The Ephemeris Encyclopedia Galactica: Sector Nine (Tulmath Space)
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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 -
SEPTEMBER 2014 OT H E D Ebn V E R S E R V ESEPTEMBERR 2014
THE DENVER OBSERVER SEPTEMBER 2014 OT h e D eBn v e r S E R V ESEPTEMBERR 2014 FROM THE INSIDE LOOKING OUT Calendar Taken on July 25th in San Luis State Park near the Great Sand Dunes in Colorado, Jeff made this image of the Milky Way during an overnight camping stop on the way to Santa Fe, NM. It was taken with a Canon 2............................. First quarter moon 60D camera, an EFS 15-85 lens, using an iOptron SkyTracker. It is a single frame, with no stacking or dark/ 8.......................................... Full moon bias frames, at ISO 1600 for two minutes. Visible in this south-facing photograph is Sagittarius, and the 14............ Aldebaran 1.4˚ south of moon Dark Horse Nebula inside of the Milky Way. He processed the image in Adobe Lightroom. Image © Jeff Tropeano 15............................ Last quarter moon 22........................... Autumnal Equinox 24........................................ New moon Inside the Observer SEPTEMBER SKIES by Dennis Cochran ygnus the Swan dives onto center stage this other famous deep-sky object is the Veil Nebula, President’s Message....................... 2 C month, almost overhead. Leading the descent also known as the Cygnus Loop, a supernova rem- is the nose of the swan, the star known as nant so large that its separate arcs were known Society Directory.......................... 2 Albireo, a beautiful multi-colored double. One and named before it was found to be one wide Schedule of Events......................... 2 wonders if Albireo has any planets from which to wisp that came out of a single star. The Veil is see the pair up-close. -
Not Surprising That the Method Begins to Break Down at This Point
152 ASTRONOMY: W. S. ADAMS hanced lines in the early F stars are normally so prominent that it is not surprising that the method begins to break down at this point. To illustrate the use of the formulae and curves we may select as il- lustrations a few stars of different spectral types and magnitudes. These are collected in Table II. The classification is from Mount Wilson determinations. TABLE H ~A M PARAIuAX srTATYP_________________ (a) I(b) (C) (a) (b) c) Mean Comp. Ob. Pi 10U96.... 7.6F5 -0.7 +0.7 +3.0 +6.5 4.7 5.8 5.7 +0#04 +0.04 Sun........ GO -0.5 +0.5 +3.0 +5.6 4.3 5.8 5.2 Lal. 38287.. 7.2 G5 -1.8 +1.5 +3.5 +7.4 +6.3 +6.2 7.3 +0.10 +0.09 a Arietis... 2.2K0O +2.5 -2.4 +0.2 +1.0 1.3 +0.2 0.8 +0.05 +0.09 aTauri.... 1.1K5 +3.0 -2.0 +0.5 -0.4 +1.9 +0.5 0.7 +0.08 +0.07 61' Cygni...6.3K8 -1.8 +5.8 +7.7 +8.2 9.3 8.9 8.8 +0.32 +0.31 Groom. 34..8.2 Ma -2.2 +6.8 +9.2 +10.2 10.5 10.4 10.4 +0.28 +0.28 The parallaxes are computed from the absolute magnitudes by the formula, to which reference has already been made, 5 logr = M - m - 5. The results are given in the next to the last column of the table, and the measured parallaxes in the final column. -
55,550 BCE and the 23 Stars of Giza I Douglas 2019
55,550 BCE and the 23 Stars of Giza I Douglas 2019 55,550 BCE and the 23 Stars of Giza Ian Douglas, B.Sc [email protected] 30 June 2019 Version 1.0.0 DOI: https://doi.org/10.5281/zenodo.3263928 This work is licensed under the Creative Commons Attribution 4.0 International License. Abstract This is a companion paper to and reliant on “Diskerfery and the Alignment of the Four Main Giza Pyramids” (Douglas, 2019 [1]). Following the geometric alignments shown in that paper, we now present the astronomical design plan with 23 stars. There is a perfect alignment with three stars, very close alignment with others, and close alignment with other prominent stars in the area. We propose that this was done to provide a date for the construction of Giza. The alignment occurs at circa 55,550BCE. Keywords: Giza, pyramids, alignment, archaeoastronomy. Contents 1. Introduction 2. Methodology, notation and accuracy 3. Overview of existing stellar explanations 4. The Quadruple Points 5. The Big Dipper hint 6. The stellar alignment 7. Round 2 8. Comparative chronology 9. Discussion 1 55,550 BCE and the 23 Stars of Giza I Douglas 2019 10. Acknowledgements 11. Bibliography 1. Introduction “Man fears time, but time fears the pyramids.” Arab proverb “When you have eliminated all which is impossible, then whatever remains, however improbable, must be the truth.” Sherlock Holmes “There are no contradictions. If you find one, check your premises.” Ayn Rand, Atlas Shrugged “There are more things in heaven and earth, Horatio, Than are dreamt of in your philosophy.” Hamlet Dedicated to the memory of Galileo Galilei. -
