DOCSLIB.ORG

Light Curves of W Ursae Majoris Systems

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Light Curves of W Ursae Majoris Systems The Light Curves of W Ursae Majoris Systems by Ian Stuart Rudnick A DISSERTATION PRESENTED TO THE GRADUATE COUNCIL OF THE UNIVERSITY OF FLORIDA IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY UNIVERSITY OF FLORIDA 1972 UNIVERSITY OF FLORIDA 3 1262 08666 451 2 To my wife, Andrea , ACKNOWLEDGMENTS The author sincerely expresses his appreciation to his conmiittee chairman and advisor, Dr. Frank BradshawJ Wood for his comments and suggestions, which greatly aided the completion of this work. The author wishes to thank Dr. R. E. Wilson of the University of South Florida for provide ing one of the synthetic light curves and for serving on the author's committee. Thanks are also due to Drs. K-Y Chen and R. C. Isler for serving on the author's committee. The author expresses his gratitude to Dr. S. M. Rucinski for providing the other synthetic light curve. The author wishes to thank Drs. J. E. Merrill and J. K. Gleim for their many helpful discussions. Thanks are also due to R. M. Williamon and T. F. Collins for their help in ob- taining some of the data and for many enlightening conver- sations. W. W. Richardson deserves highest commendation for his untiring work on the drawings. The author extends his thanks to the Department of Physics and Astronomy for providing financial support in the form of graduate assistantships, and to the Graduate School for support in the form of a Graduate School Fellow- ship* The author is indeed grateful to his parents and to his wife's parents for their encouragement. The author's wife deserves more than appreciation for her patience, encouragement, and hard work during five years of school life. Her devotion and understanding helped as nothing else could. TABLE OF CONTENTS Page ACKNOWLEDGMENTS . Hi LIST OF TABLES . vii LIST OF FIGURES . x ABSTRACT xii CHAPTER I INTRODUCTION 1 The Russell Model 2 CHAPTER II FIRST SYNTHETIC LIGHT CURVE 6 Rectification. 6 Solutions from Graphical Rectification 22 Solutions from Least Squares Rectification .... 44 Orbital Elements 55 Figures of the Components 58 Comparison of Solution with Input Parameters ... 59 CHAPTER III SECOND SYNTHETIC LIGHT CURVE. 64 Rectification , 69 Solutions ......-.„ 75 Orbital Elements and Figures of the Components . 78 Comparison of Solutions with Input Parameters. 78 CHAPTER IV THE SYSTEM OF 44i BOOTIS 87 History 87 Visual Binary 89 Spectroscopic Binary 91 Eclipsing Variable 92 Instrumentation. 93 Observations 96 Rieductioncdf Data 98 Times of Minimxam Light and the Period. 126 Variation in the period caused by motion in a visual binary system . 126 Page A recent period change 132 Light Variations. 133 Rectification . 144 Orbital Elements 146 CHAPTER V SUMMARY AND CONCLUSIONS 153 LIST OF REFERENCES 156 BIOGRAPHICAL SKETCH 161 1 LIST OF TABLES Page I Observations of First Synthetic Light Curve,; .... 7 II Graphical Rectification Coefficients for First Synthetic Light Curve 13 III Least Squares Rectification Coefficients for First Synthetic Light Curve 15 IV Rectified First Synthetic Light Curve Using Graphi- cal Rectification Coefficients 16 V Rectified First Synthetic Light Curve Using Least Squares Rectification Coefficients .... 17 VI Solutions with Different Values of Limb Darkening. 25 VII Solution for x = 0.8, 1 - £P^= 0.18, 1 - Z^^^= 0.16, o o ' = = k 0.45, p^ -0.94, a°^ = 0.9943, a^^= 0.9698. 26 VIII Solution for x = 1.0, 1 - £P^= 0.18, 1 - il^®^= 0.16, o o ' k =0.45, p^ = -0.90, a°^= 0.9905, a^^= 0.9375 ... 