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Where Are the Distant Worlds? Star Maps
W here Are the Distant Worlds? Star Maps Abo ut the Activity Whe re are the distant worlds in the night sky? Use a star map to find constellations and to identify stars with extrasolar planets. (Northern Hemisphere only, naked eye) Topics Covered • How to find Constellations • Where we have found planets around other stars Participants Adults, teens, families with children 8 years and up If a school/youth group, 10 years and older 1 to 4 participants per map Materials Needed Location and Timing • Current month's Star Map for the Use this activity at a star party on a public (included) dark, clear night. Timing depends only • At least one set Planetary on how long you want to observe. Postcards with Key (included) • A small (red) flashlight • (Optional) Print list of Visible Stars with Planets (included) Included in This Packet Page Detailed Activity Description 2 Helpful Hints 4 Background Information 5 Planetary Postcards 7 Key Planetary Postcards 9 Star Maps 20 Visible Stars With Planets 33 © 2008 Astronomical Society of the Pacific www.astrosociety.org Copies for educational purposes are permitted. Additional astronomy activities can be found here: http://nightsky.jpl.nasa.gov Detailed Activity Description Leader’s Role Participants’ Roles (Anticipated) Introduction: To Ask: Who has heard that scientists have found planets around stars other than our own Sun? How many of these stars might you think have been found? Anyone ever see a star that has planets around it? (our own Sun, some may know of other stars) We can’t see the planets around other stars, but we can see the star. -
100 Closest Stars Designation R.A
100 closest stars Designation R.A. Dec. Mag. Common Name 1 Gliese+Jahreis 551 14h30m –62°40’ 11.09 Proxima Centauri Gliese+Jahreis 559 14h40m –60°50’ 0.01, 1.34 Alpha Centauri A,B 2 Gliese+Jahreis 699 17h58m 4°42’ 9.53 Barnard’s Star 3 Gliese+Jahreis 406 10h56m 7°01’ 13.44 Wolf 359 4 Gliese+Jahreis 411 11h03m 35°58’ 7.47 Lalande 21185 5 Gliese+Jahreis 244 6h45m –16°49’ -1.43, 8.44 Sirius A,B 6 Gliese+Jahreis 65 1h39m –17°57’ 12.54, 12.99 BL Ceti, UV Ceti 7 Gliese+Jahreis 729 18h50m –23°50’ 10.43 Ross 154 8 Gliese+Jahreis 905 23h45m 44°11’ 12.29 Ross 248 9 Gliese+Jahreis 144 3h33m –9°28’ 3.73 Epsilon Eridani 10 Gliese+Jahreis 887 23h06m –35°51’ 7.34 Lacaille 9352 11 Gliese+Jahreis 447 11h48m 0°48’ 11.13 Ross 128 12 Gliese+Jahreis 866 22h39m –15°18’ 13.33, 13.27, 14.03 EZ Aquarii A,B,C 13 Gliese+Jahreis 280 7h39m 5°14’ 10.7 Procyon A,B 14 Gliese+Jahreis 820 21h07m 38°45’ 5.21, 6.03 61 Cygni A,B 15 Gliese+Jahreis 725 18h43m 59°38’ 8.90, 9.69 16 Gliese+Jahreis 15 0h18m 44°01’ 8.08, 11.06 GX Andromedae, GQ Andromedae 17 Gliese+Jahreis 845 22h03m –56°47’ 4.69 Epsilon Indi A,B,C 18 Gliese+Jahreis 1111 8h30m 26°47’ 14.78 DX Cancri 19 Gliese+Jahreis 71 1h44m –15°56’ 3.49 Tau Ceti 20 Gliese+Jahreis 1061 3h36m –44°31’ 13.09 21 Gliese+Jahreis 54.1 1h13m –17°00’ 12.02 YZ Ceti 22 Gliese+Jahreis 273 7h27m 5°14’ 9.86 Luyten’s Star 23 SO 0253+1652 2h53m 16°53’ 15.14 24 SCR 1845-6357 18h45m –63°58’ 17.40J 25 Gliese+Jahreis 191 5h12m –45°01’ 8.84 Kapteyn’s Star 26 Gliese+Jahreis 825 21h17m –38°52’ 6.67 AX Microscopii 27 Gliese+Jahreis 860 22h28m 57°42’ 9.79, -
Tímaákvarðanir Á Myrkvum Valinna Myrkvatvístirna Og Þvergöngum Fjarreikistjarna, Árin 2017-2018, Og Fjarlægðamælingar
Tímaákvarðanir á myrkvum valinna myrkvatvístirna, þvergöngum fjarreikistjarna og fjarlægðamælingar, árin 2017—2018 Snævarr Guðmundsson 2019 Náttúrustofa Suðausturlands Litlubrú 2, 780 Höfn í Hornafirði Nýheimar, Litlubrú 2 780 Höfn Í Hornafirði www.nattsa.is Skýrsla nr. Dagsetning Dreifing NattSA 2019-04 10. apríl 2019 Opin Fjöldi síðna 109 Tímaákvarðanir á myrkvum valinna myrkvatvístirna, Fjöldi mynda 229 þvergöngum fjarreikistjarna og fjarlægðamælingar, árin 2017- 2018. Verknúmer 1280 Höfundur: Snævarr Guðmundsson Verkefnið var styrkt af Prófarkarlestur Þorsteinn Sæmundsson, Kristín Hermannsdóttir og Lilja Jóhannesdóttir Útdráttur Hér er gert grein fyrir stjörnuathugunum á Hornafirði á árabilinu 2017 til loka árs 2018. Í flestum tilfellum voru