Double Star Observations Made at the Lick Observatory in May, June and July 1889

Total Page:16

File Type:pdf, Size:1020Kb

Double Star Observations Made at the Lick Observatory in May, June and July 1889 ASTRONOMISCHE NACHRICHTEN. NZ 2956-57. Double Star Observations made at the Lick Observatory in May, June and July 1889. By 5. w.BUl.lZhlZ7iZ. The following double star observations have been made since the preparation of the last preceding list (A. N. 2929-30), and principally in the months of May, June and July of the present year. Since that time the large telescope has been used the greater part of the time for other work. During the period mentioned, 62 new pairs have been discovered and measured; and measures made of 98 of the more interesting and difficult pairs from former catalogues; altogether comprising 628 separate measures. This work has been done with the 36inch equatorial with the exception of the measures of a few southern stars which could be more conveniently made with the smaller telescope. The present catalogue of new stars is the sixteenth in order of publication. These lists have appeared as follows : First Catalogue Nos. I to 81 Monthl. Not. March 1873 Ninth Catalogue Nos. 453 to 482 Monthl. Not. Dec. 1877 Second 8 > 82 L: 106 8 May 1873 Tenth )) )) 483 D 733 Memoirs R.bS Vol. 44 Third D D 107 m 182 > Dec. 1873 ~ Eleventh % B 734 B 775 Lick Obs. Publ. I Fourth D P 183 r 229 D June 1874 Twelfth B B 776 * 863 Washb. Obs. Publ. I Fifth )) P 230 D 300 D Nov. 1874 Thirteenth 3 B 864 a 1025 Memoirs R.A.S. VoI. 47 Sixth n )) 301 P 390 Astr. Nachr. No. 2062 Fourteenth B 1026 D 1038 Astr. Nachr. No. 2875 Sevenrh P P 391 m 436 D 2103 Fifteenth Y D 1039 P 1092 b a 2929-30 Eighth )) 3 437 P 452 hmer.;ourn. of Sc. J~ly1877 I Sixteenth 2 )) 1093 L) I 154 The present Catalogue, The places of the stars are given, as heretofore, for 1880. The instrument used in each observation is given .in the last column. New Double Stars. (Sixteenth Catalogue.) fl 1093. Lal. 375. p 1096. AOe. 534. R.4. oh I 4m43s Decl. + I ooI 9'. RA. 0~29~46~Decl. +57O51' 1889.630 i 55?8 , 0137 ~ 7 , 8 I 36 A and B. .633 57.8 I 0.42 7.5, 8 36 1889.594 2b5?2 .687 1 49.2 0.39 j 7.51 8.5 36 ' I .67 I 267.9 1889.65 543 039 7.3, 8.2 I I I I ,673 269.9 The following of three bright stars. /3 1094. Lal. 655. RA. oh 23ll13sS Decl. +59" 19'. 1889.526 ~ 242.8 0.60 5 , 9 36 .534 , 244.3 j 0.81 ~ 6 , 9.5 36 .537 I 246.6 0.70 i, 6 , 10 36 .~ .- 1097. Radcl. 159. 1889.53 j 244.6 0.70 I 5.7 , 9.5 RA. oh 3on13oS Decl. +57" 21'. .. 1095. 28 Andromedae. 1889.594 72.1 RA. oh ~3~47~Decl. +29O 5'. a597 69.9 .608 7 1.5 1889.509 0.4 2.37 , 8 '3 36 j 5-5 ; .61 I 7 2.8 .512 0.1 1 2.33 5.5, 14 : 36 -___. I 889.60 .5'5 1 359.7 __I 2.55 j 5.5, 13 1 36 71.6 O.57 I 8*4~8.4 I 1889.51 I 0.1 1 2.42 1 5.5 , 13.3 I The magnitude in Radcl. is 7.4, and in DM. 7.0. (Bd. 124, 4 2956 52 A and BC. I 889.583 265?3 60:'30 8.5, - I2 .58h 265.4 60.26 8.5, - 36 7889.594 I 7504 1 l2!'77 I 5 13.5 36 I 265.6 60.3 I I .608 i 12.61 6 13.5 36 _____.589 8.5 - I 36 ,611 I ;;.: 1 12.99 1 6 13.5 36 1889.58 265.4 60.29 8.5, - I The principal star is Radcl. 