27 IX Solutions for x = 0.6, 1 - Z^^/9P^= 0.2142, -l^^) + o o (1 o (1 - 1°^) =0.34 33 X Solution for x = 0.8, 1 - l^^= 0.18, 1 - 1^^^= 0.16, o o ' k = 0.50, p = -0.6608, a°^= 0.89, a^^= 0.7915 ... 34 XI Solution for x = 0.8, 1 - Z^^= 0.18, 1 - 1^^^= 0.16, o o ' k = 0.55, p^ =-0.4798, a°^= 0.78, a^^= 0.6659. ... 35 XII Solution for x = 1.0, 1 - £P^= 0.18, 1 - £^®^= o o 0.16, k = 0.60, p = -0.3225, a°^= 0.68, a^^= 0.5332 36 ^ o o o ... VI Page OP "tT" XIII Shape Curves for 0^ = 50°, X = 3.955, x = oc 4.605;- X = 0.8 and = 45?9, x = 3.476, ^^ = 4.047, X = 0.8 37 XIV Depth Curve for x = 0.8, 1 - £^ = 0.16, 1 - 1^^= 0.18 41 XV Solution for x = 0.8, 1 - i^^= 0.16, 1 -!i^^^= oc 0.145, pr-oc, k = 0.65, p = -0.1625, a^ = 0.55, a^^= 0.4548 47 o jpr_ „ ,, , „sec XVI Solution for x = 0.8, 1 - 5,^ = 0.16, 1 - H^ 0.145, pr-tr, k = 0.65, p = -0.1271, a°^= 0.525, a^''= 0.4314 ..48 o XVII Solution for X = 0.8, 1 - 2p^= 0.16, 1 - Z^^^= 0.145, k = 1.0, p = 0.1540, a = 0.305 49 ^o o XVIII 0-C's from Solution for k = 1, p = 0.1540, a = 0.305 51 o XIX Solution for x = 0.8, 1 - 1^^= 0.165, 1 - ^q^*^= 0.145, k = 0.70, p = -1.429, a°^= 1.0, aj^ = ^o o o 1.067, T= 0.558590, L^ = 0.588 ^^ XX Orbital Elements for Solutions of First Synthetic Light Curve 57 XXI Figures of the Components 60 XXII Observations of Second Synthetic Light Curve • • • 67 XXIII Rectification Coefficients for Second Synthetic Light Curve 70 XXIV Rectified Second Synthetic Light Curve -j^. OC tr XXV Solution for x = 0.4, k = 0.545, a =1.0, a„ = ' o o 1.016, p =-1.10,T = 0.3126, 1 - 2.g^= 0.265, 1 -i^^^= 0.233 -76 Vlll , Page oc XXVI Solution for x = 0.4, k = 0.65, a^ = 1.0, a^^= 1.039, p = -1.538,T = 0.447537, 1 - il?^= o o ' o 0.265, 1 - 1^^^= 0.233, L-,= 0.234 79 XXVII Orbital Elements for Solutions of Second Synthetic Light Curve 80 XXVIII Figures of the Components 81 XXIX Input Parameters for Second Synthetic Light Curve 83 XXX Comparison Stars . 97 XXXI Observations of 44i Bootis 99 XXXII Standard Stars . 112 XXXIII Recent Times of Minimum Light 127 XXXIV Times of Minimiam Light with Corrections for Motion in a Visual Binary Orbit ,...,i.,.,. 131 XXXV Solutions and Orbital Elements Mth x = .6 1 _ jiP^= 0.23, 1 - £^®°= 0.13, = 41?0, and o o ' e m /m^ = 0.50 150 LIST OF FIGURES Page 1. Observations of First Synthetic Light Curve 8 2. Graphical Rectification Plots for First Synthetic Light Curve 12 3. Rectified First Synthetic Light Curve Using Graphical Rectification Coefficients . 19 4. Rectified First Synthetic Light Curve Using Least Squares Rectification Coefficients 21 5. Solution for X = 0.8, 1 - Sp^= 0.18, 1 -l^^^= 0.16, o o k = 0.45, p^ =-0.94, a°^= 0.9943, a^^= 0.9698. ... 29 6. Solution for x =1.0, 1 - £P^= 0.18, 1 - il^®°= 0.16, ' o o ' k = 0.45, p =-0.90, 0.°^= 0.9905, a^^= 0.9375. ... 31 7. Depth Curve and Shape Curves 39 8. Superpositions of Primary and Secondary Eclipses . 43 9. 0-G's from Solution for k = 1, p = 0.1540, a = 0.305 °. 52 o 10. Observations of Second Synthetic Light Curve .... 66 11. Rectified Second Synthetic Light Curve 74 12. Visual Binary Orbit of 44i Bootis 90 13. Comparison Star Extinction for July 1, 1970 110 14. Second-order Extinction for Albireo 114 15. First-order Yellow Extinction for Albireo 117 16. First-order Blue Extinction for Albireo 119 Page 17. First-order Ultra-Violet Extinction for Albireo . 121 18. UBV Transformation Coefficients 123 19. Variation in the Period of 44i Bootis B Caused by Motion in a Visual Binary System 130 20. 0-C's from Pbhl's Light Elements 134 21. 