Revista Macrocosmo.Com ISSN 1808-0731 Ano II - Edição Nº 22 - Setembro De 2005
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Astronomie in Theorie Und Praxis 8. Auflage in Zwei Bänden Erik Wischnewski
Astronomie in Theorie und Praxis 8. Auflage in zwei Bänden Erik Wischnewski Inhaltsverzeichnis 1 Beobachtungen mit bloßem Auge 37 Motivation 37 Hilfsmittel 38 Drehbare Sternkarte Bücher und Atlanten Kataloge Planetariumssoftware Elektronischer Almanach Sternkarten 39 2 Atmosphäre der Erde 49 Aufbau 49 Atmosphärische Fenster 51 Warum der Himmel blau ist? 52 Extinktion 52 Extinktionsgleichung Photometrie Refraktion 55 Szintillationsrauschen 56 Angaben zur Beobachtung 57 Durchsicht Himmelshelligkeit Luftunruhe Beispiel einer Notiz Taupunkt 59 Solar-terrestrische Beziehungen 60 Klassifizierung der Flares Korrelation zur Fleckenrelativzahl Luftleuchten 62 Polarlichter 63 Nachtleuchtende Wolken 64 Haloerscheinungen 67 Formen Häufigkeit Beobachtung Photographie Grüner Strahl 69 Zodiakallicht 71 Dämmerung 72 Definition Purpurlicht Gegendämmerung Venusgürtel Erdschattenbogen 3 Optische Teleskope 75 Fernrohrtypen 76 Refraktoren Reflektoren Fokus Optische Fehler 82 Farbfehler Kugelgestaltsfehler Bildfeldwölbung Koma Astigmatismus Verzeichnung Bildverzerrungen Helligkeitsinhomogenität Objektive 86 Linsenobjektive Spiegelobjektive Vergütung Optische Qualitätsprüfung RC-Wert RGB-Chromasietest Okulare 97 Zusatzoptiken 100 Barlow-Linse Shapley-Linse Flattener Spezialokulare Spektroskopie Herschel-Prisma Fabry-Pérot-Interferometer Vergrößerung 103 Welche Vergrößerung ist die Beste? Blickfeld 105 Lichtstärke 106 Kontrast Dämmerungszahl Auflösungsvermögen 108 Strehl-Zahl Luftunruhe (Seeing) 112 Tubusseeing Kuppelseeing Gebäudeseeing Montierungen 113 Nachführfehler -
Extrasolar Planets
Extrasolar Planets to appear in Encyclopedia of Time, Sage Publishing, in preparation, H.J. Birx (Ed.) The term extrasolar planets or exoplanets stands for planets outside our Solar System, i.e. not orbiting the Sun, but other stars. Planets in our Solar System are defined as objects with enough mass to be spherical and round by their own gravity and to be alone on their orbit around the Sun, i.e. to be the dominant object in a particular orbit, and not to be a moon or asteroid (see the entry Planet in this encyclopedia for the official definition, the historical debate, and a discussion of the planets of our Solar System). Most exoplanets are discovered by observing the stellar motion around the common center of mass of the star+planet system, i.e. by observing somehow the motion of the objects in orbit around each other, i.e. by measuring precisely the periodic variation of certain values, e.g. radial velocity or brightness, with time, e.g. the first extrasolar planets were found with the timing technique around a pulsating neutron star. The recent definition of Planets of our Solar System by the International Astronomical Union deals mainly with the question of the minimum mass for an object to qualify as planet and excludes Pluto. This matter was raised by the fact that more and more objects similar to Pluto were discovered by larger and larger telescopes. The questions of maximum mass and formation of planets were left out in this new definition, possibly partly because there is not yet a consensus in the international community. -
The Slow Spin of the Young Sub-Stellar Companion GQ Lupi B and Its Orbital Configuration Henriette Schwarz1?, Christian Ginski1, Remco J
