomy Dept., 601 Campbell Hall, University of California, Berkeley, CA 94720 3NSF Center for Adaptive Optics, University of California –2– 1. Introduction One of the most significant findings related to planet formation is that 5% of nearby F, G, and K dwarfs are orbited by extrasolar giant planets (Marcy et al. 2000). Given the 58 known stars with planets (SWPs), we can begin to test how and why the properties of these systems are unique relative to the entire population of nearby stars. Particularly helpful information would be to identify other stars that formed in the same physical environment as each SWP. A study of such a group could reveal the circumstances and physical conditions that are linked to the formation of giant planets. One distinguishing characteristic of stars with planets is that they have significantly higher metallicities than comparable stars of the same spectral type (Butler et al. 2000; Santos et al. 2001). This correlation of extrasolar planets with high metallicity stars could be due to the accretion of rocky material or planets onto the stellar photosphere after the protoplanetary phase (Laughlin 2000; Sandquist et al. 1998). On the other hand, the high metallicities may originate from the time of star formation due to conditions unique to the parental cloud (Santos et al. 2001; Pinsonneault et al. 2001). Objects that are members of the same star forming environment will share similar locations and kinematics when they are young. Their velocity dispersion will initially trace the velocity dispersion of the parental cloud. As the parental cloud disperses in 107-108 years, the velocity dispersion of some members may increase significantly due to interactions with other stars, spiral arms, and massive molecular clouds (Asiain et al. 1999b). Without any significant disruption, the random dispersion in V4 will stretch the group into a tube during its Galactic orbit (Skuljan et al. 1997). The U and W velocities will also evolve from their initial values and eventually oscillate out of phase. However, even though the spatial cohesiveness disappears on timescales of one galactic orbit, some fraction of the initial group will share a similar V velocity component on timescales of several galactic orbits (Skuljan et al. 1999). Numerous stellar kinematic groups (Table 1) have been identified based on the above arguments. Most kinematic group identified so far are relatively young, <1 Gyr associations of stars in the process of being scattered. Older kinematic associations could, in principle, retain enough cohesiveness in velocity space to be classified as stellar kinematic associations even after 1 Gyr (Wielen 1971; Terlevich 1987), as in the case of the HR 1614 kinematic group (Feltzing & Holmberg 2000). The density in (U,V,W) space of such groups shall 4Unless otherwise noted, space velocities are given relative to the Sun with positive U directed toward the galactic center, positive V in the direction of galactic rotation, and positive W in the direction of the north galactic pole. –3– nonetheless decrease with time, impairing the probability of identifying a large fraction of the same initial kinematic association. The present sample of SWPs are chromospherically quiet and generally have estimated ages between 1 and 10 Gyr. The likelihood that sister stars from the time of star formation still share their kinematics is low. Nevertheless, we find that two SWPs, HD 75732 (55 Cnc) and HD 134987, are already listed as possible members of the Hyades Group (Eggen 1985, 1996). These pre-Hipparcos studies relied on proper motion and parallax information only. In the post-Hipparcos era the study of stellar kinematic groups is pushing forward with more precise position, proper motion, and parallax information that when combined with radial velocity data gives improved knowledge of the 3-dimensional spatial kinematics (Chereul et al. 1999; Skuljan et al. 1999; Asiain et al. 1999a). The primary goal of this paper is to identify stars in the Hipparcos catalog that share the U, V, W space motions of SWPs. We will call stars that have matching U, V, W motions “kinematic companions” without implying that this test establishes a real physical connection in a group’s dynamical or chemical history. We present our list of kinematic companions purely as candidate moving groups that should be investigated more thoroughly. In addition to the kinematic test, we will study the metallicity correlation between the SWPs and their companions, and a control group and their companions. 