viðfangsefnin óeiginlegar breytistjörnur, aðallega myrkvatvístirni, en einnig var fylgst með nokkrum fjarreikistjörnum. Í mælingum á myrkvatvístirnum og fjarreikistjörnum er markmiðið að tímasetja myrkva og þvergöngur. Einnig er sagt frá niðurstöðum á nándarstjörnunni Ross 248 og athugunum á lausþyrpingunni NGC 7790 og breytistjörnum í nágrenni hennar. Markmið mælinga á nándarstjörnu og lausþyrpingum er að meta fjarlægðir eða aðra eiginleika fyrirbæranna. Að lokum eru kynntar athuganir á litrófi nokkurra bjartra stjarna. Í samantektinni er sagt frá hverju viðfangsefni í sérköflum. Þessi samantekt er sú þriðja um stjörnuathuganir sem er gefin út af Náttúrustofu Suðausturlands. Niðurstöður hafa verið sendar í alþjóðlegan gagnagrunn þar sem þær, ásamt fjölda sambærilegra mæligagna frá stjörnuáhugamönnum, eru aðgengilegar stjarnvísindasamfélaginu. Hægt er að sækja skýrslur um stjörnuathuganir á vefslóðina: http://nattsa.is/utgefid-efni/. Lykilorð: myrkvatvístirni, fjarreikistjörnur, breytistjörnur, lausþyrpingar, ljósmælingar, fjarlægðir stjarna, litróf stjarna. ii Tímaákvarðanir á myrkvum valinna myrkvatvístirna, þvergöngum fjarreikistjarna og fjarlægðamælingar, árin 2017-2018. — Annáll 2017-2018. Timings of selected eclipsing binaries, exoplanet transits and distance measurements in 2017- 2018. -
The Search for Exomoons and the Characterization of Exoplanet Atmospheres
Corso di Laurea Specialistica in Astronomia e Astrofisica The search for exomoons and the characterization of exoplanet atmospheres Relatore interno : dott. Alessandro Melchiorri Relatore esterno : dott.ssa Giovanna Tinetti Candidato: Giammarco Campanella Anno Accademico 2008/2009 The search for exomoons and the characterization of exoplanet atmospheres Giammarco Campanella Dipartimento di Fisica Università degli studi di Roma “La Sapienza” Associate at Department of Physics & Astronomy University College London A thesis submitted for the MSc Degree in Astronomy and Astrophysics September 4th, 2009 Università degli Studi di Roma ―La Sapienza‖ Abstract THE SEARCH FOR EXOMOONS AND THE CHARACTERIZATION OF EXOPLANET ATMOSPHERES by Giammarco Campanella Since planets were first discovered outside our own Solar System in 1992 (around a pulsar) and in 1995 (around a main sequence star), extrasolar planet studies have become one of the most dynamic research fields in astronomy. Our knowledge of extrasolar planets has grown exponentially, from our understanding of their formation and evolution to the development of different methods to detect them. Now that more than 370 exoplanets have been discovered, focus has moved from finding planets to characterise these alien worlds. As well as detecting the atmospheres of these exoplanets, part of the characterisation process undoubtedly involves the search for extrasolar moons. The structure of the thesis is as follows. In Chapter 1 an historical background is provided and some general aspects about ongoing situation in the research field of extrasolar planets are shown. In Chapter 2, various detection techniques such as radial velocity, microlensing, astrometry, circumstellar disks, pulsar timing and magnetospheric emission are described. A special emphasis is given to the transit photometry technique and to the two already operational transit space missions, CoRoT and Kepler. -
Useful Constants
Appendix A Useful Constants A.1 Physical Constants Table A.1 Physical constants in SI units Symbol Constant Value c Speed of light 2.997925 × 108 m/s −19 e Elementary charge 1.602191 × 10 C −12 2 2 3 ε0 Permittivity 8.854 × 10 C s / kgm −7 2 μ0 Permeability 4π × 10 kgm/C −27 mH Atomic mass unit 1.660531 × 10 kg −31 me Electron mass 9.109558 × 10 kg −27 mp Proton mass 1.672614 × 10 kg −27 mn Neutron mass 1.674920 × 10 kg h Planck constant 6.626196 × 10−34 Js h¯ Planck constant 1.054591 × 10−34 Js R Gas constant 8.314510 × 103 J/(kgK) −23 k Boltzmann constant 1.380622 × 10 J/K −8 2 4 σ Stefan–Boltzmann constant 5.66961 × 10 W/ m K G Gravitational constant 6.6732 × 10−11 m3/ kgs2 M. Benacquista, An Introduction to the Evolution of Single and Binary Stars, 223 Undergraduate Lecture Notes in Physics, DOI 