55,500 BCE and the 23 Stars of Giza I Douglas 2019
55,500 BCE and the 23 Stars of Giza I Douglas 2019 55,500 BCE and the 23 Stars of Giza Ian Douglas, B.Sc [email protected] 3 December 2019 Version 1.1.0 DOI: https://doi.org/10.5281/zenodo.3263927 This work is licensed under the Creative Commons Attribution 4.0 International License. Please check via DOI for latest version on Zenodo, where there is proper version control. Abstract This is a companion paper to and reliant on “Diskerfery and the Alignment of the Four Main Giza Pyramids” (Douglas, 2019 [1]). Following the geometric alignments shown in that paper, we now present the astronomical design plan with 23 stars. There is a perfect alignment with two stars, very close alignment with others, and close alignment with other prominent stars in the area. We propose that this was done to provide a date for the construction of Giza. The alignment occurs at circa 55,500BCE. Keywords: Giza, pyramids, alignment, archaeoastronomy. Contents 1. Introduction 2. Methodology, notation and accuracy 3. Overview of existing stellar explanations 4. The Quadruple Points 5. The Big Dipper hint 6. The stellar alignment 7. Rounds 2 and 3 8. Comparative chronology 9. Discussion 1 55,500 BCE and the 23 Stars of Giza I Douglas 2019 10. Acknowledgements 11. Bibliography Changes: 1.0.2 22 July 2019: Added date from Scott Creighton [2]. 1.04 Aug/Sep: round 3, comment about Khafre 3-4-5 design. Added dates from and comments about The Treatise on the Egyptian Pyramids. Not published. 1.1.0 November/December 2019: Major update. -
Annual Report / Rapport Annuel / Jahresbericht 1996
Annual Report / Rapport annuel / Jahresbericht 1996 ✦ ✦ ✦ E U R O P E A N S O U T H E R N O B S E R V A T O R Y ES O✦ 99 COVER COUVERTURE UMSCHLAG Beta Pictoris, as observed in scattered light Beta Pictoris, observée en lumière diffusée Beta Pictoris, im Streulicht bei 1,25 µm (J- at 1.25 microns (J band) with the ESO à 1,25 microns (bande J) avec le système Band) beobachtet mit dem adaptiven opti- ADONIS adaptive optics system at the 3.6-m d’optique adaptative de l’ESO, ADONIS, au schen System ADONIS am ESO-3,6-m-Tele- telescope and the Observatoire de Grenoble télescope de 3,60 m et le coronographe de skop und dem Koronographen des Obser- coronograph. l’observatoire de Grenoble. vatoriums von Grenoble. The combination of high angular resolution La combinaison de haute résolution angu- Die Kombination von hoher Winkelauflö- (0.12 arcsec) and high dynamical range laire (0,12 arcsec) et de gamme dynamique sung (0,12 Bogensekunden) und hohem dy- (105) allows to image the disk to only 24 AU élevée (105) permet de reproduire le disque namischen Bereich (105) erlaubt es, die from the star. Inside 50 AU, the main plane jusqu’à seulement 24 UA de l’étoile. A Scheibe bis zu einem Abstand von nur 24 AE of the disk is inclined with respect to the l’intérieur de 50 UA, le plan principal du vom Stern abzubilden. Innerhalb von 50 AE outer part. Observers: J.-L. Beuzit, A.-M. -
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. -
Thursday, December 22Nd Swap Meet & Potluck Get-Together Next First