2. Method We cross-correlate the 118,218 stars in the Hipparcos catalog with the 36,145 stars in the Barbier-Brossat & Figon (2000) catalog of stellar radial velocities (hereafter BBF). For the 21,497 stars shared between the two catalogs, we derive the U, V, W velocity components and their standard deviations (Johnson & Soderblom 1987) using the Hipparcos data for positions, proper motions, and parallaxes.5 For the SWPs we use the mean radial velocities and standard deviations that have been determined by the planet search programs. The SWP BD -10 3166 was not detected by Hipparcos and is excluded from our study, leaving a total SWP sample of 57 stars. We define a box with dimensions (∆U, ∆V, ∆W) = (4, 2, 6) km s−1 centered on the average U, V, W values for each SWP. The space velocities of a given co-eval group will evolve out of this box, and in fact the U, V, W distribution resembles a tilted spheroid rather than 5Relative to the Local Standard of Rest, the Sun has U = 10.0 km s−1,V=5.25kms−1, and W = 7.17 km s−1 (Dehnen & Binney 1998). –4– a box (Skuljan et al. 1997). By making the box small we are selecting only a core group of co-moving stars. Thus our results give a lower limit to the number of members in each possible stellar kinematic group. The benefit of this approach is that we are excluding a large number of interlopers. We select the stars that have average U, V, W values within −1 −1 −1 the box. We then reject those that have σU >2kms ,σV >1kms and σW >3kms . We therefore limit the sample to only stars with relatively well-determined space velocities. Even though the average U, V, W values will place stars within the U, V, W box of a given SWP, the standard deviation in the space motions may give a significant probability that the companion lies outside of the box. We treat the uncertainties using a Monte-Carlo draw, assuming a Gaussian distribution for the errors, centered on the average U, V, W values, and with dispersions equal to σU , σV and σW . We produce 1000 random draws for each kinematic companion. A probability of kinematic membership, PKM, is computed by incrementing a counter, Ci, by 1 each time the U, V, W of a companion falls within the kinematic box of the SWP. We then have PKM =Ci / 1000. Finally, we select only those stars that have PKM > 0.75 as the most secure members of a possible kinematic association. 3. Results: Candidate kinematic companions and the metallicity distribution In Table 2 we give our derived velocity information for the SWPs and any Hipparcos stars that are kinematic companions based on the search parameters defined in the previous section. We find that 27 SWPs have at least one kinematic companion, 14 have three or more kinematic companions, and that two pairs of SWPs are kinematic companions with each other. If we compare Table 2 to Table 1 with the goal of finding matches in U, V and W 6, we find that 13 SWPs and their companions appear kinematically associated with known moving groups. Each of these possible matches will be examined on a case-by-case basis below. However, to estimate the probability that the SWP and SWP companion populations are physically linked, we compare their stellar abundances, which are unusually high for the SWP population. We take take only the F, G, and K stars and use only the Schuster & Nissen (1989) method for determining stellar abundances. As a control group, we take the 37 F, G, and K stars without known planets from Santos et al.
Load more

Recommended publications
  • Lurking in the Shadows: Wide-Separation Gas Giants As Tracers of Planet Formation
    Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation Thesis by Marta Levesque Bryan In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy CALIFORNIA INSTITUTE OF TECHNOLOGY Pasadena, California 2018 Defended May 1, 2018 ii © 2018 Marta Levesque Bryan ORCID: [0000-0002-6076-5967] All rights reserved iii ACKNOWLEDGEMENTS First and foremost I would like to thank Heather Knutson, who I had the great privilege of working with as my thesis advisor. Her encouragement, guidance, and perspective helped me navigate many a challenging problem, and my conversations with her were a consistent source of positivity and learning throughout my time at Caltech. I leave graduate school a better scientist and person for having her as a role model. Heather fostered a wonderfully positive and supportive environment for her students, giving us the space to explore and grow - I could not have asked for a better advisor or research experience. I would also like to thank Konstantin Batygin for enthusiastic and illuminating discussions that always left me more excited to explore the result at hand. Thank you as well to Dimitri Mawet for providing both expertise and contagious optimism for some of my latest direct imaging endeavors. Thank you to the rest of my thesis committee, namely Geoff Blake, Evan Kirby, and Chuck Steidel for their support, helpful conversations, and insightful questions. I am grateful to have had the opportunity to collaborate with Brendan Bowler. His talk at Caltech my second year of graduate school introduced me to an unexpected population of massive wide-separation planetary-mass companions, and lead to a long-running collaboration from which several of my thesis projects were born.