430, and is 1~41~f. d Cassiopeiae, and 2'58" n. @ I 103. 44 Cassiopeiae. RA. 1~35~12'Decl. +59" 56'. 1.63 1 6.5, 12.5 I 36 1.81 j 6 , 13.5 1 36 p 1104. Groombridge 370. RA. 1~35~~51'Decl. +52"17'. p I 100. Lal, 21 55. RA. I 7"sS Decl. 4-60" r 8'. 1889.589 1 199.1 .6x1 I 195.2 1889.526 1 45.3 I '0.5' I 7.5 t 7.5 ! 36 ,616I 197.4 0.41 I 7.31 7.3 1 36 1889.60 1 197.2 Found with the 12inch. 1889.54 I 43.6 I 0.48 I 7.4 I 7.4 I @ 1105. Pleiades. 1x01. p Cassiopeiae. RA. 3h41m26s Decl. +23"49', RA. ih17~~27~ Decl. +67"30'. 1889.589 1 60.2 A and B. 034 ! 9.5, ro 36 ,594 I 58.4 0.33 1 8.8, 10 I 36 36 .689 j 54.6 II .__-___________0.31 9.5, 1 36 36 1889.62 I 57.y 0.33 I 9.3, 10.3 i 36 a534 1 40.6 I 3 24 36 Rather difficult pair 1~4'f. and 413 n. of Alcyone. It 1889.52 I 41.2 I 3.19 is DM.+23?554. /3 I 106. Pleiades. A and C (= 2 R.4. 3h42m58s Decl. +23" 5 1'. 107.3 1 28.21 1889.594 51.7 I 0.40 I 1.5, 11.5 36 .526 I 107.2 ' 27.84 Difficult pair; too faint for the DM. Place from the .534 ~ 107.4 I 28.10 Paris map of the Pleiades. It is 55' f. and 416 n. of 1889.52 I 107.4 , 28.01 28 Tauri (Pleione). p 1107. AOe, 12884. C and D (= 2' 117). RA. 13~20~36~Decl. -2 1'44'. I 1889.515 255.6 I 2.83 9-51 9.7 36 1889.35 I 1.36 8.5 ! XZ 255.0 ~ 8.5, .523 1 2.87 9.5 1 9.7 36 - 8.6, 8.6 12 .526 I 254.5 2.87 9.8, 10 36 -373 *375 -_ - I2 .534 253.9 2.88 9.5 I 9.7 36 1 I i 1.18 .378 8.5 8.5 i 36 1889.52 I 254.7 I 2.86 9.6, 9 8 .38I 0.98 -> - 136 The new star is not difficult. I 887.3 7 1.1 7 8.5 I 8.5 I p 1102. AOe. ;lo, p I 108. B.A.C. 4631. RA. 13~46~32~Decl. -3594'. A and B. 1889.583 335.6 0.93 10.5, 10.5 12 1889.373 81.3 1.48 : 6 I 6 12 .586 335.3 0.82 10.5, 10.5 36 ,383 1 86.9 1 1.14 I 6 6 ' 36 .589 338.0 1 0.77 1 10 I0 --36 .386 I 83.9 1.21 1 -, - 1 36 1889.58 I 336.3 I 0.84 1 10.3, 10.3 1889.38 I 84.0 I 1.28 I 6 6 I 53 54 A and D (= HIV.24). #lr113. B.A.C.4886. 1889.383 35901 1 65125 -, 8.5 36 RA. 14~41~21~Decl. +2"32'. .386 I 359.0 1 65.18 -,-- - 36 _____.__- - 1889.397 ~ 13701 4!'63 6 , 11.5 36 1889.38 359.0 65.21 - , - .400 I 136.7 4.42 6.5, 12.5 36 A and C. ---.4O3 137.6 4.58 I 6 , 11.5 36 1889.386 168.2 27.5a -, 12 I 36 1889.40 137.1 I 4.54 I 6.2, 11.8 Magnitude in DM. 7.7. /3 I 109. DM. +502846. KA. 14~3~18~Decl. +5O14'. A and B. #l I I 14. B.A.C. 5090. RA. 21~42~Decl. -28O 27'. ,I 889.38 I 321.3 1.83 1 -, 13.5 ish .386 322.6 1.62 - 1 I4 A and B. 321.8 1 1.88 - , 13.5 .. - -397- . __ __ 12 1889.373 3'9.7 ' 0.73 , 7 9 7,s 1889.39 321.9 I 1.78 - I '3.7 -383 3253 I 0.52 , 7 * 7-3 36 A and C. .386 I 331.5 0.69 i 7 , 7 36 __ - -__ - - - - - I I 889.38 I 356.0 53.02 ' 9 , 9 1889.38 325.7 I 0.65 I 7 9 7.3 1 .386 356.1 , 53.02 ~ 9 1 9 .397 356.8 I 53.08 j 9 1 9 AB and C (= H, 4774). 1889.39 356-3 53.04 I 9 9 9 9.28 1 - , I1 1889.373 5.8 j 12 .383 6.2 ' 9.27 1 - , 9 I 36 8 I I 10. Taylor 6665. .386 7 . ~ k5 ' 9.09 - ~___9.5 I 36- KA. 14~I 2"'2gS Decl. -36O 18'. I 889.38 5.8 1 9.21 -, 9.8 I 1889.389 127.7 3.82 6.5, 12 1 I2 There seems to be no change in the angle of the 1310 4.00 I 7.5, 12.5' 12 .392 I wide pair, as Herschel found 8?5 in 1834. .408 133.3 1 4.02 1 7 1 12-51 12 1 889.39 130.7 I 3.95 1 7 01 12.3 #l I I 15. Lal. 29840. ,f I I I I.