0-C's from New Light Elements 135 22. Yellow Light Curve of 44i Bootis 136 23. Blue Light Curve of 44i Bootis 137 24. The Light Curves of Different Authors 139 25. The Light Curves of Different Authors 140 26. Deformities of the Light Curve of 44i Bootis on Two Nights 143 Abstract of Dissertation Presented to the Graduate Council of the University of Florida in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy The Light Curves of W Ursae Majoris Systems by Ian Stuart Rudnick June, 1972 Chairman: Frank Bradshaw Wood Major Department: Astronomy Two synthetic light curves computed from theoretical astrophysical models of W Ursae Majoris systems are discussed. Solutions of these light curves, based on the geometrical Russell model and the Russell-Merrill method of solution of the light curves of eclipsing binaries, are presented. The relatively shallow minima caused by the partial eclipses of the first synthetic light curve lead to a problem of indeterminacy in the solution. The "observed" points in the shoulders of both synthetic light curves fall below the theoretical light curves predicted by the solutions. The addition of third light in the solution of the two synthetic light curves improves the fit of the solutions to the light curves; however, there is no sound basis for adding this third light. The orbital elements predicted by the Russell- Merrill solutions of the two synthetic light curves are not at all close to the orbital elements used to generate these light curves from the theoretical astrophysical models. In particular the Russell-Merrill solution underestimates the sizes of the components. It is concluded that the Russell model is not compatible with the theoretical astrophysical models used to generate the synthetic light curves.
Load more

Recommended publications
  • Radio Images of a Large Stellar Coronal Loop on Algol
    Radio Images of A Large Stellar Coronal Loop on Algol W. M. Peterson*, R. L. Mutel*, M. Gudel**,¨ W. M. Goss† *Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, Iowa 52240, USA **ETH Zurich, Institute of Astronomy, 8093 Zurich, Switzerland †National Radio Astronomy Observatory, Pete V. Domenici Science Operations Center, 1003 Lopezville Road, Socorro, New Mexico 87801, USA The close binary Algol contains a radio-bright K subgiant star in a very close (0.062 AU), rapid (2.86 day) orbit with a main sequence B8 star. Since the rotation periods of the two stars are tidally locked to the orbital period, the consequent rapid rotation drives a robust magnetic dynamo. A large body of evidence points to the existence of an extended, complex coronal magnetosphere originating at the cooler K subgiant1–4. The detailed morphology of the subgiant’s corona and its possible interaction with its companion are unknown, though theory predicts that the coronal plasma should be confined in magnetic loop structure5, as seen on the Sun. Here we report multi-epoch radio imaging of the Algol system, in which we see a large, persistent coronal loop approximately one subgiant diameter in height, whose base is straddling the subgiant and whose apex is oriented toward the B star. This strongly suggests that a persistent asymmetric magnetic field structure is aligned between the two stars. The loop is larger than anticipated theoretically6, 7, but the size may be a result of a magnetic interaction between the two stars. 1 We made six twelve-hour observations of Algol during a period from 6 April to 17 August 2008 with the High Sensitivity Array (HSA), a global very long baseline interferometer array.
