Astronomy Magazine 2017 Index
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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. -
Arxiv:2010.13762V1 [Astro-Ph.EP] 26 Oct 2020
Draft version October 27, 2020 Typeset using LATEX default style in AASTeX63 A Framework for Relative Biosignature Yields from Future Direct Imaging Missions Noah W. Tuchow 1 and Jason T. Wright 1 1Department of Astronomy & Astrophysics and Center for Exoplanets and Habitable Worlds and Penn State Extraterrestrial Intelligence Center 525 Davey Laboratory The Pennsylvania State University University Park, PA, 16802, USA ABSTRACT Future exoplanet direct imaging missions, such as HabEx and LUVOIR, will select target stars to maximize the number of Earth-like exoplanets that can have their atmospheric compositions charac- terized. Because one of these missions' aims is to detect biosignatures, they should also consider the expected biosignature yield of planets around these stars. In this work, we develop a method of computing relative biosignature yields among potential target stars, given a model of habitability and biosignature genesis, and using a star's habitability history. As an illustration and first application of this method, we use MESA stellar models to calculate the time evolution of the habitable zone, and examine three simple models for biosignature genesis to calculate the relative biosignature yield for different stars. We find that the relative merits of K stars versus F stars depend sensitively on model choice. In particular, use of the present-day habitable zone as a proxy for biosignature detectability favors young, luminous stars lacking the potential for long-term habitability. Biosignature yields are also sensitive to whether life can arise on Cold Start exoplanets that enter the habitable zone after formation, an open question deserving of more attention. Using the case study of biosignature yields calculated for θ Cygni and 55 Cancri, we find that robust mission design and target selection for HabEx and LUVOIR depends on: choosing a specific model of biosignature appearance with time; the terrestrial planet occurrence rate as a function of orbital separation; precise knowledge of stellar properties; and accurate stellar evolutionary histories. -
An October 2003 Amateur Observation of HD 209458B
Tsunami 3-2004 A Shadow over Oxie Anders Nyholm A shadow over Oxie – An October 2003 amateur observation of HD 209458b Anders Nyholm Rymdgymnasiet Kiruna, Sweden April 2004 Tsunami 3-2004 A Shadow over Oxie Anders Nyholm Abstract This paper describes a photometry observation by an amateur astronomer of a transit of the extrasolar planet HD 209458b across its star on the 26th of October 2003. A description of the telescope, CCD imager, software and method used is provided. The preparations leading to the transit observation are described, along with a chronology. The results of the observation (in the form of a time-magnitude diagram) is reproduced, investigated and discussed. It is concluded that the HD 209458b transit most probably was observed. A number of less successful attempts at observing HD 209458b transits in August and October 2003 are also described. A general introduction describes the development in astronomy leading to observations of extrasolar planets in general and amateur observations of extrasolar planets in particular. Tsunami 3-2004 A Shadow over Oxie Anders Nyholm Contents 1. Introduction 3 2. Background 3 2.1 Transit pre-history: Mercury and Venus 3 2.2 Extrasolar planets: a brief history 4 2.3 Early photometry proposals 6 2.4 HD 209458b: discovery and study 6 2.5 Stellar characteristics of HD 209458 6 2.6 Characteristics of HD 209458b 7 3. Observations 7 3.1 Observatory, equipment and software 7 3.2 Test observation of SAO 42275 on the 14th of April 2003 7 3.3 Selection of candidate transits 7 3.4 Test observation and transit observation attempts in August 2003 8 3.5 Transit observation attempt on the 12th of October 2003 8 3.6 Transit observation attempt on the 26th of October 2003 8 4. -
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. -
Hot Jupiters with Relatives: Discovery of Additional Planets in Orbit Around WASP-41 and WASP-47?,??