Recommended publications
  • Analysis of New High-Precision Transit Light Curves of WASP-10 B: Starspot
    Astronomy & Astrophysics manuscript no. wasp10 c ESO 2018 September 10, 2018 Analysis of new high-precision transit light curves of WASP-10 b: starspot occultations, small planetary radius, and high metallicity⋆ G. Maciejewski1,2, St. Raetz2, N.Nettelmann3, M. Seeliger2, Ch. Adam2, G. Nowak1, and R. Neuh¨auser2 1 Toru´nCentre for Astronomy, Nicolaus Copernicus University, Gagarina 11, PL–87100 Toru´n, Poland e-mail: [email protected] 2 Astrophysikalisches Institut und Universit¨ats-Sternwarte, Schillerg¨asschen 2–3, D–07745 Jena, Germany 3 Institut f¨ur Physik, Universit¨at Rostock, D–18051 Rostock, Germany Received ...; accepted ... ABSTRACT Context. The WASP-10 planetary system is intriguing because different values of radius have been reported for its transiting exoplanet. The host star exhibits activity in terms of photometric variability, which is caused by the rotational modulation of the spots. Moreover, a periodic modulation has been discovered in transit timing of WASP-10 b, which could be a sign of an additional body perturbing the orbital motion of the transiting planet. Aims. We attempt to refine the physical parameters of the system, in particular the planetary radius, which is crucial for studying the internal structure of the transiting planet. We also determine new mid-transit times to confirm or refute observed anomalies in transit timing. Methods. We acquired high-precision light curves for four transits of WASP-10 b in 2010. Assuming various limb-darkening laws, we generated best-fit models and redetermined parameters of the system. The prayer-bead method and Monte Carlo simulations were used to derive error estimates.
    [Show full text]
  • A Hot Subdwarf-White Dwarf Super-Chandrasekhar Candidate
    A hot subdwarf–white dwarf super-Chandrasekhar candidate supernova Ia progenitor Ingrid Pelisoli1,2*, P. Neunteufel3, S. Geier1, T. Kupfer4,5, U. Heber6, A. Irrgang6, D. Schneider6, A. Bastian1, J. van Roestel7, V. Schaffenroth1, and B. N. Barlow8 1Institut fur¨ Physik und Astronomie, Universitat¨ Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, D-14476 Potsdam-Golm, Germany 2Department of Physics, University of Warwick, Coventry, CV4 7AL, UK 3Max Planck Institut fur¨ Astrophysik, Karl-Schwarzschild-Straße 1, 85748 Garching bei Munchen¨ 4Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA 5Texas Tech University, Department of Physics & Astronomy, Box 41051, 79409, Lubbock, TX, USA 6Dr. Karl Remeis-Observatory & ECAP, Astronomical Institute, Friedrich-Alexander University Erlangen-Nuremberg (FAU), Sternwartstr. 7, 96049 Bamberg, Germany 7Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 8Department of Physics and Astronomy, High Point University, High Point, NC 27268, USA *[email protected] ABSTRACT Supernova Ia are bright explosive events that can be used to estimate cosmological distances, allowing us to study the expansion of the Universe. They are understood to result from a thermonuclear detonation in a white dwarf that formed from the exhausted core of a star more massive than the Sun. However, the possible progenitor channels leading to an explosion are a long-standing debate, limiting the precision and accuracy of supernova Ia as distance indicators. Here we present HD 265435, a binary system with an orbital period of less than a hundred minutes, consisting of a white dwarf and a hot subdwarf — a stripped core-helium burning star.