Io – December 2011 p.1 IO - December 2011 Issue 2011-12 PO Box 7264 Eugene Astronomical Society Annual Club Dues $25 Springfield, OR 97475 President: Sam Pitts - 688-7330 www.eugeneastro.org Secretary: Jerry Oltion - 343-4758 Additional Board members: EAS is a proud member of: Jacob Strandlien, Tony Dandurand, John Loper. Next Meeting: Thursday, December 22nd Swap Meet & Potluck Get-Together Our December meeting will be a chance to visit and share a potluck dinner with fellow amateur astronomers, plus swap extra gear for new and exciting equipment from somebody else’s stash. Bring some food to share and any astronomy gear you’d like to sell, trade, or give away. We will have on hand some of the gear that was donated to the club this summer, including mirrors, lenses, blanks, telescope parts, and even entire telescopes. Come check out the bargains and visit with your fellow amateur astronomers in a relaxed evening before Christmas. We also encourage people to bring any new gear or projects they would like to show the rest of the club. The meeting is at 7:00 on December 22nd at EWEB’s Community Room, 500 E. 4th in Eugene. Next First Quarter Fridays: December 2nd and 30th Our November star party was clouded out, along with a good deal of the month afterward. If that sounds familiar, that’s because it is: I changed the date in the previous sentence from October to November and left the rest of the sentence intact. Yes, our autumn weather is predictable. Here’s hoping for a lucky break in the weather for our two December star parties. -
3-D Starmap 15.0 All Stars Within 15 Parsecs (50 Light-Years) of Sol
3-D Starmap 15.0 All stars within 15 parsecs (50 light-years) of Sol. Gl 815 2.0:14.9:-1.0 All units are in parsecs. (1 parsec = 3.26 light-years) 1.5 Gl 792 Stars are plotted in cartesian x,y,z coordinates. 3.2:14.7:-0.2 X-Y plane is the plane of the galaxy. Alderamin 2.3 -2.8:14.5:2.4 +x is Coreward, -x is Rimward, NN 4276 -3.9:14.4:0.4 +y is Spinward, -y is Trailing 1.2 Star data is from HYG database. 3.2 Stars circled in green are likely to host 14.0 human-habitable planets, according to 3 Eta Cephei 1.3 -1.9:13.9:2.9 the HabCat database. Gray lines link each star with its two closest neighbors. 2.9 3.0 Green lines link habitable stars with their two Hip 101516 5.7:13.5:-2.3 closest habitable neighbors. NN 4338 B GJ 1228 -4.1:13.4:-4.8 3.0 1.5:13.4:6.2 Gl 878 2.6 GJ 1270 0.4 Links are labeled with their distance in parsecs. -4.6:13.3:0.3 -1.5:13.3:-3.3 3.1 2.6 Gl 794 NN 4109 Winchell Chung: Nyrath the nearly wise 5.5:13.1:-2.3 2.0 7.0:13.1:1.5 http://www.projectrho.com/starmap.html 13.0 Gl 738 2.3 6.5:13.0:3.4 Gl 875.1 1.9 -1.2:12.9:-5.9 2.2 1.5 1.6 2.2 2.7 NN 4073 4.6:12.6:4.5 Gl 14 -6.1:12.5:-5.5 Gl 52 2.6 Gl 806 -28..6:12.4:0.3 1.3:12.4:0.2 4.4 3.8 NN 3069 BD+27°4120 2.6 Gl 813 BD+31°3767 -8.5:12.3:-2.3 2.4:12.3:-4.1 4.9:12.3:-3.55.1:12.3:0.8 BD+57°2735 -4.8:12.2:-0.7 19 Draconis -1.2:12.1:9.0 1.7 12.0 2.1 1.3 Gl 742 26 Draconis NN 4228 3.0 -2.4:11.9:5.6 -0.2:11.9:7.6 4.3:11.6.9:-7.4 1.1 2.5 3.8 1.7 2.4 1.9 35 Gamma Cephei GJ 1243 2.1 2.9 -6.4:11.6:3.6 1.9:11.6:2.1 NN 3117 2.3 NN 4040 2.8 -9.5:11.5:0.6 1.9 2.1 4.1 3.4:11.5:6.4 -
Estimation of the Masses of Selected Stars of Pulkovo Program by Means
Research in Astronomy and Astrophysics manuscript no. (LATEX: ShakhtGorshanov.tex; printed on July 17, 2018; 19:47) Estimation of the masses of selected stars of Pulkovo program by means of astrometry methods. N.A.Shakht1, D.L.Gorshanov1 and O.O.Vasilkova1 Central (Pulkovo) Astronomical Observatory of Russian Academy of Sciences, St-Petersburg,Russia; [email protected] Abstract Stars of Pulkovo observatory program are observed on 65-cm refractor during many years for study their positions and movement. We represent example of two visual bi- nary stars, for which orbits and masses of components were determined, and two astrometric stars, for which masses of their unseen companions have been estimated. The first stars are: ADS 14636 (61 Cygni) and ADS 7251 and others are: Gliese 623 and ADS 8035 (Alpha UMa). The direct astrometric methods were used for estimation of mass-ratio and masses. Key words: stellar masses, orbits, binaries individual: 61 Cygni, Alpha UMa, Gliese 623, ADS 7251 1 INTRODUCTION The mass of the star is one of its most important characteristics. Amount of matter in a star determines its temperature and pressure in the center, and also determines other characteristics of the star and then its evolutionary path. Direct estimates of the mass of the star are made on the basis of the law of universal arXiv:1802.04044v1 [astro-ph.SR] 12 Feb 2018 gravitation.The study of binary stars has allowed to establish the unity of Newton’s laws in the Universe and to obtain the fundamental knowledge about the masses of stars on the basis of observations. -