Astronomy & Astrophysics manuscript no. AA-2016-28908-preprint c ESO 2016 July 4, 2016 The slow spin of the young sub-stellar companion GQ Lupi b and its orbital configuration Henriette Schwarz1?, Christian Ginski1, Remco J. de Kok1; 2, Ignas A. G. Snellen1, Matteo Brogi3; 5, and Jayne L. Birkby4; 6 1 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands 2 SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands 3 Center for Astrophysics and Space Astronomy, University of Colorado at Boulder, CO 80309 Boulder, USA 4 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MA 02138 Cambridge, USA 5 NASA Hubble Fellow 6 NASA Sagan Fellow ABSTRACT The spin of a planet or brown dwarf is related to the accretion process, and therefore studying spin can help promote our understand- ing of the formation of such objects. We present the projected rotational velocity of the young sub-stellar companion GQ Lupi b, along with its barycentric radial velocity. The directly imaged exoplanet or brown dwarf companion joins a small but growing en- semble of wide-orbit sub-stellar companions with a spin measurement. The GQ Lupi system was observed at high spectral resolution (R ∼100 000), and in the analysis we made use of both spectral and spatial filtering to separate the signal of the companion from that of the host star. We detect both CO (S/N=11.6) and H2O (S/N=7.7) in the atmosphere of GQ Lupi b by cross-correlating with model +0:9 −1 spectra, and we find it to be a slow rotator with a projected rotational velocity of 5:3−1:0 km s . -
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. -
An Upper Limit on the Mass of the Circumplanetary Disk for DH Tau B
Draft version August 28, 2021 Preprint typeset using LATEX style emulateapj v. 12/16/11 AN UPPER LIMIT ON THE MASS OF THE CIRCUM-PLANETARY DISK FOR DH TAU B* Schuyler G. Wolff1, Franc¸ois Menard´ 2, Claudio Caceres3, Charlene Lefevre` 4, Mickael Bonnefoy2,Hector´ Canovas´ 5,Sebastien´ Maret2, Christophe Pinte2, Matthias R. Schreiber6, and Gerrit van der Plas2 Draft version August 28, 2021 ABSTRACT DH Tau is a young (∼1 Myr) classical T Tauri star. It is one of the few young PMS stars known to be associated with a planetary mass companion, DH Tau b, orbiting at large separation and detected by direct imaging. DH Tau b is thought to be accreting based on copious Hα emission and exhibits variable Paschen Beta emission. NOEMA observations at 230 GHz allow us to place constraints on the disk dust mass for both DH Tau b and the primary in a regime where the disks will appear optically thin. We estimate a disk dust mass for the primary, DH Tau A of 17:2 ± 1:7 M⊕, which gives a disk- to-star mass ratio of 0.014 (assuming the usual Gas-to-Dust mass ratio of 100 in the disk). We find a conservative disk dust mass upper limit of 0.42M⊕ for DH Tau b, assuming that the disk temperature is dominated by irradiation from DH Tau b itself. Given the environment of the circumplanetary disk, variable illumination from the primary or the equilibrium temperature of the surrounding cloud would lead to even lower disk mass estimates. A MCFOST radiative transfer model including heating of the circumplanetary disk by DH Tau b and DH Tau A suggests that a mass averaged disk temperature of 22 K is more realistic, resulting in a dust disk mass upper limit of 0.09M⊕ for DH Tau b. -
September 2020 BRAS Newsletter
A Neowise Comet 2020, photo by Ralf Rohner of Skypointer Photography Monthly Meeting September 14th at 7:00 PM, via Jitsi (Monthly meetings are on 2nd Mondays at Highland Road Park Observatory, temporarily during quarantine at meet.jit.si/BRASMeets). GUEST SPEAKER: NASA Michoud Assembly Facility Director, Robert Champion What's In This Issue? President’s Message Secretary's Summary Business Meeting Minutes Outreach Report Asteroid and Comet News Light Pollution Committee Report Globe at Night Member’s Corner –My Quest For A Dark Place, by Chris Carlton Astro-Photos by BRAS Members Messages from the HRPO REMOTE DISCUSSION Solar Viewing Plus Night Mercurian Elongation Spooky Sensation Great Martian Opposition Observing Notes: Aquila – The Eagle Like this newsletter? See PAST ISSUES