    [Show full text]
  • 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.
    [Show full text]
  • Fine-Structure Feii and Siii Absorption in the Spectrum of GRB 051111
    Draft version November 11, 2018 Preprint typeset using LATEX style emulateapj Fine-Structure Fe II and Si II Absorption in the Spectrum of GRB051111: Implications for the Burst Environment E. Berger1,2,3, B. E. Penprase4, D. B. Fox5, S. R. Kulkarni6, G. Hill7, B. Schaefer7, and M. Reed7 Draft version November 11, 2018 ABSTRACT We present an analysis of fine-structure transitions of Fe II and Si II detected in a high-resolution optical spectrum of the afterglow of GRB051111 (z =1.54948). The fine-structure absorption features arising from Fe II* to Fe II****, as well as Si II*, are confined to a narrow velocity structure extending over ±30 km s−1, which we interpret as the burst local environment, most likely a star forming region. We investigate two scenarios for the excitation of the fine-structure levels by collisions with electrons and radiative pumping by an infra-red or ultra-violet radiation field produced by intense star formation in the GRB environment, or by the GRB afterglow itself. We find that the conditions required for collisional excitation of Fe II fine-structure states cannot be easily reconciled with the relatively weak Si II* absorption. Radiative pumping by either IR or UV emission requires > 103 massive hot OB stars within a compact star-forming region a few pc in size, and in the case of IR pumping a large dust content. On the other hand, it is possible that the GRB itself provides the source of IR and/or UV radiation, in which case we estimate that the excitation takes place at a distance of ∼ 10 − 20 pc from the burst.
    [Show full text]
  • Jahresbericht 1997 Zum Titelbild: Ein Neugeborener Stern (Kreuz), Tief in Den Staub Der Molekülwolke L1551 Eingebettet, Aus Der Er Entstand
    Max-Planck-Institut für Astronomie Heidelberg-Königstuhl Jahresbericht 1997 Zum Titelbild: Ein neugeborener Stern (Kreuz), tief in den Staub der Molekülwolke L1551 eingebettet, aus der er entstand. Er ist nicht im Optischen, sondern nur als Infrarotquelle zu erkennen. Er emittiert in Polrichtung einen hellen Jet aus ioni- siertem Gas, beleuchtet einen ausgedehnten Reflexionsnebel, und regt die Herbig-Haro-Objekte HH 28 und HH 29 zum eigenen Leuchten an. Mehr dazu auf Seite 23–29. Max-Planck-Institut für Astronomie Heidelberg-Königstuhl Jahresbericht 1997 Das Max-Planck-Institut für Astronomie Geschäftsführende Direktoren: Prof. Dr. Steven Beckwith (bis 31. 8.), Prof. Dr. Immo Appenzeller (ab 1.8.1998) Wissenschaftliche Mitglieder, Kollegium, Direktoren: Prof. Dr. Immo Appenzeller (ab 1.8.1998, kommissarisch), Prof. Dr. Steven Beckwith, (ab 1. 9. 1998 beurlaubt), Prof. Dr. Hans Elsässer (bis 31. 3. 1997), Prof. Dr. Hans-Walter Rix (ab 1. 1. 1999). Fachbeirat: Prof. R. Bender, München; Prof. R.-J. Dettmar, Bochum; Prof. G. Hasinger, Potsdam; Prof. P. Léna, Meudon; Prof. M. Moles Villlamate, Madrid, Prof. F. Pacini, Firenze; Prof. K.-H. Schmidt, Potsdam; Prof. P.A. Strittmatter, Tuscon; Prof. S.D.M. White, Garching; Prof. L. Woltjer, St. Michel Obs. Derzeit hat das MPIA rund 160 Mitarbeiter, davon 43 Wissenschaftler, 37 Nachwuchs- und Gastwissenschaftler sowie 80 Techniker und Verwaltungsangestellte. Studenten der Fakultät für Physik und Astronomie der Universität Heidelberg führen am Institut Diplom- und Doktorarbeiten aus. In den Werkstätten des Instituts werden ständig Lehrlinge ausgebildet. Anschrift: MPI für Astronomie, Königstuhl 17, D-69117 Heidelberg. Telefon: 0049-6221-5280, Fax: 0049-6221-528246. E-mail: [email protected], Anonymous ftp: ftp.mpia-hd.mpg.de Homepage: http://www.mpia-hd.mpg.de Isophot Datacenter : [email protected].