    [Show full text]
  • THE BUSOT OBSERVATORY: TOWARDS a ROBOTIC AUTONOMOUS TELESCOPE Revista Mexicana De Astronomía Y Astrofísica, Vol
    Revista Mexicana de Astronomía y Astrofísica ISSN: 0185-1101 [email protected] Instituto de Astronomía México García-Lozano, R.; Rodes, J.J.; Torrejón, J.M.; Bernabeú, G.; Berná, J.A. THE BUSOT OBSERVATORY: TOWARDS A ROBOTIC AUTONOMOUS TELESCOPE Revista Mexicana de Astronomía y Astrofísica, vol. 48, 2016, pp. 16-21 Instituto de Astronomía Distrito Federal, México Available in: http://www.redalyc.org/articulo.oa?id=57150517002 How to cite Complete issue Scientific Information System More information about this article Network of Scientific Journals from Latin America, the Caribbean, Spain and Portugal Journal's homepage in redalyc.org Non-profit academic project, developed under the open access initiative RevMexAA (Serie de Conferencias), 48, 16–21 (2016) THE BUSOT OBSERVATORY: TOWARDS A ROBOTIC AUTONOMOUS TELESCOPE R. Garc´ıa-Lozano1,2,3, J. J. Rodes1,2, J. M. Torrej´on1,2, G. Bernab´eu1,2, and J. A.´ Bern´a1,2 RESUMEN Presentamos el observatorio de Busot, nuestro proyecto de telescopio rob´otico con capacidad para trabajar aut´onomamente. Este observatorio astron´omico, que consigui´ola categor´ıa de Minor Planet Center MPC-J02 en 2009, incluye un telescopio MEADE LX200GPS de 36 cm de di´ametro, una c´upula de 2 m de altura, una c´amara CCD ST8-XME de SBIG, con un sistema de ´optica adaptativa AO-8 y una rueda de filtros equipada con un sistema UBVRI. Estamos trabajando en la instalaci´on de un espectr´ografo SGS ST-8 al telescopio mediante un haz de fibra ´optica. Actualmente, estamos involucrados en el estudio a largo plazo de fuentes variables como sistemas binarios de rayos X y estrellas variables.
    [Show full text]
  • W Ursae Majoris Contact Binary Variables As X-Ray Sources W
    The Astronomical Journal, 131:990–993, 2006 February # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. W URSAE MAJORIS CONTACT BINARY VARIABLES AS X-RAY SOURCES W. P. Chen,1,2 Kaushar Sanchawala,1 and M. C. Chiu2 Received 2005 August 24; accepted 2005 October 29 ABSTRACT We present cross-identification of archived ROSAT X-ray point sources with W UMa variable stars found in the All-Sky Automated Survey. A total of 34 W UMa stars have been found associated with X-ray emission. We compute the distances of these W UMa systems and hence their X-ray luminosities. Our data support the ‘‘supersaturation’’ phenomenon seen in these fast rotators, namely that the faster a W UMa star rotates, the weaker its X-ray luminosity. Key words: binaries: close — stars: activity — stars: general — stars: rotation — X-rays: binaries 1. W URSAE MAJORIS STARS IN THE ALL-SKY almost 1000 periodic pulsating variables, and more than 1000 AUTOMATED SURVEY DATABASE irregular stars among the 1,300,000 stars in the R:A: ¼ 0h 6h quarter of the southern sky (Pojmanski 2002). The ASAS-3 W Ursae Majoris (W UMa) variables, also called EW stars, database now includes about 4000 entries in the list of contact are contact eclipsing binaries of main-sequence component stars eclipsing binaries (called ‘‘EC’’ in the ASAS classification). with periods of 0.2–1.4 days. The component stars may have different masses but fill their Roche lobes to share a common Light curves for variables identified by ASAS-2 are available online without classification of variable types.
