Hawaii's Sky Tonight

Total Page：16

File Type：pdf, Size：1020Kb

Hawaii’s Sky Tonight DECEMBER BISHOP MUSEUM www.bishopmuseum.org/planetarium 2018 © 2016 Bishop Museum. All rights reserved. For personal use only. N Unauthorized copying, distribution, or adaptation is strictly prohibited. Ursa Minor (Little Dipper) Polaris (North Star) Cepheus Deneb Gemini Cassiopeia Castor Auriga The Milky Cygnus Pollux Capella Way Algol Andromeda Canis Perseus Minor Pegasus Aries E Procyon Aldebaran Pleiades W Betelgeuse Taurus Orion Pisces Aquarius Rigel Mars Sirius Lepus Cetus Eridanus Fomalhaut Piscis Phoenix Austrinus Achernar S HOW TO USE THIS MAP: HAWAIIAN STAR NAMES: SKY MAP KEY: 1. Find north in the sky by using the 1st Magnitude 3rd Magnitude ∙Achernar = Kalanikauleleāiwi (Chief with Altar Made of Bones) Big Dipper or Cassiopeia. 2nd Magnitude 4th Magnitude 2. Face north and hold the sky map ∙Aldebaran = Kapuahi (Sacred Fire) directly in front of you with “N” (on Planets ∙Auriga/Capella = Hōkūlei (Lei of Stars) the map) at the bottom. ∙Betelgeuse = Kalaukoko (Brilliant Red 3. Look for stars in the northern sky. Stars Constellations Planets Star) 4. To view other parts of the sky, turn ∙Cassiopeia = 'Iwa Keli'i (Great Frigate to that direction and hold the sky MOON “MAHINA” PHASES: Bird) map with that same direction at ∙Cetus = Kohōla (The Whale) the bottom. ∙Gemini = Nā Māhoe (The Twins) ∙Orion = Ka Heihei O Nā Keiki (The Cats VIEWING TIMES FOR MAP: Cradle Game of the Children) 10 PM 9 PM 8 PM ∙Pleiades = Makali'i (The Tiny Eyes) Early Mid Late New First Full Last ∙Polaris = Hōkūpa'a (Stationary Star) Month Month Month 12/7 12/15 12/22 12/29 ∙Sirius = A'ā (Fire) This sky map is set for the latitude of O'ahu (21˚ N), but can be used for other Hawaiian Islands, from Hawai'i (19˚ N) to Kaua'i (22˚ N)..

Copy Link

Recommended publications

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.
[Show full text]
Sydney Observatory Night Sky Map September 2012 a Map for Each Month of the Year, to Help You Learn About the Night Sky
Sydney Observatory night sky map September 2012 A map for each month of the year, to help you learn about the night sky www.sydneyobservatory.com This star chart shows the stars and constellations visible in the night sky for Sydney, Melbourne, Brisbane, Canberra, Hobart, Adelaide and Perth for September 2012 at about 7:30 pm (local standard time). For Darwin and similar locations the chart will still apply, but some stars will be lost off the southern edge while extra stars will be visible to the north. Stars down to a brightness or magnitude limit of 4.5 are shown. To use this chart, rotate it so that the direction you are facing (north, south, east or west) is shown at the bottom. The centre of the chart represents the point directly above your head, called the zenith, and the outer circular edge represents the horizon. h t r No Star brightness Moon phase Last quarter: 08th Zero or brighter New Moon: 16th 1st magnitude LACERTA nd Deneb First quarter: 23rd 2 CYGNUS Full Moon: 30th rd N 3 E LYRA th Vega W 4 LYRA N CORONA BOREALIS HERCULES BOOTES VULPECULA SAGITTA PEGASUS DELPHINUS Arcturus Altair EQUULEUS SERPENS AQUILA OPHIUCHUS SCUTUM PISCES Moon on 23rd SERPENS Zubeneschamali AQUARIUS CAPRICORNUS E SAGITTARIUS LIBRA a Saturn Centre of the Galaxy Antares Zubenelgenubi t s Antares VIRGO s t SAGITTARIUS P SCORPIUS P e PISCESMICROSCOPIUM AUSTRINUS SCORPIUS Mars Spica W PISCIS AUSTRINUS CORONA AUSTRALIS Fomalhaut Centre of the Galaxy TELESCOPIUM LUPUS ARA GRUSGRUS INDUS NORMA CORVUS INDUS CETUS SCULPTOR PAVO CIRCINUS CENTAURUS TRIANGULUM