10.1007/978-1-4419-9991-7, © Springer Science+Business Media New York 2013 224 A Useful Constants Table A.2 Useful combinations and alternate units Symbol Constant Value 2 mHc Atomic mass unit 931.50MeV 2 mec Electron rest mass energy 511.00keV 2 mpc Proton rest mass energy 938.28MeV 2 mnc Neutron rest mass energy 939.57MeV h Planck constant 4.136 × 10−15 eVs h¯ Planck constant 6.582 × 10−16 eVs k Boltzmann constant 8.617 × 10−5 eV/K hc 1,240eVnm hc¯ 197.3eVnm 2 e /(4πε0) 1.440eVnm A.2 Astronomical Constants Table A.3 Astronomical units Symbol Constant Value AU Astronomical unit 1.4959787066 × 1011 m ly Light year 9.460730472 × 1015 m pc Parsec 2.0624806 × 105 AU 3.2615638ly 3.0856776 × 1016 m d Sidereal day 23h 56m 04.0905309s 8.61640905309 -
Dynamical Stability of the Inner Belt Around Epsilon Eridani
A&A 499, L13–L16 (2009) Astronomy DOI: 10.1051/0004-6361/200811609 & c ESO 2009 Astrophysics Letter to the Editor Dynamical stability of the inner belt around Epsilon Eridani M. Brogi1, F. Marzari2, and P. Paolicchi1 1 University of Pisa, Department of Physics, Largo Pontecorvo 3, 56127 Pisa, Italy e-mail: [email protected]; [email protected] 2 University of Padua, Department of Physics, via Marzolo 8, 35131 Padua, Italy e-mail: [email protected] Received 31 December 2008 / Accepted 17 April 2009 ABSTRACT Context. Recent observations with Spitzer and the Caltech Submillimeter Observatory have discovered the presence of a dust belt at about 3 AU, internal to the orbit of known exoplanet Eri b. Aims. We investigate via numerical simulations the dynamical stability of a putative belt of minor bodies, as the collisional source of the observed dust ring. This belt must be located inside the orbit of the planet, since any external source would be ineffective in resupplying the inner dust band. Methods. We explore the long-term behaviour of the minor bodies of the belt and how their lifetime depends on the orbital parameters of the planet, in particular for reaching a steady state. Results. Our computations show that for an eccentricity of Eri b equal or higher than 0.15, the source belt is severely depleted of its original mass and substantially reduced in width. A “dynamical” limit of 0.10 comes out, which is inconsistent with the first estimate of the planet eccentricity (0.70 ± 0.04), while the alternate value (0.23 ± 0.2) can be consistent within the uncertainties. -
The Photosphere and Circumstellar Environment of the Be Star Achernar
New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry Proceedings IAU Symposium No. 307, 2014 c International Astronomical Union 2015 G.Meynet,C.Georgy,J.H.Groh&Ph.Stee,eds. doi:10.1017/S1743921314006905 The photosphere and circumstellar environment of the Be star Achernar Daniel M. Faes1,2, Armando Domiciano de Souza2,AlexC.Carciofi1 and Philippe Bendjoya2 1 Instituto de Astronomia, Geof´ısica e Ciˆencias Atmosf´ericas, Universidade de S˜ao Paulo, Rua do Mat˜ao 1226, Cidade Universit´aria, 05508-900, S˜ao Paulo, SP, Brazil email: [email protected] 2 Lab. J.-L. Lagrange, UMR 7293 - Observatoire de la Cˆote d’Azur (OCA), Univ. de Nice-Sophia Antipolis (UNS), CNRS, Valrose, 06108 Nice, France Abstract. Achernar is a key target to investigate high stellar rotation and the Be phenonemon. It is also the hottest star for which detailed photospheric information is available. Here we report our results to determine the photospheric parameters of Achernar and evaluate how the emission of a Viscous Decretion Disk (VDD) around it would be observable. The analysis is based on interferometric data (PIONIER and AMBER at ESO-VLTI), complemented by spectroscopy and polarimetry for the circumstellar emission. For the first time fundamental parameters of a Be photosphere were determined. The presence of a residual disk at the quiescent phase and some characteristics of the new formed disk (2013 activity) are also discussed. This is rare opportunity to precisely determine the stellar brightness distribution and evaluate the evolution of a just formed Be disk. Keywords. stars: individual (Achernar), stars: fundamental parameters, techniques: interfero- metric, circumstellar matter, stars: emission-line, Be 1. -