    [Show full text]
  • San Diego Astronomy Association Celebrating 40 Years of Astronomical Outreach
    San Diego Astronomy Association Celebrating 40 Years of Astronomical Outreach Office (619) 645-8940 Observatory (619) 766-9118 The Scales http://www.sdaa.org by Scott Baker A Non-Profit Educational Association P.O. Box 23215, San Diego, CA 92193-3215 This month’s constellation is Libra “The Scales”. In ancient times, the great civilizations of the time had different ideas about SDAA Business Meeting Libra. The Greeks, didn’t see scales they considered this portion Will be held at: of the sky part of Scorpius. As a matter of fact, the two bright- SKF Condition Monitoring est stars in the constellation, Alpha and Beta Librae, have names 5271 Viewridge Court San Diego, CA 92123 that refer back to the constellation of Scorpius. They are known May 11th at 7:00pm as Zubenelgenubi and Zubeneschamalia, which are derivations of older Arabic names that translate into “Southern Claw” (i.e. of Program Meeting the Scorpion) for Alpha Librae and “The Northern Claw” for Beta June 16th at 7:00PM Librae. Showing of the film The Romans however, saw a scale or balance in the constella- “Universe: tion, and so named it Libra. They felt the constellation was impor- The Cosmology Quest” tant enough to give a place in the twelve Zodiacal Constellations, and is the only constellation of the Zodiac that represents and Mission Trails Regional Park Visitor & Interpretive Center inanimate object. Why so important you ask? 4000 years ago, 1 Father Junipero Serra Trail the sun, when entering Libra, marked the beginning of autumn, San Diego, CA 92119 Snacks ∗ Prizes ∗ Info ∗ Fun Doors open at 6:30PM See page 6 for details CONTENTS June 2004 Vol.
    [Show full text]
  • Libra (Astrology) - Wikipedia, the Free Encyclopedia
    מַ זַל מֹאזְ נַיִם http://www.morfix.co.il/en/Libra بُ ْر ُج ال ِميزان http://www.arabdict.com/en/english-arabic/Libra برج ِمي َزان https://translate.google.com/#en/fa/Libra Ζυγός Libra - Wiktionary http://en.wiktionary.org/wiki/Libra Libra Definition from Wiktionary, the free dictionary See also: libra Contents 1 English 1.1 Etymology 1.2 Pronunciation 1.3 Proper noun 1.3.1 Synonyms 1.3.2 Derived terms 1.3.3 Translations 1.3.4 See also 1.4 Noun 1.4.1 Antonyms 1.4.2 Translations 1.5 See also 1.6 Anagrams 2 Portuguese 2.1 Noun 3 Spanish 3.1 Proper noun English Signs of the Zodiac Virgo Scorpio English Wikipedia has an article about Libra. Etymology From Latin lībra (“scales, balance”). Pronunciation IPA (key): /ˈliːbrə/ Homophone: libre 1 of 3 6/9/2015 7:13 PM Libra - Wiktionary http://en.wiktionary.org/wiki/Libra Audio (US) 0:00 MENU Proper noun Libra 1. (astronomy ): A constellation of the zodiac, supposedly shaped like a set of scales. 2. (astrology ): The astrological sign for the scales, ruled by Venus and covering September 24 - October 23 (tropical astrology) or October 16 - November 16 (sidereal astrology). Synonyms ♎ Derived terms Libran Librae Translations constellation [show ▼] astrological sign [show ▼] See also Zubenelgenubi Zubeneschamali Noun Libra ( plural Libras ) 1. Someone with a Libra star sign Antonyms Aries Translations Someone with a Libra star sign [show ▼] See also 2 of 3 6/9/2015 7:13 PM Libra - Wiktionary http://en.wiktionary.org/wiki/Libra (Western astrology signs ) Western astrology sign ; Aries, Taurus, Gemini, Cancer, Leo, Virgo, Libra , Scorpio, Sagittarius, Capricorn, Aquarius, Pisces (Category: en:Astrology) Anagrams Arbil brail Portuguese Noun Libra f 1.