[Show full text]
An Independent Determination of Fomalhaut B's Orbit and The
A&A 561, A43 (2014) Astronomy DOI: 10.1051/0004-6361/201322229 & c ESO 2013 Astrophysics An independent determination of Fomalhaut b’s orbit and the dynamical effects on the outer dust belt H. Beust1, J.-C. Augereau1, A. Bonsor1,J.R.Graham3,P.Kalas3 J. Lebreton1, A.-M. Lagrange1, S. Ertel1, V. Faram az 1, and P. Thébault2 1 UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG) UMR 5274, 38041 Grenoble, France e-mail: [email protected] 2 Observatoire de Paris, Section de Meudon, 92195 Meudon Principal Cedex, France 3 Department of Astronomy, University of California at Berkeley, Berkeley CA 94720, USA Received 8 July 2013 / Accepted 13 November 2013 ABSTRACT Context. The nearby star Fomalhaut harbors a cold, moderately eccentric (e ∼ 0.1) dust belt with a sharp inner edge near 133 au. A low-mass, common proper motion companion, Fomalhaut b (Fom b), was discovered near the inner edge and was identiﬁed as a planet candidate that could account for the belt morphology. However, the most recent orbit determination based on four epochs of astrometry over eight years reveals a highly eccentric orbit (e = 0.8 ± 0.1) that appears to cross the belt in the sky plane projection. Aims. We perform here a full orbital determination based on the available astrometric data to independently validate the orbit estimates previously presented. Adopting our values for the orbital elements and their associated uncertainties, we then study the dynamical interaction between the planet and the dust ring, to check whether the proposed disk sculpting scenario by Fom b is plausible.
[Show full text]
Sirius Astronomer
FEBRUARY 2013 Free to members, subscriptions $12 for 12 Volume 40, Number 2 Jupiter is featured often in this newsletter because it is one of the most appealing objects in the night sky even for very small telescopes. The king of Solar System planets is prominent in the night sky throughout the month, located near Aldebaran in the constellation Taurus. Pat Knoll took this image on January 18th from his observing site at Kearney Mesa, California, using a Meade LX200 Classic at f/40 with a 4X Powermate. The image was compiled from a two-minute run with an Imaging Source DFK 21AU618.AS camera . OCA CLUB MEETING STAR PARTIES COMING UP The free and open club meeting The Black Star Canyon site will open The next session of the Beginners will be held February 8 at 7:30 PM on February 2. The Anza site will be Class will be held at the Heritage in the Irvine Lecture Hall of the open on February 9. Members are en- Museum of Orange County at Hashinger Science Center at couraged to check the website calen- 3101 West Harvard Street in San- Chapman University in Orange. dar for the latest updates on star par- ta Ana on February 1st. The fol- This month, UCSD’s Dr. Burgasser ties and other events. lowing class will be held March will present “The Coldest Stars: Y- 1st Dwarfs and the Fuzzy Border be- Please check the website calendar for tween Stars and Planets.” the outreach events this month! Volun- GOTO SIG: TBA teers are always welcome! Astro-Imagers SIG: Feb.