online back to 2009 Visit us on Facebook – Baton Rouge Astronomical Society Baton Rouge Astronomical Society Newsletter, Night Visions Page 2 of 27 September 2020 President’s Message Welcome to September. You may have noticed that this newsletter is showing up a little bit later than usual, and it’s for good reason: release of the newsletter will now happen after the monthly business meeting so that we can have a chance to keep everybody up to date on the latest information. Sometimes, this will mean the newsletter shows up a couple of days late. But, the upshot is that you’ll now be able to see what we discussed at the recent business meeting and have time to digest it before our general meeting in case you want to give some feedback. Now that we’re on the new format, business meetings (and the oft neglected Light Pollution Committee Meeting), are going to start being open to all members of the club again by simply joining up in the respective chat rooms the Wednesday before the first Monday of the month—which I encourage people to do, especially if you have some ideas you want to see the club put into action. -
Planets and Exoplanets
NASE Publications Planets and exoplanets Planets and exoplanets Rosa M. Ros, Hans Deeg International Astronomical Union, Technical University of Catalonia (Spain), Instituto de Astrofísica de Canarias and University of La Laguna (Spain) Summary This workshop provides a series of activities to compare the many observed properties (such as size, distances, orbital speeds and escape velocities) of the planets in our Solar System. Each section provides context to various planetary data tables by providing demonstrations or calculations to contrast the properties of the planets, giving the students a concrete sense for what the data mean. At present, several methods are used to find exoplanets, more or less indirectly. It has been possible to detect nearly 4000 planets, and about 500 systems with multiple planets. Objetives - Understand what the numerical values in the Solar Sytem summary data table mean. - Understand the main characteristics of extrasolar planetary systems by comparing their properties to the orbital system of Jupiter and its Galilean satellites. The Solar System By creating scale models of the Solar System, the students will compare the different planetary parameters. To perform these activities, we will use the data in Table 1. Planets Diameter (km) Distance to Sun (km) Sun 1 392 000 Mercury 4 878 57.9 106 Venus 12 180 108.3 106 Earth 12 756 149.7 106 Marte 6 760 228.1 106 Jupiter 142 800 778.7 106 Saturn 120 000 1 430.1 106 Uranus 50 000 2 876.5 106 Neptune 49 000 4 506.6 106 Table 1: Data of the Solar System bodies In all cases, the main goal of the model is to make the data understandable. -
Observer “Build a Safe Solar Filter”, by John Land 4
INSIDE THIS ISSUE: ASTRONOMY CLUB OF TULSA CALENDAR AND EVENTS 2 GREAT ECLIPSE AND SOLAR FILTERS, BY JOHN LAND 3 OBSERVER “BUILD A SAFE SOLAR FILTER”, BY JOHN LAND 4 ASTRONOMY CONVENTIONS FOR 2017, APRIL 2017 BY JOHN LAND 5 MESSIER MARATHON AND CARAVAN INFO, BY TAMARA GREEN 6 PRESIDENT’S MESSAGE 8 TREASURER’S AND MEMBERSHIP REPORT 9 NASA’S “THE SPACE PLACE” NEWSLETTER 10 “ WHAT IT’S LIKE ON A TRAPPIST-1 PLANET”, BY MARCUS WOO 12 WHERE WE MEET 14 OFFICERS, BOARD & STAFF 15 PERMISION TO REPRINT ANYTHING FROM THIS NEWSLETTER IS GRANTED, PROVIDED THAT CREDIT IS GIVEN TO THE ORIGINAL AUTHOR AND THAT THE ASTRONOMY CLUB OF TULSA “OBSERVER” IS LISTED AS THE ORIGINAL SOURCE. FOR ORIGINAL CONTENT CREDITED TO OTHERS AND SO NOTED IN THIS PUBLICATION, YOU SHOULD OBTAIN PERMISSION FROM THAT RESPECTIVE SOURCE PRIOR TO REPRINTING. THANK YOU VERY MUCH FOR YOUR COOPERATION. PLEASE ENJOY THIS EDITION OF THE OBSERVER. THE ASTRONOMY CLUB TULSA IS A PROUD MEMBER OF PHOTOS: TOP: Saying “So Long” to our