    [Show full text]
  • Publications Year: 2005 1. Apostolovska, G., Ivanova, V
    Publications year: 2005 1. Apostolovska, G., Ivanova, V., Borisov, G., Bilkina B., CCD of Asteroids at Rozhen National Astronomical Observatory from 2001 to 2003, 2005, Aerospace Research in Bulgaria, 20, 314-322 2. Apostolovska, G. Bilkina, B., Observations of the Comet Machholz 2004 Q2, MPC 53603- 53604, 24 Feb. 2005. 3. Bachev, R., Strigachev, A., Semkov, E., Short-term optical variability of high-redshift QSO's, 2005, MNRAS, 358, 774-780 4. Bode, M., Zamanov, R., Marchant, J., O'Brien, T. J., V2361 Cygni, 2005, IAUC, .No. 8511 5. Budding, E., Bakis, V., Erdem, A., Demircan, O., Iliev, L., Iliev, I., Slee, O. B., Multi-Facility Study of the Algol-Type Binary Delta Librae, 2005, Ap&SS, 296, 371-389 6. van Cauteren, P., Lampens, P., Robertson, C. W., Strigachev, A., Search for intrinsic variable stars in three open clusters: NGC 1664, NGC 6811, NGC 7209, 2005, Co. Ast., 146, 21-32 7. Dechev, M., Duchlev, P., Koleva, K., Kokotanekova, J., Petrov, N., Publ. Astron. Soc. R. Bo? kovi?, 2005, 5, 145-152 8. Dechev, M., Duchlev, P. Koleva, K. Petrov, N., Helical internal structures in eruptive prominences, 2005, Aerospace Research in Bulgaria, 20 245-252 9. Dimitrov, D. P., Panov, K. P., The flare activity of YZ CMi in 1999 – 2004, 2005, Aerospace Research in Bulgaria, 20, 214-217 10. Dimitrov, D. P., Panov, K. P., Long-term photometric investigation of FK Com, 2005, Aerospace Research in Bulgaria, 20, 218-223 11. Djurasevic, G. Dimitrov, D., Arbutina, B. Albayrak, B., Selam, S. O., A study of close binary system EE Cet, 2005, Mem Soc.
    [Show full text]
  • Astronomy with the Naked Eye a New Geography of the Heavens With
    A N EW G EOG R AP H Y OF TH E H EAV EN S W I T H D ESCR IPTIO N S A N D CH A R TS O l’ CONbTELLA TlONS. STARS. AN D PLA N ETS BY R R E P S E R V I SS G A T T . / 8 8 4 7 NEW Y ORK AND DONDON M C M V I I ! RRE P. s s av x ss g GA TT , 1 . 0 mm 33. 1 907 CONTENTS FIIE PLEASURE OF KNOWI NG TH E CONSTELLATI ONS — ’ the sta rs as lan dma rks Eflect of going north or south on the a p — — pearan ce of the hea vens Personal in fluen ce of the s ta rs View — ing the cons tella tion. a mid hi storic scenes Cass iopeia seen fro m ’ — Clytemnestra s tomb The celestia l pagea nt fro mMount Etna — — The sta rs ann ounce the seas ons Atmos pheric influence on — t he a ppea rance of the s ta rs Indi v idua lity of the stars 4 ta r — — — magn itudes Sta r colors The c ha rmof s ta r gro u pings The — h a rmony of the spheres How scientific astronomy has drifted Page 1 NSTELLATIONS ON TH E MERI DI AN I N JAN U ARY — 0! the meridian The dou ble revol u tion of the hea ven s — ~ ~ cha rioteer Ca pella a n d its his tory Ca melopa r — — — the Bu ll Aldeba ran The Hyades The Pleia ' of and su er a u the e ad es— n p stition bo t Pl i O on .
    [Show full text]
  • Pulsating Components in Binary and Multiple Stellar Systems---A
    Research in Astron. & Astrophys. Vol.15 (2015) No.?, 000–000 (Last modified: — December 6, 2014; 10:26 ) Research in Astronomy and Astrophysics Pulsating Components in Binary and Multiple Stellar Systems — A Catalog of Oscillating Binaries ∗ A.-Y. Zhou National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; [email protected] Abstract We present an up-to-date catalog of pulsating binaries, i.e. the binary and multiple stellar systems containing pulsating components, along with a statistics on them. Compared to the earlier compilation by Soydugan et al.(2006a) of 25 δ Scuti-type ‘oscillating Algol-type eclipsing binaries’ (oEA), the recent col- lection of 74 oEA by Liakos et al.(2012), and the collection of Cepheids in binaries by Szabados (2003a), the numbers and types of pulsating variables in binaries are now extended. The total numbers of pulsating binary/multiple stellar systems have increased to be 515 as of 2014 October 26, among which 262+ are oscillating eclipsing binaries and the oEA containing δ Scuti componentsare updated to be 96. The catalog is intended to be a collection of various pulsating binary stars across the Hertzsprung-Russell diagram. We reviewed the open questions, advances and prospects connecting pulsation/oscillation and binarity. The observational implication of binary systems with pulsating components, to stellar evolution theories is also addressed. In addition, we have searched the Simbad database for candidate pulsating binaries. As a result, 322 candidates were extracted. Furthermore, a brief statistics on Algol-type eclipsing binaries (EA) based on the existing catalogs is given. We got 5315 EA, of which there are 904 EA with spectral types A and F.