[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]
Download This Article in PDF Format
A&A 574, A120 (2015) Astronomy DOI: 10.1051/0004-6361/201424944 & c ESO 2015 Astrophysics High-contrast imaging with Spitzer: deep observations of Vega, Fomalhaut, and Eridani Markus Janson1, Sascha P. Quanz2, Joseph C. Carson3, Christian Thalmann2, David Lafrenière4, and Adam Amara2 1 Department of Astronomy, Stockholm University, 106 91 Stockholm, Sweden e-mail: [email protected] 2 Institute for Astronomy, ETH Zurich, 9093 Zurich, Switzerland e-mail: [email protected], [thalmann;adam.amara]@phys.ethz.ch 3 Department of Physics and Astronomy, College of Charleston, Charleston, SC 29424 , USA e-mail: [email protected] 4 Department of Physics, University of Montreal, Montreal, QC H31T 1J4T, Canada e-mail: [email protected] Received 8 September 2014 / Accepted 13 December 2014 ABSTRACT Stars with debris disks are intriguing targets for direct-imaging exoplanet searches, owing both to previous detections of wide planets in debris disk systems, and to commonly existing morphological features in the disks themselves that may be indicative of a planetary inﬂuence. Here we present observations of three of the most nearby young stars, which are also known to host massive debris disks: Vega, Fomalhaut, and Eri. The Spitzer Space Telescope is used at a range of orientation angles for each star to supply a deep contrast through angular diﬀerential imaging combined with high-contrast algorithms. The observations provide the opportunity to probe substantially colder bound planets (120–330 K) than is possible with any other technique or instrument. For Vega, some apparently very red candidate point sources detected in the 4.5 μm image remain to be tested for common proper motion.
[Show full text]
Dynamics of Dust Particles Near Sun, Vega and Fomalhaut
Geophysical Research Abstracts Vol. 20, EGU2018-9532-1, 2018 EGU General Assembly 2018 © Author(s) 2018. CC Attribution 4.0 license. Dynamics of Dust Particles near Sun, Vega and Fomalhaut Johann Stamm (1), Carsten Baumann (1), Andrzej Czechowski (2), Ingrid Mann (1), and Margaretha Myrvang (1) (1) UiT The Arctic University of Norway, Institute for physics and Technology, Faculty of Science and Technology, Tromsø, Norway, (2) Polish Academy of Sciences, Space Research Center, Warsaw, Poland Several stars with debris disks show an unresolved excess emission at wavelengths shorter than 30 micrometer. It is believed that the excess emission origins from warm dust near the star. The dust is produced near the star and by collisions of planetesimals. When it is close to the star, it gets heated. In a similar way, the Sun is surrounded by hot dust of the inner planetary dust cloud. The orbits of the dust are influenced by gravitation, radiation pressure and also by the Lorentz force, since stellar wind impacts and photoionization by stellar photons charge the dust particles. The ratio of charge-to-mass (q/m) increases with decreasing dust grain radius, so that the Lorentz force is more important for the smaller dust sizes. The vicinity of the Sun will be explored with the ESA mission Solar Orbiter and these model calculations provide a basis for predicting the dust fluxes at the spacecraft. We consider here the dust trajectories around three stars: The Sun, Vega and Fomalhaut. The stellar mag- netic field is approximated as a Parker spiral in all cases. While the magnetic field strengths of the Sun and Vega are derived from observational data, the magnetic field strength of Fomalhaut is estimated.