Winter stars; BOTTOM: Saying “Hello Again!” to our Spring and Summer Stars. Both photos taken at the ACT Observatory April 2016 by Tamara Green. THE ASTRONOMICAL LEAGUE APRIL 2017 SUN MON TUE WED THU FRI SAT MOON PHASES AND HOLIDAYS: 1 2 3 4 5 6 7 8 APRIL FOOLS’ DAY SAT APR 1 FIRST QUARTER MON APR 3 9 10 11 12 13 14 15 FULL MOON TUES APR 11 GOOD FRIDAY FRI APR 14 16 17 18 19 20 21 22 EASTER SUNDAY SUN APR 16 23 24 25 26 27 28 29 LAST QUARTER WED APR 19 EARTH DAY SAT APR 22 30 NEW MOON WED APR 26 UPCOMING EVENTS: SIDEWALK ASTRONOMY SAT APR 8 7:30 PM BASS PRO GENERAL MEETING FRI APR 14 7:00 PM JENKS HS PLANETARIUM PUBLIC STAR PARTY SAT APR 15 7:30 PM ACT OBSERVATORY MEMBERS’ NIGHT** FRI APR 21 8:00 PM ACT OBSERVATORY MESSIER MARATHON** SAT APR 22 3:00 PM (CARAVAN) TUVA GENERAL MEETING FRI MAY 5 7:00 PM JENKS HS PLANETARIUM SIDEWALK ASTRONOMY SAT MAY 6 7:30 PM BASS PRO PUBLIC STAR PARTY SAT MAY 20 8:00 PM ACT OBSERVATORY MEMBERS’ NIGHT** FRI MAY 26 8:15 PM ACT OBSERVATORY **MEMBERS AND FAMILY ONLY PLEASE. -
RASNZ Occultation Section Circular CN2009/1 April 2013 NOTICES
ISSN 11765038 (Print) RASNZ ISSN 23241853 (Online) OCCULTATION CIRCULAR CN2009/1 April 2013 SECTION Lunar limb Profile produced by Dave Herald's Occult program showing 63 events for the lunar graze of a bright, multiple star ZC2349 (aka Al Niyat, sigma Scorpi) on 31 July 2009 by two teams of observers from Wellington and Christchurch. The lunar profile is drawn using data from the Kaguya lunar surveyor, which became available after this event. The path the star followed across the lunar landscape is shown for one set of observers (Murray Forbes and Frank Andrews) by the trail of white circles. There are several instances where a stepped event was seen, due to the two brightest components disappearing or reappearing. See page 61 for more details. Visit the Occultation Section website at http://www.occultations.org.nz/ Newsletter of the Occultation Section of the Royal Astronomical Society of New Zealand Table of Contents From the Director.............................................................................................................................. 2 Notices................................................................................................................................................. 3 Seventh TransTasman Symposium on Occultations............................................................3 Important Notice re Report File Naming...............................................................................4 Observing Occultations using Video: A Beginner's Guide.................................................. -
1949 Handbook of the British Astronomical Association
THE HANDBOOK OF THE BRITISH ASTRONOMICAL ASSOCIATION 1 9 4 9 1948 NOVEMBER Price to Members 3s. N on Members 5s. CONTENTS Preface ... ... ... ... ... ... ... 1 Planetary Diagram ... ... ... ' ... 2 V i s i b i l i t y o f P l a n e t s ....................................................................... ........................................................................ 3 Tim e Reckoning .........................! ............................ ........................................................................ 4 S u n , 1 9 4 9 ............................................................................................................................................................... 5 Eclipses, 1949 .................................................................... .. ............................_ .................................. 8 M o o n , 1 9 4 9 . ....................................................................... ............................ 9 L i b r a t i o n ............................................................................................. .................................................. 1 0 O b s e r v a t i o n o f O c c u l t a t i o n s . .................................................................................................................... 1 0 L unar O ccultations, 1949 ........................... .................................................. 1 2 A p p e a r a n c e o f P l a n e t s ................................................................... .................................................................... -