    [Show full text]
  • Stability of Planets in Binary Star Systems
    StabilityStability ofof PlanetsPlanets inin BinaryBinary StarStar SystemsSystems Ákos Bazsó in collaboration with: E. Pilat-Lohinger, D. Bancelin, B. Funk ADG Group Outline Exoplanets in multiple star systems Secular perturbation theory Application: tight binary systems Summary + Outlook About NFN sub-project SP8 “Binary Star Systems and Habitability” Stand-alone project “Exoplanets: Architecture, Evolution and Habitability” Basic dynamical types S-type motion (“satellite”) around one star P-type motion (“planetary”) around both stars Image: R. Schwarz Exoplanets in multiple star systems Observations: (Schwarz 2014, Binary Catalogue) ● 55 binary star systems with 81 planets ● 43 S-type + 12 P-type systems ● 10 multiple star systems with 10 planets Example: γ Cep (Hatzes et al. 2003) ● RV measurements since 1981 ● Indication for a “planet” (Campbell et al. 1988) ● Binary period ~57 yrs, planet period ~2.5 yrs Multiplicity of stars ~45% of solar like stars (F6 – K3) with d < 25 pc in multiple star systems (Raghavan et al. 2010) Known exoplanet host stars: single double triple+ source 77% 20% 3% Raghavan et al. (2006) 83% 15% 2% Mugrauer & Neuhäuser (2009) 88% 10% 2% Roell et al. (2012) Exoplanet catalogues The Extrasolar Planets Encyclopaedia http://exoplanet.eu Exoplanet Orbit Database http://exoplanets.org Open Exoplanet Catalogue http://www.openexoplanetcatalogue.com The Planetary Habitability Laboratory http://phl.upr.edu/home NASA Exoplanet Archive http://exoplanetarchive.ipac.caltech.edu Binary Catalogue of Exoplanets http://www.univie.ac.at/adg/schwarz/multiple.html Habitable Zone Gallery http://www.hzgallery.org Binary Catalogue Binary Catalogue of Exoplanets http://www.univie.ac.at/adg/schwarz/multiple.html Dynamical stability Stability limit for S-type planets Rabl & Dvorak (1988), Holman & Wiegert (1999), Pilat-Lohinger & Dvorak (2002) Parameters (a , e , μ) bin bin Outer limit at roughly max.
    [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]
  • Platform-Independent Mobile Robot Communication
    Philipp A. Baer Platform-Independent Development of Robot Communication Software kassel university press This work has been accepted by the faculty of Electrical Engineering and Computer Science of the University of Kassel as a thesis for acquiring the academic degree of Doktor der Ingenieurwissenschaften (Dr.-Ing.). Advisers: Prof. Dr. Kurt Geihs Prof. Dr. Gerhard K. Kraetzschmar Additional Doctoral Committee Members: Prof. Dr. Albert Zündorf Prof. Dr. Klaus David Defense day: 04th December 2008 Bibliographic information published by Deutsche Nationalbibliothek The Deutsche Nationalbibliothek lists this publication in the Deutsche Nationalbibliografie; detailed bibliographic data is available in the Internet at http://dnb.d-nb.de. Zugl.: Kassel, Univ., Diss. 2008 ISBN print: 978-3-89958-644-2 ISBN online: 978-3-89958-645-9 URN: urn:nbn:de:0002-6453 © 2008, kassel university press GmbH, Kassel www.upress.uni-kassel.de Printed by: Unidruckerei, University of Kassel Printed in Germany Für Mutti und Mama. Mutti, du bleibst unvergessen. * 29. September 1923 = 14. Oktober 2008 Contents List of Figuresv List of Tables vii Abstract ix I Introduction1 1 Introduction3 1.1 Motivation.........................................4 1.1.1 Software Structure................................5 1.1.2 Development Methodology...........................5 1.1.3 Communication.................................6 1.1.4 Configuration and Monitoring.........................6 1.2 Problem Analysis.....................................7 1.2.1 Development Methodology...........................7 1.2.2 Communication Infrastructure........................8 1.2.3 Resource Discovery...............................8 1.3 Solution Approach....................................9 1.4 Major Results........................................ 11 1.5 Overview.......................................... 12 2 Foundations 13 2.1 Autonomous Mobile Robots............................... 13 2.1.1 Hardware Architecture............................. 14 2.1.2 Robot Software.................................