[Show full text]
1 Hubblecast Episode 22: Hubble Directly Observes
ne Hubblecast Episode 22: Hubble directly observes planet orbiting Fomalhaut EMBARGOED UNTIL 20:30 (CET)/02:30 pm EST 13 Nov, 2008 00:00 Zoom into image of [Visual starts] Fomalhaut 00:00 [Narrator] The NASA/ESA Hubble Space Telescope has discovered an extrasolar planet, for the first time using direct visible-light Animated artist’s imaging. The strange world is far-flung from its parent star, is impression of the surrounded by a colossal belt of gas and dust, and may even planet, and gas / have rings more impressive than Saturn’s. dust 00:19 Introductory [Intro] graphics 00:35 [Woman] This is the Hubblecast! News and images from the NASA/ESA Hubble Space Telescope. EPISODE 22: Hubble Directly Travelling through time and space with our host Doctor J, Observes Planet a.k.a. Dr. Joe Liske. Orbiting Fomalhaut 00:47 Dr. J in virtual [Dr. J] studio, background Hello, and welcome to another episode of the Hubblecast. Our Hubble Fomalhaut favourite orbiting observatory has been busy helping system images astronomers to study extrasolar planets — those enigmatic worlds orbiting stars other than our Sun. And, what do you Name: Dr. J know, Hubble has done it again. It has delivered yet another Episode: Hubble stunning breakthrough when it turned its gaze on the star Directly Observes Fomalhaut. Planet Orbiting Fomalhaut Topic: Extrasolar Planets Vodcast No.: 2008/10 1 01:12 Panning image of [Narrator] night sky, circling / Fomalhaut is visible from the southern hemisphere, and is one labelling Fomalhaut of the brightest stars in our night sky. Lying around 25 light- years distant, it’s also relatively close.
[Show full text]
The Detectability of Nightside City Lights on Exoplanets
Draft version September 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The Detectability of Nightside City Lights on Exoplanets Thomas G. Beatty1 1Department of Astronomy and Steward Observatory, University of Arizona, Tucson, AZ 85721; [email protected] ABSTRACT Next-generation missions designed to detect biosignatures on exoplanets will also be capable of plac- ing constraints on the presence of technosignatures (evidence for technological life) on these same worlds. Here, I estimate the detectability of nightside city lights on habitable, Earth-like, exoplan- ets around nearby stars using direct-imaging observations from the proposed LUVOIR and HabEx observatories. I use data from the Soumi National Polar-orbiting Partnership satellite to determine the surface ﬂux from city lights at the top of Earth's atmosphere, and the spectra of commercially available high-power lamps to model the spectral energy distribution of the city lights. I consider how the detectability scales with urbanization fraction: from Earth's value of 0.05%, up to the limiting case of an ecumenopolis { or planet-wide city. I then calculate the minimum detectable urbanization fraction using 300 hours of observing time for generic Earth-analogs around stars within 8 pc of the Sun, and for nearby known potentially habitable planets. Though Earth itself would not be detectable by LUVOIR or HabEx, planets around M-dwarfs close to the Sun would show detectable signals from city lights for urbanization levels of 0.4% to 3%, while city lights on planets around nearby Sun-like stars would be detectable at urbanization levels of & 10%. The known planet Proxima b is a particu- larly compelling target for LUVOIR A observations, which would be able to detect city lights twelve times that of Earth in 300 hours, an urbanization level that is expected to occur on Earth around the mid-22nd-century.
[Show full text]
ASTR 300 Stars and Stellar Systems Spring 2011 Homeworksetno.3 Duemarch10,2011
ASTR 300 Stars and Stellar Systems Spring 2011 HomeworkSetNo.3 DueMarch10,2011 Please type up or print out your homework and staple the pages together. Leave a blank space to write in mathematical equations or diagrams. Make sure you show your work for any calculations – “magical” answers will receive no credit. Problems are due at the beginning of the lecture. Review questions, Problems, etc. which have a chapter and number noted are from your text Stars and Galaxies, 7th edition. 1. Why is it difﬁcult to ﬁnd out how common the most luminous stars are ? The least luminous stars ? (Chapt. 9, Review Question 13) 2. The parallax of the bright star Vega is 0.129 seconds of arc. What is the distance of Vega in parsecs ? In light-years ? By how much, during the year, does the position of Vega shift relative to distant background stars ? If an astronomer were observing from the surface of Jupiter’s moon Europa, by how much would Vega shift during the Jovian year ? (Hint: Jupiter is 5.2 AU from the sun.) 3. A binary star system contains one star of mass 0.8 M⊙ and another of mass 2.2 M⊙. They are in circular orbits and the distance between the centers of the stars is 1.5 AU. (a) What is the period P of the binary? (b) Find the location of the center of mass (i.e., how far is it from the center of the more massive star?). (c) Compare the gravitational force of the two stars on a small mass m located at the center of mass.