    [Show full text]
  • Introduction
    Cambridge University Press 978-1-107-53420-9 - The Cambridge Double Star Atlas Bruce Macevoy and Wil Tirion Excerpt More information INTRODUCTION This new edition of the Cambridge Double Star Atlas Jim Mullaney’s choice of nineteenth century double is designed to improve its utility for amateur star catalog labels has been retained as a tribute both astronomers of all skill levels. to his original Atlas concept and to the bygone astral For the first time in a publication of this type, the explorers who discovered over 90% of the systems in the focus is squarely on double stars as physical systems,so target list (see Appendix D). These labels are also a far as these can be identified with existing data. convenient link to the legacy double star literature and a Using the procedures described in Appendix A, the compact labeling style for the Atlas charts. However, target list of double stars has been increased to 2,500 as a convenience to the digital astronomer, the target systems by adding 1,100 “high probability” physical list provides both the Henry Draper (HD) and double and multiple stars and deleting more than Smithsonian (SAO) catalog numbers for each system. 850 systems beyond the reach of amateur telescopes The first will identify each system in the research or lacking any evidence of a physical connection. literature and online astronomical databases, the second Wil Tirion has completely relabeled the Atlas charts is a compact targeting command or search keyword to reflect these changes, and left in place the previous recognized by most GoTo telescope mounts and edition’s double star icons as a basis for comparison.
    [Show full text]
  • Basic Astronomy Labs
    Astronomy Laboratory Exercise 31 The Magnitude Scale On a dark, clear night far from city lights, the unaided human eye can see on the order of five thousand stars. Some stars are bright, others are barely visible, and still others fall somewhere in between. A telescope reveals hundreds of thousands of stars that are too dim for the unaided eye to see. Most stars appear white to the unaided eye, whose cells for detecting color require more light. But the telescope reveals that stars come in a wide palette of colors. This lab explores the modern magnitude scale as a means of describing the brightness, the distance, and the color of a star. The earliest recorded brightness scale was developed by Hipparchus, a natural philosopher of the second century BCE. He ranked stars into six magnitudes according to brightness. The brightest stars were first magnitude, the second brightest stars were second magnitude, and so on until the dimmest stars he could see, which were sixth magnitude. Modern measurements show that the difference between first and sixth magnitude represents a brightness ratio of 100. That is, a first magnitude star is about 100 times brighter than a sixth magnitude star. Thus, each magnitude is 100115 (or about 2. 512) times brighter than the next larger, integral magnitude. Hipparchus' scale only allows integral magnitudes and does not allow for stars outside this range. With the invention of the telescope, it became obvious that a scale was needed to describe dimmer stars. Also, the scale should be able to describe brighter objects, such as some planets, the Moon, and the Sun.