    [Show full text]
  • Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs
    Draft version July 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The California Legacy Survey I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal,1 Benjamin J. Fulton,1, 2 Lea A. Hirsch,3 Howard T. Isaacson,4 Andrew W. Howard,1 Cayla M. Dedrick,5, 6 Ilya A. Sherstyuk,1 Sarah C. Blunt,1, 7 Erik A. Petigura,8 Heather A. Knutson,9 Aida Behmard,9, 7 Ashley Chontos,10, 7 Justin R. Crepp,11 Ian J. M. Crossfield,12 Paul A. Dalba,13, 14 Debra A. Fischer,15 Gregory W. Henry,16 Stephen R. Kane,13 Molly Kosiarek,17, 7 Geoffrey W. Marcy,1, 7 Ryan A. Rubenzahl,1, 7 Lauren M. Weiss,10 and Jason T. Wright18, 19, 20 1Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 6Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 7NSF Graduate Research Fellow 8Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 9Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 10Institute for Astronomy, University of Hawai`i,
    [Show full text]
  • Winter Observing Notes
    Wynyard Planetarium & Observatory Winter Observing Notes Wynyard Planetarium & Observatory PUBLIC OBSERVING – Winter Tour of the Sky with the Naked Eye NGC 457 CASSIOPEIA eta Cas Look for Notice how the constellations 5 the ‘W’ swing around Polaris during shape the night Is Dubhe yellowish compared 2 Polaris to Merak? Dubhe 3 Merak URSA MINOR Kochab 1 Is Kochab orange Pherkad compared to Polaris? THE PLOUGH 4 Mizar Alcor Figure 1: Sketch of the northern sky in winter. North 1. On leaving the planetarium, turn around and look northwards over the roof of the building. To your right is a group of stars like the outline of a saucepan standing up on it’s handle. This is the Plough (also called the Big Dipper) and is part of the constellation Ursa Major, the Great Bear. The top two stars are called the Pointers. Check with binoculars. Not all stars are white. The colour shows that Dubhe is cooler than Merak in the same way that red-hot is cooler than white-hot. 2. Use the Pointers to guide you to the left, to the next bright star. This is Polaris, the Pole (or North) Star. Note that it is not the brightest star in the sky, a common misconception. Below and to the right are two prominent but fainter stars. These are Kochab and Pherkad, the Guardians of the Pole. Look carefully and you will notice that Kochab is slightly orange when compared to Polaris. Check with binoculars. © Rob Peeling, CaDAS, 2007 version 2.0 Wynyard Planetarium & Observatory PUBLIC OBSERVING – Winter Polaris, Kochab and Pherkad mark the constellation Ursa Minor, the Little Bear.
    [Show full text]
  • Open Batalha-Dissertation.Pdf
    The Pennsylvania State University The Graduate School Eberly College of Science A SYNERGISTIC APPROACH TO INTERPRETING PLANETARY ATMOSPHERES A Dissertation in Astronomy and Astrophysics by Natasha E. Batalha © 2017 Natasha E. Batalha Submitted in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy August 2017 The dissertation of Natasha E. Batalha was reviewed and approved∗ by the following: Steinn Sigurdsson Professor of Astronomy and Astrophysics Dissertation Co-Advisor, Co-Chair of Committee James Kasting Professor of Geosciences Dissertation Co-Advisor, Co-Chair of Committee Jason Wright Professor of Astronomy and Astrophysics Eric Ford Professor of Astronomy and Astrophysics Chris Forest Professor of Meteorology Avi Mandell NASA Goddard Space Flight Center, Research Scientist Special Signatory Michael Eracleous Professor of Astronomy and Astrophysics Graduate Program Chair ∗Signatures are on file in the Graduate School. ii Abstract We will soon have the technological capability to measure the atmospheric compo- sition of temperate Earth-sized planets orbiting nearby stars. Interpreting these atmospheric signals poses a new challenge to planetary science. In contrast to jovian-like atmospheres, whose bulk compositions consist of hydrogen and helium, terrestrial planet atmospheres are likely comprised of high mean molecular weight secondary atmospheres, which have gone through a high degree of evolution. For example, present-day Mars has a frozen surface with a thin tenuous atmosphere, but 4 billion years ago it may have been warmed by a thick greenhouse atmosphere. Several processes contribute to a planet’s atmospheric evolution: stellar evolution, geological processes, atmospheric escape, biology, etc. Each of these individual processes affects the planetary system as a whole and therefore they all must be considered in the modeling of terrestrial planets.