[Show full text]
The MESAS Project: Long Wavelength Follow-Up Observations of Sirius A
Draft version March 11, 2019 Typeset using LATEX twocolumn style in AASTeX62 The MESAS Project: Long wavelength follow-up observations of Sirius A Jacob Aaron White,1 J. Aufdenberg,2 A. C. Boley,3 M. Devlin,4 S. Dicker,4 P. Hauschildt,5 A. G. Hughes,3 A. M. Hughes,6 B. Mason,7 B. Matthews,8 A. Moor,´ 1 T. Mroczkowski,9 C. Romero,4 J. Sievers,10 S. Stanchfield,4 F. Tapia,11, 12 and D. Wilner13 1Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, Konkoly-Thege Miklósút 15-17, 1121 Budapest, Hungary 2Physical Sciences Department, Embry-Riddle Aeronautical University, 600 S Clyde Morris Blvd., Daytona Beach, FL 32114, USA 3Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Rd., Vancouver, BC V6T 1T7, Canada 4Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104, USA 5Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany 6Department of Astronomy, Van Vleck Observatory, Wesleyan University, 96 Foss Hill Dr., Middletown, CT 06459, USA 7National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA 8Herzberg Institute, National Research Council of Canada, 5071 W. Saanich Road, Victoria, BC V9E 2E7, Canada 9ESO-European Organization for Astronomical Research in the Southern hemisphere, Karl-Schwarzschild-Str. 2, D-85748 Garching b. Munchen, Germany 10McGill University, 3600 University Street, Montreal, QC H3A 2T8, Canada 11Posgrado en Ciencias de la Tierra, Universidad Nacional Autnoma de México, Morelia, 58190, México 12Escuela Nacional de Estudios Superiores Unidad Morelia, Universidad Nacional Autnoma de México, Morelia, 58190, México 13Center for Astrophysics | Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA (Received 02-15-2019; Revised 03-05-2019; Accepted 03-08-2019) Submitted to ApJ ABSTRACT Modeling the submillimeter to centimeter emission of stars is challenging due to a lack of sensitive observations at these long wavelengths.
[Show full text]
Capella - Betelgeuse - Canopus Vs
Capella - Betelgeuse - Canopus vs. Canopus - Achernar - Fomalhaut and also Vega and Acrux. Full post with detailed answers Aug 07th, 2016 Hello to all, In my recent Skywatcher Quizz post ( http://fer3.com/arc/m2.aspx/Skywatcher-Quizz-Couëtte-jul-2016- g35938) I wrote : " (10) To-morrow morning, I will admire the magnificent unique and only 1st Magnitude star line-up : CANOPUS - ACHERNAR - FOMALHAUT from East to West about one hour before Sun rise ". Well ... I was not entirely right then. You will learn why hereafter … ******* This morning when flying my A343 towards an easterly direction to land at Darwin (again !) in the last part of the night, and while we had to twist our necks to admire from the cockpit right windows our well known and now familiar Canopus - Achernar - Fomalhaut alignment (with this latter star being our neck twisting one) …… … I was amazed to "discover" a second remarkable 1st Magnitude Star alignment just in front of us - just over the horizon and surrounding the Darwin City lights glowing against a dark night contrast - as follows: On AUG 04th, 2016 by 18:50 UT, from a position around 100 NM West of Darwin, N.T. Australia (we were flying towards the East), and at FL140 I could see from left to right in our front windows CAPELLA - BETELGEUSE - CANOPUS *** above the horizon at respective heights not exceeding 20 degrees. This one is definitely a splendid alignment of bright Celestial Navigational Stars too, looking that it spans over a wider range than the other one. ******* Let us then take the opportunity to crunch a few numbers in the following drill: For each of the " Canopus - Achernar - Fomalhaut " and " Capella - Betelgeuse - Canopus " alignments: 1 - Compute the angular separation between its extreme stars (i.e.
[Show full text]