    [Show full text]
  • The Extragalactic Distance Scale
    The Extragalactic Distance Scale Published in "Stellar astrophysics for the local group" : VIII Canary Islands Winter School of Astrophysics. Edited by A. Aparicio, A. Herrero, and F. Sanchez. Cambridge ; New York : Cambridge University Press, 1998 Calibration of the Extragalactic Distance Scale By BARRY F. MADORE1, WENDY L. FREEDMAN2 1NASA/IPAC Extragalactic Database, Infrared Processing & Analysis Center, California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA 91125, USA 2Observatories, Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena CA 91101, USA The calibration and use of Cepheids as primary distance indicators is reviewed in the context of the extragalactic distance scale. Comparison is made with the independently calibrated Population II distance scale and found to be consistent at the 10% level. The combined use of ground-based facilities and the Hubble Space Telescope now allow for the application of the Cepheid Period-Luminosity relation out to distances in excess of 20 Mpc. Calibration of secondary distance indicators and the direct determination of distances to galaxies in the field as well as in the Virgo and Fornax clusters allows for multiple paths to the determination of the absolute rate of the expansion of the Universe parameterized by the Hubble constant. At this point in the reduction and analysis of Key Project galaxies H0 = 72km/ sec/Mpc ± 2 (random) ± 12 [systematic]. Table of Contents INTRODUCTION TO THE LECTURES CEPHEIDS BRIEF SUMMARY OF THE OBSERVED PROPERTIES OF CEPHEID
    [Show full text]
  • A Basic Requirement for Studying the Heavens Is Determining Where In
    Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun­ damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short).
    [Show full text]
  • 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.
    [Show full text]
  • Binocular Double Star Logbook
    Astronomical League Binocular Double Star Club Logbook 1 Table of Contents Alpha Cassiopeiae 3 14 Canis Minoris Sh 251 (Oph) Psi 1 Piscium* F Hydrae Psi 1 & 2 Draconis* 37 Ceti Iota Cancri* 10 Σ2273 (Dra) Phi Cassiopeiae 27 Hydrae 40 & 41 Draconis* 93 (Rho) & 94 Piscium Tau 1 Hydrae 67 Ophiuchi 17 Chi Ceti 35 & 36 (Zeta) Leonis 39 Draconis 56 Andromedae 4 42 Leonis Minoris Epsilon 1 & 2 Lyrae* (U) 14 Arietis Σ1474 (Hya) Zeta 1 & 2 Lyrae* 59 Andromedae Alpha Ursae Majoris 11 Beta Lyrae* 15 Trianguli Delta Leonis Delta 1 & 2 Lyrae 33 Arietis 83 Leonis Theta Serpentis* 18 19 Tauri Tau Leonis 15 Aquilae 21 & 22 Tauri 5 93 Leonis OΣΣ178 (Aql) Eta Tauri 65 Ursae Majoris 28 Aquilae Phi Tauri 67 Ursae Majoris 12 6 (Alpha) & 8 Vul 62 Tauri 12 Comae Berenices Beta Cygni* Kappa 1 & 2 Tauri 17 Comae Berenices Epsilon Sagittae 19 Theta 1 & 2 Tauri 5 (Kappa) & 6 Draconis 54 Sagittarii 57 Persei 6 32 Camelopardalis* 16 Cygni 88 Tauri Σ1740 (Vir) 57 Aquilae Sigma 1 & 2 Tauri 79 (Zeta) & 80 Ursae Maj* 13 15 Sagittae Tau Tauri 70 Virginis Theta Sagittae 62 Eridani Iota Bootis* O1 (30 & 31) Cyg* 20 Beta Camelopardalis Σ1850 (Boo) 29 Cygni 11 & 12 Camelopardalis 7 Alpha Librae* Alpha 1 & 2 Capricorni* Delta Orionis* Delta Bootis* Beta 1 & 2 Capricorni* 42 & 45 Orionis Mu 1 & 2 Bootis* 14 75 Draconis Theta 2 Orionis* Omega 1 & 2 Scorpii Rho Capricorni Gamma Leporis* Kappa Herculis Omicron Capricorni 21 35 Camelopardalis ?? Nu Scorpii S 752 (Delphinus) 5 Lyncis 8 Nu 1 & 2 Coronae Borealis 48 Cygni Nu Geminorum Rho Ophiuchi 61 Cygni* 20 Geminorum 16 & 17 Draconis* 15 5 (Gamma) & 6 Equulei Zeta Geminorum 36 & 37 Herculis 79 Cygni h 3945 (CMa) Mu 1 & 2 Scorpii Mu Cygni 22 19 Lyncis* Zeta 1 & 2 Scorpii Epsilon Pegasi* Eta Canis Majoris 9 Σ133 (Her) Pi 1 & 2 Pegasi Δ 47 (CMa) 36 Ophiuchi* 33 Pegasi 64 & 65 Geminorum Nu 1 & 2 Draconis* 16 35 Pegasi Knt 4 (Pup) 53 Ophiuchi Delta Cephei* (U) The 28 stars with asterisks are also required for the regular AL Double Star Club.