    [Show full text]
  • Early China DID BABYLONIAN ASTROLOGY
    Early China http://journals.cambridge.org/EAC Additional services for Early China: Email alerts: Click here Subscriptions: Click here Commercial reprints: Click here Terms of use : Click here DID BABYLONIAN ASTROLOGY INFLUENCE EARLY CHINESE ASTRAL PROGNOSTICATION XING ZHAN SHU ? David W. Pankenier Early China / Volume 37 / Issue 01 / December 2014, pp 1 - 13 DOI: 10.1017/eac.2014.4, Published online: 03 July 2014 Link to this article: http://journals.cambridge.org/abstract_S0362502814000042 How to cite this article: David W. Pankenier (2014). DID BABYLONIAN ASTROLOGY INFLUENCE EARLY CHINESE ASTRAL PROGNOSTICATION XING ZHAN SHU ?. Early China, 37, pp 1-13 doi:10.1017/eac.2014.4 Request Permissions : Click here Downloaded from http://journals.cambridge.org/EAC, by Username: dpankenier28537, IP address: 71.225.172.57 on 06 Jan 2015 Early China (2014) vol 37 pp 1–13 doi:10.1017/eac.2014.4 First published online 3 July 2014 DID BABYLONIAN ASTROLOGY INFLUENCE EARLY CHINESE ASTRAL PROGNOSTICATION XING ZHAN SHU 星占術? David W. Pankenier* Abstract This article examines the question whether aspects of Babylonian astral divination were transmitted to East Asia in the ancient period. An often-cited study by the Assyriologist Carl Bezold claimed to discern significant Mesopotamian influence on early Chinese astronomy and astrology. This study has been cited as authoritative ever since, includ- ing by Joseph Needham, although it has never been subjected to careful scrutiny. The present article examines the evidence cited in support of the claim of transmission. Traces of Babylonian Astrology in the “Treatise on the Celestial Offices”? In , the Assyriologist Carl Bezold published an article concerning the Babylonian influence he claimed to discern in Sima Qian’s 司馬遷 and Sima Tan’s 司馬談 “Treatise on the Celestial Offices” 天官書 (c.
    [Show full text]
  • IAU Division C Working Group on Star Names 2019 Annual Report
    IAU Division C Working Group on Star Names 2019 Annual Report Eric Mamajek (chair, USA) WG Members: Juan Antonio Belmote Avilés (Spain), Sze-leung Cheung (Thailand), Beatriz García (Argentina), Steven Gullberg (USA), Duane Hamacher (Australia), Susanne M. Hoffmann (Germany), Alejandro López (Argentina), Javier Mejuto (Honduras), Thierry Montmerle (France), Jay Pasachoff (USA), Ian Ridpath (UK), Clive Ruggles (UK), B.S. Shylaja (India), Robert van Gent (Netherlands), Hitoshi Yamaoka (Japan) WG Associates: Danielle Adams (USA), Yunli Shi (China), Doris Vickers (Austria) WGSN Website: https://www.iau.org/science/scientific_bodies/working_groups/280/ ​ WGSN Email: [email protected] ​ The Working Group on Star Names (WGSN) consists of an international group of astronomers with expertise in stellar astronomy, astronomical history, and cultural astronomy who research and catalog proper names for stars for use by the international astronomical community, and also to aid the recognition and preservation of intangible astronomical heritage. The Terms of Reference and membership for WG Star Names (WGSN) are provided at the IAU website: https://www.iau.org/science/scientific_bodies/working_groups/280/. ​ ​ ​ WGSN was re-proposed to Division C and was approved in April 2019 as a functional WG whose scope extends beyond the normal 3-year cycle of IAU working groups. The WGSN was specifically called out on p. 22 of IAU Strategic Plan 2020-2030: “The IAU serves as the ​ internationally recognised authority for assigning designations to celestial bodies and their surface features. To do so, the IAU has a number of Working Groups on various topics, most notably on the nomenclature of small bodies in the Solar System and planetary systems under Division F and on Star Names under Division C.” WGSN continues its long term activity of researching cultural astronomy literature for star names, and researching etymologies with the goal of adding this information to the WGSN’s online materials.