    [Show full text]
  • Numerical Simulations of Mass Transfer in Close and Contact Binaries Using Bipolytropes
    Louisiana State University LSU Digital Commons LSU Doctoral Dissertations Graduate School 2017 Numerical Simulations of Mass Transfer in Close and Contact Binaries Using Bipolytropes Kundan Vaman Kadam Louisiana State University and Agricultural and Mechanical College, [email protected] Follow this and additional works at: https://digitalcommons.lsu.edu/gradschool_dissertations Part of the Physical Sciences and Mathematics Commons Recommended Citation Kadam, Kundan Vaman, "Numerical Simulations of Mass Transfer in Close and Contact Binaries Using Bipolytropes" (2017). LSU Doctoral Dissertations. 4325. https://digitalcommons.lsu.edu/gradschool_dissertations/4325 This Dissertation is brought to you for free and open access by the Graduate School at LSU Digital Commons. It has been accepted for inclusion in LSU Doctoral Dissertations by an authorized graduate school editor of LSU Digital Commons. For more information, please [email protected]. NUMERICAL SIMULATIONS OF MASS TRANSFER IN CLOSE AND CONTACT BINARIES USING BIPOLYTROPES A Dissertation Submitted to the Graduate Faculty of the Louisiana State University and Agricultural and Mechanical College in partial fulfillment of the requirements for the degree of Doctor of Philosophy in The Department of Physics and Astronomy by Kundan Vaman Kadam B.S. in Physics, University of Mumbai, 2005 M.S., University of Mumbai, 2007 May 2017 Acknowledgments I am grateful to my advisor, Geoff Clayton, for supporting me wholeheartedly throughout the graduate school and keeping me motivated even when things didn't go as planned. I'd like to thank Hartmut Kaiser for allowing me to work on my dissertation through the NSF CREATIV grant. I am thankful to Juhan Frank for insightful discussions on the physics of binary systems and their simulations.
    [Show full text]
  • Transits of Mercury, 1605–2999 CE
    Appendix A Transits of Mercury, 1605–2999 CE Date (TT) Int. Offset Date (TT) Int. Offset Date (TT) Int. Offset 1605 Nov 01.84 7.0 −0.884 2065 Nov 11.84 3.5 +0.187 2542 May 17.36 9.5 −0.716 1615 May 03.42 9.5 +0.493 2078 Nov 14.57 13.0 +0.695 2545 Nov 18.57 3.5 +0.331 1618 Nov 04.57 3.5 −0.364 2085 Nov 07.57 7.0 −0.742 2558 Nov 21.31 13.0 +0.841 1628 May 05.73 9.5 −0.601 2095 May 08.88 9.5 +0.326 2565 Nov 14.31 7.0 −0.599 1631 Nov 07.31 3.5 +0.150 2098 Nov 10.31 3.5 −0.222 2575 May 15.34 9.5 +0.157 1644 Nov 09.04 13.0 +0.661 2108 May 12.18 9.5 −0.763 2578 Nov 17.04 3.5 −0.078 1651 Nov 03.04 7.0 −0.774 2111 Nov 14.04 3.5 +0.292 2588 May 17.64 9.5 −0.932 1661 May 03.70 9.5 +0.277 2124 Nov 15.77 13.0 +0.803 2591 Nov 19.77 3.5 +0.438 1664 Nov 04.77 3.5 −0.258 2131 Nov 09.77 7.0 −0.634 2604 Nov 22.51 13.0 +0.947 1674 May 07.01 9.5 −0.816 2141 May 10.16 9.5 +0.114 2608 May 13.34 3.5 +1.010 1677 Nov 07.51 3.5 +0.256 2144 Nov 11.50 3.5 −0.116 2611 Nov 16.50 3.5 −0.490 1690 Nov 10.24 13.0 +0.765 2154 May 13.46 9.5 −0.979 2621 May 16.62 9.5 −0.055 1697 Nov 03.24 7.0 −0.668 2157 Nov 14.24 3.5 +0.399 2624 Nov 18.24 3.5 +0.030 1707 May 05.98 9.5 +0.067 2170 Nov 16.97 13.0 +0.907 2637 Nov 20.97 13.0 +0.543 1710 Nov 06.97 3.5 −0.150 2174 May 08.15 3.5 +0.972 2644 Nov 13.96 7.0 −0.906 1723 Nov 09.71 13.0 +0.361 2177 Nov 09.97 3.5 −0.526 2654 May 14.61 9.5 +0.805 1736 Nov 11.44 13.0 +0.869 2187 May 11.44 9.5 −0.101 2657 Nov 16.70 3.5 −0.381 1740 May 02.96 3.5 +0.934 2190 Nov 12.70 3.5 −0.009 2667 May 17.89 9.5 −0.265 1743 Nov 05.44 3.5 −0.560 2203 Nov
    [Show full text]