    [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]
  • Eclipsing Systems with Pulsating Components (Types Β Cep, Δ Sct, Γ Dor Or Red Giant) in the Era of High-Accuracy Space Data
    galaxies Review Eclipsing Systems with Pulsating Components (Types b Cep, d Sct, g Dor or Red Giant) in the Era of High-Accuracy Space Data Patricia Lampens Royal Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium; [email protected] Abstract: Eclipsing systems are essential objects for understanding the properties of stars and stellar systems. Eclipsing systems with pulsating components are furthermore advantageous because they provide accurate constraints on the component properties, as well as a complementary method for pulsation mode determination, crucial for precise asteroseismology. The outcome of space missions aiming at delivering high-accuracy light curves for many thousands of stars in search of planetary systems has also generated new insights in the field of variable stars and revived the interest of binary systems in general. The detection of eclipsing systems with pulsating components has particularly benefitted from this, and progress in this field is growing fast. In this review, we showcase some of the recent results obtained from studies of eclipsing systems with pulsating components based on data acquired by the space missions Kepler or TESS. We consider different system configurations including semi-detached eclipsing binaries in (near-)circular orbits, a (near-)circular and non-synchronized eclipsing binary with a chemically peculiar component, eclipsing binaries showing the heartbeat phenomenon, as well as detached, eccentric double-lined systems. All display one or more pulsating component(s). Among the great variety of known classes of pulsating stars, we discuss unevolved or slightly evolved pulsators of spectral type B, A or F and red giants with solar-like oscillations. Some systems exhibit additional phenomena such as tidal effects, angular momentum transfer, (occasional) Citation: Lampens, P.
    [Show full text]
  • Introduction to Astronomical Photometry, Second Edition
    This page intentionally left blank Introduction to Astronomical Photometry, Second Edition Completely updated, this Second Edition gives a broad review of astronomical photometry to provide an understanding of astrophysics from a data-based perspective. It explains the underlying principles of the instruments used, and the applications and inferences derived from measurements. Each chapter has been fully revised to account for the latest developments, including the use of CCDs. Highly illustrated, this book provides an overview and historical background of the subject before reviewing the main themes within astronomical photometry. The central chapters focus on the practical design of the instruments and methodology used. The book concludes by discussing specialized topics in stellar astronomy, concentrating on the information that can be derived from the analysis of the light curves of variable stars and close binary systems. This new edition includes numerous bibliographic notes and a glossary of terms. It is ideal for graduate students, academic researchers and advanced amateurs interested in practical and observational astronomy. Edwin Budding is a research fellow at the Carter Observatory, New Zealand, and a visiting professor at the Çanakkale University, Turkey. Osman Demircan is Director of the Ulupınar Observatory of Çanakkale University, Turkey. Cambridge Observing Handbooks for Research Astronomers Today’s professional astronomers must be able to adapt to use telescopes and interpret data at all wavelengths. This series is designed to provide them with a collection of concise, self-contained handbooks, which covers the basic principles peculiar to observing in a particular spectral region, or to using a special technique or type of instrument. The books can be used as an introduction to the subject and as a handy reference for use at the telescope, or in the office.
    [Show full text]