2021 Solar Rituality and Ephemerides
HE LANETARY YSTEM T P S Ideas, Formulas and Forms for a new Culture/Civilization 2021 SOLAR RITUALITY AND EPHEMERIDES (December 2020) [email protected] 1 2021 SOLAR RITUALITY AND EPHEMERIDES A rhythmic and ritual coordination and sowing for a planetary Order The TPS solar Sowing Ia, Fa a F a C a Ca intends to a a a" a aa " a ba a " the cyclic pulsations of the higher Creators, the planetary, solar and cosmic Entities: the conscious Dream of a New Culture and Civilization, as a manifestation on Earth of the evolutionary Plan and of a new human planetary Order.1 By working we learn to work, and in this Workshop of spatial Thought we learn together to build more and more knowingly Harmonic Thought-forms, as a result of a right or heavenly way of being and existing, in order to set up a better Future and to progressively release our humanity from its lower trammels. Humanity can and has to spread, in an impersonal and disinterested way, Seeds or Ideas capable of fertilizing consciousness making it resound to infinity: "Culture is a treasure of consciousness, therefore the field of the sowing of the new Thought is the human consciousness ... It is a vast field like Heaven: no one knows its boundaries. Thus the seeds to be spread have no number or form ... Only with formless seeds an infinite field can be cultivated. And the soil of human consciousness is ready to welcome them: many signs prove it, both above and below, and sowing cannot be deferred". -
The Spinning-Top Be Star Achernar from VLTI-VINCI
A&A 407, L47–L50 (2003) Astronomy DOI: 10.1051/0004-6361:20030786 & c ESO 2003 Astrophysics The spinning-top Be star Achernar from VLTI-VINCI A. Domiciano de Souza1,P.Kervella2,S.Jankov3,L.Abe1, F. Vakili1,3,E.diFolco4, and F. Paresce4 1 Laboratoire Univ. d’Astroph. de Nice (LUAN), CNRS UMR 6525, Parc Valrose, 06108 Nice Cedex 02, France 2 European Southern Observatory (ESO), Alonso de Cordova 3107, Casilla 19001, Vitacura, Santiago 19, Chile 3 Observatoire de la Cˆote d’Azur, D´epartement FRESNEL, CNRS UMR 6528, Boulevard de l’Observatoire, Letter to the Editor BP 4229, 06304 Nice, France 4 European Southern Observatory (ESO), Karl-Schwarzschild str. 2, 85748 Garching, Germany Received 5 May 2003 / Accepted 22 May 2003 Abstract. We report here the first observations of a rapidly rotating Be star, α Eridani, using Earth-rotation synthesis on the Very Large Telescope (VLT) Interferometer. Our measures correspond to a 2a/2b = 1.56 0.05 apparent oblate star, 2a and 2b being the equivalent uniform disc angular diameters in the equatorial and polar direction. Considering± the presence of a circum- stellar envelope (CSE) we argue that our measurement corresponds to a truly distorted star since α Eridani exhibited negligible Hα emission during the interferometric observations. In this framework we conclude that the commonly adopted Roche approx- imation (uniform rotation and centrally condensed mass) should not apply to α Eridani. This result opens new perspectives to basic astrophysical problems, such as rotationally enhanced mass loss and internal angular momentum distribution. In addition to its intimate relation with magnetism and pulsation, rapid rotation thus provides a key to the Be phenomenon: one of the outstanding non-resolved problems in stellar physics. -
Astron 104 Laboratory #7 the H-R Diagram Section 10.1, 10.5
Lab #7 Name: Date: Section: Astron 104 Laboratory #7 The H-R Diagram Section 10.1, 10.5 Introduction The Hertzsprung-Russell diagram, or H-R diagram for short, relates two fundamental properties of stars and helps reveal how stars work. In an H-R diagram we plot the luminosity (how bright it is) of a star against its surface temperature. The majority of the stars lie on a narrow band which runs from the top left of the diagram (hot, bright stars) to the bottom right (cool, dim stars). This band is known as the main sequence, and highlights where stars spend the majority of their lives. A small number of stars near the ends of their lives do not lie on the main sequence, and these are classified as red giants, red supergiants, or white dwarfs, depending on their stage of evolution. Experiment 1 This lab will utilize the color and luminosity of different stars, enabling you to construct a Hertzsprung-Russell diagram. 