Download This Issue (Pdf)
Volume 46 Number 1 JAAVSO 2018 The Journal of the American Association of Variable Star Observers Optical Flares and Quasi-Periodic Pulsations on CR Draconis during Periastron Passage Upper panel: 2017-10-10-flare photon counts, time aligned with FFT spectrogram. Lower panel: FFT spectrogram shows time in UT seconds versus QPP periods in seconds. Flares cited by Doyle et al. (2018) are shown with (*). Also in this issue... • The Dwarf Nova SY Cancri and its Environs • KIC 8462852: Maria Mitchell Observatory Photographic Photometry 1922 to 1991 • Visual Times of Maxima for Short Period Pulsating Stars III • Recent Maxima of 86 Short Period Pulsating Stars Complete table of contents inside... The American Association of Variable Star Observers 49 Bay State Road, Cambridge, MA 02138, USA The Journal of the American Association of Variable Star Observers Editor John R. Percy Kosmas Gazeas Kristine Larsen Dunlap Institute of Astronomy University of Athens Department of Geological Sciences, and Astrophysics Athens, Greece Central Connecticut State University, and University of Toronto New Britain, Connecticut Toronto, Ontario, Canada Edward F. Guinan Villanova University Vanessa McBride Associate Editor Villanova, Pennsylvania IAU Office of Astronomy for Development; Elizabeth O. Waagen South African Astronomical Observatory; John B. Hearnshaw and University of Cape Town, South Africa Production Editor University of Canterbury Michael Saladyga Christchurch, New Zealand Ulisse Munari INAF/Astronomical Observatory Laszlo L. Kiss of Padua Editorial Board Konkoly Observatory Asiago, Italy Geoffrey C. Clayton Budapest, Hungary Louisiana State University Nikolaus Vogt Baton Rouge, Louisiana Katrien Kolenberg Universidad de Valparaiso Universities of Antwerp Valparaiso, Chile Zhibin Dai and of Leuven, Belgium Yunnan Observatories and Harvard-Smithsonian Center David B. -
Extra-Solar Planets 2
REVIEW ARTICLE Extra-solar planets M A C Perryman Astrophysics Division, European Space Agency, ESTEC, Noordwijk 2200AG, The Netherlands; and Leiden Observatory, University of Leiden, The Netherlands Abstract. The discovery of the first extra-solar planet surrounding a main-sequence star was announced in 1995, based on very precise radial velocity (Doppler) measurements. A total of 34 such planets were known by the end of March 2000, and their numbers are growing steadily. The newly-discovered systems confirm some of the features predicted by standard theories of star and planet formation, but systems with massive planets having very small orbital radii and large eccentricities are common and were generally unexpected. Other techniques being used to search for planetary signatures include accurate measurement of positional (astrometric) displacements, gravitational microlensing, and pulsar timing, the latter resulting in the detection of the first planetary mass bodies beyond our Solar System in 1992. The transit of a planet across the face of the host star provides significant physical diagnostics, and the first such detection was announced in 1999. Protoplanetary disks, which represent an important evolutionary stage for understanding planet formation, are being imaged from space. In contrast, direct imaging of extra-solar planets represents an enormous challenge. Long-term efforts are directed towards infrared space interferometry, the detection of Earth-mass planets, and measurement of their spectral characteristics. Theoretical atmospheric models provide predictions of planetary temperatures, radii, albedos, chemical condensates, and spectral features as a function of mass, composition and distance from the host star. Efforts to characterise planets occupying the ‘habitable zone’, in which liquid water may be present, and indicators of the arXiv:astro-ph/0005602v1 31 May 2000 presence of life, are advancing quantitatively.