A Study of Asteroid Pole-Latitude Distribution Based on an Extended
Astronomy & Astrophysics manuscript no. aa˙2009 c ESO 2018 August 22, 2018 A study of asteroid pole-latitude distribution based on an extended set of shape models derived by the lightcurve inversion method 1 1 1 2 3 4 5 6 7 J. Hanuˇs ∗, J. Durechˇ , M. Broˇz , B. D. Warner , F. Pilcher , R. Stephens , J. Oey , L. Bernasconi , S. Casulli , R. Behrend8, D. Polishook9, T. Henych10, M. Lehk´y11, F. Yoshida12, and T. Ito12 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holeˇsoviˇck´ach 2, 18000 Prague, Czech Republic ∗e-mail: [email protected] 2 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 3 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 4 Goat Mountain Astronomical Research Station, 11355 Mount Johnson Court, Rancho Cucamonga, CA 91737, USA 5 Kingsgrove, NSW, Australia 6 Observatoire des Engarouines, 84570 Mallemort-du-Comtat, France 7 Via M. Rosa, 1, 00012 Colleverde di Guidonia, Rome, Italy 8 Geneva Observatory, CH-1290 Sauverny, Switzerland 9 Benoziyo Center for Astrophysics, The Weizmann Institute of Science, Rehovot 76100, Israel 10 Astronomical Institute, Academy of Sciences of the Czech Republic, Friova 1, CZ-25165 Ondejov, Czech Republic 11 Severni 765, CZ-50003 Hradec Kralove, Czech republic 12 National Astronomical Observatory, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan Received 17-02-2011 / Accepted 13-04-2011 ABSTRACT Context. In the past decade, more than one hundred asteroid models were derived using the lightcurve inversion method. Measured by the number of derived models, lightcurve inversion has become the leading method for asteroid shape determination. -
APRIL 2017 OBSERVER ** See “ASTRO NEWS,” Page 4, for Full Details on This Story
The Denver APRIL 2017 OBSERVER ** See “ASTRO NEWS,” Page 4, for full details on this story. Overview of the Trappist-1 system (center), with comparisons to the size of Jupiter and the orbits of its Galilean moons (top), and to our inner solar system (bottom). The planets in the respective solar systems are not drawn to the same scale as their orbits, but they are all in proportion to each other. Image credit: NASA/JPL-Caltech APRIL SKIES by Zachary Singer The Solar System Sky Calendar April starts off with Mercury at maximum 3 First-Quarter Moon elongation (its widest angle from the Sun as 11 Full Moon seen from Earth). On that April 1st morning, the 19 Last-Quarter Moon planet will be about 40% illuminated and more 26 New Moon than 10° above the western horizon 40 minutes after sunset; Mercury’s disk will be 8” across. Over the following week, as the planet sweeps In the Observer quickly toward its line-up (“inferior conjunc- tion”) with the Sun, its disk grows to about 9” Venus, on the evening of March 23, 2017. In early April, the planet will display a similar appearance President’s Message . 2 and its phase shrinks into a crescent. Soon after in pre-dawn skies. Image © Ron Pearson. that, Mercury’s increasingly slimmer (and dim- Society Directory. 2 mer) crescent becomes lost in the solar glare; tion from the Sun and distance from us, the disk Schedule of Events . 2 inferior conjunction is on the 20th. shrinks but the crescent thickens, so the overall By the 1st, Venus has swung out of the Sun’s brightness increases to -4.5! (If, instead of get- DAS News .