1. Go to the Start Menu 2. Click on All Programs 3. Click on Virtual Astronomy 4. Click on Start Virtual Astronomy Lab 5. Click on Unit 16: The Hertzsprung Russell Diagram 6. Click on Start Lab Astron 104 Spring 2016 1 Lab #7 7. Click on View the Stars The view shows a portion of the sky containing a number of stars, with a range of surface temperatures. The stars are shown as colored, with the hottest stars being blue and the coolest stars red. By selecting \Number of stars" from the top menu, you may change the number of stars appearing in the window. -
Detectability of Atmospheric Features of Earth-Like Planets in the Habitable
Astronomy & Astrophysics manuscript no. Wunderlich_etal_2019_arxiv c ESO 2019 May 8, 2019 Detectability of atmospheric features of Earth-like planets in the habitable zone around M dwarfs Fabian Wunderlich1, Mareike Godolt1, John Lee Grenfell2, Steffen Städt3, Alexis M. S. Smith2, Stefanie Gebauer2, Franz Schreier3, Pascal Hedelt3, and Heike Rauer1; 2; 4 1 Zentrum für Astronomie und Astrophysik, Technische Universität Berlin, Hardenbergstraße 36, 10623 Berlin, Germany e-mail: [email protected] 2 Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt, Rutherfordstraße 2, 12489 Berlin, Germany 3 Institut für Methodik der Fernerkundung, Deutsches Zentrum für Luft- und Raumfahrt, 82234 Oberpfaffenhofen, Germany 4 Institut für Geologische Wissenschaften, Freie Universität Berlin, Malteserstr. 74-100, 12249 Berlin, Germany ABSTRACT Context. The characterisation of the atmosphere of exoplanets is one of the main goals of exoplanet science in the coming decades. Aims. We investigate the detectability of atmospheric spectral features of Earth-like planets in the habitable zone (HZ) around M dwarfs with the future James Webb Space Telescope (JWST). Methods. We used a coupled 1D climate-chemistry-model to simulate the influence of a range of observed and modelled M-dwarf spectra on Earth-like planets. The simulated atmospheres served as input for the calculation of the transmission spectra of the hy- pothetical planets, using a line-by-line spectral radiative transfer model. To investigate the spectroscopic detectability of absorption bands with JWST we further developed a signal-to-noise ratio (S/N) model and applied it to our transmission spectra. Results. High abundances of methane (CH4) and water (H2O) in the atmosphere of Earth-like planets around mid to late M dwarfs increase the detectability of the corresponding spectral features compared to early M-dwarf planets. -
The Fundamentals of Stargazing Sky Tours South
The Fundamentals of Stargazing Sky Tours South 01 – The March Sky Copyright © 2014-2016 Mintaka Publishing Inc. www.CosmicPursuits.com -2- The Constellation Orion Let’s begin the tours of the deep-southern sky with the most famous and unmistakable constellation in the heavens, Orion, which will serve as a guide for other bright constellations in the southern late-summer sky. Head outdoors around 8 or 9 p.m. on an evening in early March, and turn towards the north. If you can’t find north, you can ask someone else, or get a small inexpensive compass, or use the GPS in your smartphone or tablet. But you need to face at least generally northward before you can proceed. You will also need a good unobstructed view of the sky in the north, so you may need to get away from structures and trees and so on. The bright stars of the constellation Orion (in this map, south is up and east is to the right) And bring a pair of binoculars if you have them, though they are not necessary for this tour. Fundamentals of Stargazing -3- Now that you’re facing north with a good view of a clear sky, make a 1/8th of a turn to your left. Now you are facing northwest, more or less. Turn your gaze upward about halfway to the point directly overhead. Look for three bright stars in a tidy line. They span a patch of sky about as wide as your three middle fingers held at arm’s length. This is the “belt” of the constellation Orion.