A&A 586, A93 (2016) Astronomy DOI: 10.1051/0004-6361/201526965 & c ESO 2016 Astrophysics Hot Jupiters with relatives: discovery of additional planets in orbit around WASP-41 and WASP-47?;?? M. Neveu-VanMalle1;2, D. Queloz2;1, D. R. Anderson3, D. J. A. Brown4, A. Collier Cameron5, L. Delrez6, R. F. Díaz1, M. Gillon6, C. Hellier3, E. Jehin6, T. Lister7, F. Pepe1, P. Rojo8, D. Ségransan1, A. H. M. J. Triaud9;10;1, O. D. Turner3, and S. Udry1 1 Observatoire Astronomique de l’Université de Genève, Chemin des Maillettes 51, 1290 Sauverny, Switzerland e-mail: [email protected] 2 Cavendish Laboratory, J J Thomson Avenue, Cambridge, CB3 0HE, UK 3 Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK 4 Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UK 5 SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, Fife, KY16 9SS, UK 6 Institut d’Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août, 17, Bat. B5C, 19C 4000 Liège 1, Belgium 7 Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr. Suite 102, Goleta, CA 93117, USA 8 Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile 9 Centre for Planetary Sciences, University of Toronto at Scarborough, 1265 Military Trail, Toronto, ON, M1C 1A4, Canada 10 Department of Astronomy & Astrophysics, University of Toronto, Toronto, ON, M5S 3H4, Canada Received 14 July 2015 / Accepted 30 September 2015 ABSTRACT We report the discovery of two additional planetary companions to WASP-41 and WASP-47. -
Variable Star Classification and Light Curves Manual
Variable Star Classification and Light Curves An AAVSO course for the Carolyn Hurless Online Institute for Continuing Education in Astronomy (CHOICE) This is copyrighted material meant only for official enrollees in this online course. Do not share this document with others. Please do not quote from it without prior permission from the AAVSO. Table of Contents Course Description and Requirements for Completion Chapter One- 1. Introduction . What are variable stars? . The first known variable stars 2. Variable Star Names . Constellation names . Greek letters (Bayer letters) . GCVS naming scheme . Other naming conventions . Naming variable star types 3. The Main Types of variability Extrinsic . Eclipsing . Rotating . Microlensing Intrinsic . Pulsating . Eruptive . Cataclysmic . X-Ray 4. The Variability Tree Chapter Two- 1. Rotating Variables . The Sun . BY Dra stars . RS CVn stars . Rotating ellipsoidal variables 2. Eclipsing Variables . EA . EB . EW . EP . Roche Lobes 1 Chapter Three- 1. Pulsating Variables . Classical Cepheids . Type II Cepheids . RV Tau stars . Delta Sct stars . RR Lyr stars . Miras . Semi-regular stars 2. Eruptive Variables . Young Stellar Objects . T Tau stars . FUOrs . EXOrs . UXOrs . UV Cet stars . Gamma Cas stars . S Dor stars . R CrB stars Chapter Four- 1. Cataclysmic Variables . Dwarf Novae . Novae . Recurrent Novae . Magnetic CVs . Symbiotic Variables . Supernovae 2. Other Variables . Gamma-Ray Bursters . Active Galactic Nuclei 2 Course Description and Requirements for Completion This course is an overview of the types of variable stars most commonly observed by AAVSO observers. We discuss the physical processes behind what makes each type variable and how this is demonstrated in their light curves. Variable star names and nomenclature are placed in a historical context to aid in understanding today’s classification scheme. -
To Trappist-1 RAIR Golaith Ship
Mission Profile Navigator 10:07 AM - 12/2/2018 page 1 of 10 Interstellar Mission Profile for SGC Navigator - Report - Printable ver 4.3 Start: omicron 2 40 Eri (Star Trek Vulcan home star) (HD Dest: Trappist-1 2Mass J23062928-0502285 in Aquarii [X -9.150] [Y - 26965) (Keid) (HIP 19849) in Eridani [X 14.437] [Y - 38.296] [Z -3.452] 7.102] [Z -2.167] Rendezvous Earth date arrival: Tuesday, December 8, 2420 Ship Type: RAIR Golaith Ship date arrival: Tuesday, January 8, 2419 Type 2: Rendezvous with a coasting leg ( Top speed is reached before mid-point ) Start Position: Start Date: 2-December-2018 Star System omicron 2 40 Eri (Star Trek Vulcan home star) (HD 26965) (Keid) Earth Polar Primary Star: (HIP 19849) RA hours: inactive Type: K0 V Planets: 1e RA min: inactive Binary: B, C, b RA sec: inactive Type: M4.5V, DA2.9 dec. degrees inactive Rank from Earth: 69 Abs Mag.: 5.915956445 dec. minutes inactive dec. seconds inactive Galactic SGC Stats Distance l/y Sector X Y Z Earth to Start Position: 16.2346953 Kappa 14.43696547 -7.10221947 -2.16744969 Destination Arrival Date (Earth time): 8-December-2420 Star System Earth Polar Trappist-1 2Mass J23062928-0502285 Primary Star: RA hours: inactive Type: M8V Planets 4, 3e RA min: inactive Binary: B C RA sec: inactive Type: 0 dec. degrees inactive Rank from Earth 679 Abs Mag.: 18.4 dec. minutes inactive Course Headings SGC decimal dec. seconds inactive RA: (0 <360) 232.905748 dec: (0-180) 91.8817176 Galactic SGC Sector X Y Z Destination: Apparent position | Start of Mission Omega -9.09279603 -38.2336637 -3.46695345 Destination: Real position | Start of Mission Omega -9.09548281 -38.2366036 -3.46626331 Destination: Real position | End of Mission Omega -9.14988933 -38.2961361 -3.45228825 Shifts in distances of Destination Distance l/y X Y Z Change in Apparent vs. -
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. -
A Complete Bibliography of Publications in Journal for the History of Astronomy
A Complete Bibliography of Publications in Journal for the History of Astronomy Nelson H. F. Beebe University of Utah Department of Mathematics, 110 LCB 155 S 1400 E RM 233 Salt Lake City, UT 84112-0090 USA Tel: +1 801 581 5254 FAX: +1 801 581 4148 E-mail: [email protected], [email protected], [email protected] (Internet) WWW URL: http://www.math.utah.edu/~beebe/ 10 May 2021 Version 1.28 Title word cross-reference $8.95 [Had84]. $87 [CWW17]. $89.95 [Gan15]. 8 = 1;2;3 [Cov15]. $90 [Ano15f]. $95 [Swe17c]. c [Kin87, NRKN16, Rag05]. mul [Kur19]. muld [Kur19]. [Kur19]. · $100 [Apt14]. $120 [Hen15b]. $127 [Llo15]. 3 [Ano15f, Ash82, Mal10, Ste12a]. ∆ [MS04]. $135.00 [Smi96]. $14 [Sch15]. $140 [GG14]. $15 [Jar90]. $17.95 [Had84]. $19.95 -1000 [Hub83]. -4000 [Gin91b]. -601 [Mul83, Nau98]. 20 [Ost07]. 2000 [Eva09b]. [Hub83]. -86 [Mar75]. -Ft [Edd71b, Mau13]. $24.95 [Lep14, Bro90]. $27 [W lo15]. $29 -inch [Ost07]. -year [GB95]. -Year-Old [Sha14]. $29.25 [Hea15]. $29.95 [Eva09b]. [Ger17, Mes15]. 30 [Mau13]. $31.00 [Bra15]. $34 [Sul14]. $35 Zaga´_ n [CM10]. [Ano15f, Dev14b, Lau14, Mir17, Rap15a]. $38 [Dan19b, Vet19]. $39.95 [Mol14b]. /Catalogue [Kun91]. /Charles [Tur07]. $39.99 [Bec15]. $40 [Dun20, LF15, Rob86]. /Collected [Gin93]. /Heretic [Tes10]. 40 [Edd71b]. $42 [Nau98]. $45 [Kes15]. /the [War08]. $49.95 [Ree20]. $49.99 [Bec15]. $50 [Kru17, Rem15]. $55 [Bon19b]. $60 [Mal15]. 0 [Ave18, Hei14a, Oes15, Swe17c, Wlo15, 600 [GB95]. $72 [Ave18]. $79 [Wil15]. 1 2 Ash82]. [Dic97a]. 1970 [Kru08]. 1971 [Wil75]. 1973 [Doe19]. 1975 [Ost80]. 1976 [Gin02d]. 1979 1 [Ano15f, BH73a, Ber14, Bru78b, Eva87b, [Ano78d]. -
Double and Multiple Star Measurements in the Northern Sky with a 10” Newtonian and a Fast CCD Camera in 2006 Through 2009
Vol. 6 No. 3 July 1, 2010 Journal of Double Star Observations Page 180 Double and Multiple Star Measurements in the Northern Sky with a 10” Newtonian and a Fast CCD Camera in 2006 through 2009 Rainer Anton Altenholz/Kiel, Germany e-mail: rainer.anton”at”ki.comcity.de Abstract: Using a 10” Newtonian and a fast CCD camera, recordings of double and multiple stars were made at high frame rates with a notebook computer. From superpositions of “lucky images”, measurements of 139 systems were obtained and compared with literature data. B/w and color images of some noteworthy systems are also presented. mented double stars, as will be described in the next Introduction section. Generally, I used a red filter to cope with By using the technique of “lucky imaging”, seeing chromatic aberration of the Barlow lens, as well as to effects can strongly be reduced, and not only the reso- reduce the atmospheric spectrum. For systems with lution of a given telescope can be pushed to its limits, pronounced color contrast, I also made recordings but also the accuracy of position measurements can be with near-IR, green and blue filters in order to pro- better than this by about one order of magnitude. This duce composite images. This setup was the same as I has already been demonstrated in earlier papers in used with telescopes under the southern sky, and as I this journal [1-3]. Standard deviations of separation have described previously [1-3]. Exposure times varied measurements of less than +/- 0.05 msec were rou- between 0.5 msec and 100 msec, depending on the tinely obtained with telescopes of 40 or 50 cm aper- star brightness, and on the seeing. -
Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland)
Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland) American Astronomical Society August, 2019 100 — New Discoveries scope (JWST), as well as other large ground-based and space-based telescopes coming online in the next 100.01 — Review of TESS’s First Year Survey and two decades. Future Plans The status of the TESS mission as it completes its first year of survey operations in July 2019 will bere- George Ricker1 viewed. The opportunities enabled by TESS’s unique 1 Kavli Institute, MIT (Cambridge, Massachusetts, United States) lunar-resonant orbit for an extended mission lasting more than a decade will also be presented. Successfully launched in April 2018, NASA’s Tran- siting Exoplanet Survey Satellite (TESS) is well on its way to discovering thousands of exoplanets in orbit 100.02 — The Gemini Planet Imager Exoplanet Sur- around the brightest stars in the sky. During its ini- vey: Giant Planet and Brown Dwarf Demographics tial two-year survey mission, TESS will monitor more from 10-100 AU than 200,000 bright stars in the solar neighborhood at Eric Nielsen1; Robert De Rosa1; Bruce Macintosh1; a two minute cadence for drops in brightness caused Jason Wang2; Jean-Baptiste Ruffio1; Eugene Chiang3; by planetary transits. This first-ever spaceborne all- Mark Marley4; Didier Saumon5; Dmitry Savransky6; sky transit survey is identifying planets ranging in Daniel Fabrycky7; Quinn Konopacky8; Jennifer size from Earth-sized to gas giants, orbiting a wide Patience9; Vanessa Bailey10 variety of host stars, from cool M dwarfs to hot O/B 1 KIPAC, Stanford University (Stanford, California, United States) giants. 2 Jet Propulsion Laboratory, California Institute of Technology TESS stars are typically 30–100 times brighter than (Pasadena, California, United States) those surveyed by the Kepler satellite; thus, TESS 3 Astronomy, California Institute of Technology (Pasadena, Califor- planets are proving far easier to characterize with nia, United States) follow-up observations than those from prior mis- 4 Astronomy, U.C. -
Astronomy Magazine 2011 Index Subject Index
Astronomy Magazine 2011 Index Subject Index A AAVSO (American Association of Variable Star Observers), 6:18, 44–47, 7:58, 10:11 Abell 35 (Sharpless 2-313) (planetary nebula), 10:70 Abell 85 (supernova remnant), 8:70 Abell 1656 (Coma galaxy cluster), 11:56 Abell 1689 (galaxy cluster), 3:23 Abell 2218 (galaxy cluster), 11:68 Abell 2744 (Pandora's Cluster) (galaxy cluster), 10:20 Abell catalog planetary nebulae, 6:50–53 Acheron Fossae (feature on Mars), 11:36 Adirondack Astronomy Retreat, 5:16 Adobe Photoshop software, 6:64 AKATSUKI orbiter, 4:19 AL (Astronomical League), 7:17, 8:50–51 albedo, 8:12 Alexhelios (moon of 216 Kleopatra), 6:18 Altair (star), 9:15 amateur astronomy change in construction of portable telescopes, 1:70–73 discovery of asteroids, 12:56–60 ten tips for, 1:68–69 American Association of Variable Star Observers (AAVSO), 6:18, 44–47, 7:58, 10:11 American Astronomical Society decadal survey recommendations, 7:16 Lancelot M. Berkeley-New York Community Trust Prize for Meritorious Work in Astronomy, 3:19 Andromeda Galaxy (M31) image of, 11:26 stellar disks, 6:19 Antarctica, astronomical research in, 10:44–48 Antennae galaxies (NGC 4038 and NGC 4039), 11:32, 56 antimatter, 8:24–29 Antu Telescope, 11:37 APM 08279+5255 (quasar), 11:18 arcminutes, 10:51 arcseconds, 10:51 Arp 147 (galaxy pair), 6:19 Arp 188 (Tadpole Galaxy), 11:30 Arp 273 (galaxy pair), 11:65 Arp 299 (NGC 3690) (galaxy pair), 10:55–57 ARTEMIS spacecraft, 11:17 asteroid belt, origin of, 8:55 asteroids See also names of specific asteroids amateur discovery of, 12:62–63