    [Show full text]
  • Mètodes De Detecció I Anàlisi D'exoplanetes
    MÈTODES DE DETECCIÓ I ANÀLISI D’EXOPLANETES Rubén Soussé Villa 2n de Batxillerat Tutora: Dolors Romero IES XXV Olimpíada 13/1/2011 Mètodes de detecció i anàlisi d’exoplanetes . Índex - Introducció ............................................................................................. 5 [ Marc Teòric ] 1. L’Univers ............................................................................................... 6 1.1 Les estrelles .................................................................................. 6 1.1.1 Vida de les estrelles .............................................................. 7 1.1.2 Classes espectrals .................................................................9 1.1.3 Magnitud ........................................................................... 9 1.2 Sistemes planetaris: El Sistema Solar .............................................. 10 1.2.1 Formació ......................................................................... 11 1.2.2 Planetes .......................................................................... 13 2. Planetes extrasolars ............................................................................ 19 2.1 Denominació .............................................................................. 19 2.2 Història dels exoplanetes .............................................................. 20 2.3 Mètodes per detectar-los i saber-ne les característiques ..................... 26 2.3.1 Oscil·lació Doppler ........................................................... 27 2.3.2 Trànsits
    [Show full text]
  • En Interaktiv Visualisering Av Data Och Upptäcktsmetoder Karin Reidarman
    LIU-ITN-TEK-A-018/045--SE Exoplaneter: En Interaktiv Visualisering av Data och Upptäcktsmetoder Karin Reidarman 2018-11-30 Department of Science and Technology Institutionen för teknik och naturvetenskap Linköping University Linköpings universitet nedewS ,gnipökrroN 47 106-ES 47 ,gnipökrroN nedewS 106 47 gnipökrroN LIU-ITN-TEK-A-018/045--SE Exoplaneter: En Interaktiv Visualisering av Data och Upptäcktsmetoder Examensarbete utfört i Medieteknik vid Tekniska högskolan vid Linköpings universitet Karin Reidarman Handledare Emil Axelsson Examinator Anders Ynnerman Norrköping 2018-11-30 Upphovsrätt Detta dokument hålls tillgängligt på Internet – eller dess framtida ersättare – under en längre tid från publiceringsdatum under förutsättning att inga extra- ordinära omständigheter uppstår. Tillgång till dokumentet innebär tillstånd för var och en att läsa, ladda ner, skriva ut enstaka kopior för enskilt bruk och att använda det oförändrat för ickekommersiell forskning och för undervisning. Överföring av upphovsrätten vid en senare tidpunkt kan inte upphäva detta tillstånd. All annan användning av dokumentet kräver upphovsmannens medgivande. För att garantera äktheten, säkerheten och tillgängligheten finns det lösningar av teknisk och administrativ art. Upphovsmannens ideella rätt innefattar rätt att bli nämnd som upphovsman i den omfattning som god sed kräver vid användning av dokumentet på ovan beskrivna sätt samt skydd mot att dokumentet ändras eller presenteras i sådan form eller i sådant sammanhang som är kränkande för upphovsmannens litterära eller konstnärliga anseende eller egenart. För ytterligare information om Linköping University Electronic Press se förlagets hemsida http://www.ep.liu.se/ Copyright The publishers will keep this document online on the Internet - or its possible replacement - for a considerable time from the date of publication barring exceptional circumstances.
    [Show full text]
  • Introduction the Constellations of the Winter
    Introduction The winter sky is an excellent place to begin exploring the constellations that make up the night sky. Orion is the key, or signpost, for locating many of the other constellations in the winter sky. There are two convenient ways to locate all of the main constellations around Orion once Orion is located. Fortunately, Orion is easy to locate and well known to most people. The first way is to follow lines made by pairs of stars in Orion. The second way is to locate the great winter Orion is the key for hexagon of bright star around Orion. cracking the winter sky. The Constellations of the Winter Sky If you live in the northern latitudes and you scan the sky from the southern horizon to the region overhead, you should be able to see the following constellations on a clear winter night: Orion the Hunter, Canis Major the Great Dog, Canis Minor the Little Dog, Taurus the Bull, Auriga the Charioteer, Gemini the Twins and the Pleiades star cluster. (See the map on the next page). In Greek mythology, Orion was a great hunter who eventually offended the gods, especially Apollo. Apollo tricked Artemis, the Goddess of the hunt, into shooting Orion on a bet. When she discovered that she had shot Orion, she quickly lifted him to the heavens and made him immortal, where he now hunts eternally with his two dogs, Canis Major and Canis Minor. In front of him is his prey Taurus the Bull. The myths surrounding Auriga the Charioteer vary, but it is an ancient constellation dating back to at least to the Ancient Greeks.
    [Show full text]