DOCSLIB.ORG

To the Literature

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

SMITHSONIAN MISCELLANEOUS COLLECTIONS 1312 INDEX TO THE LITERATURE OF THE SPECTROSCOPE (188 7- I 900, BOTH inclusive) [CONTINUATION OF THE PREVIOUS INDEX BY THE SAME AUTHOR PUBLISHED IN I888] BY ALFRED TUCKERMAN WASHINGTON CITY PUBLISHED BY THE SMITHSONIAN INSTITUTION 1902 Zbe Iknicljeibocftec press, IIAcw J^orfe PREFACE. In this volume I have continued my Index to the Literature of the Spectroscope, Smithsonian Miscellaneous Collections No. 658 (published in 1888), to the end of the year 1900, after which date the International Committee for Indexing Scientific Literature begins the continuation of the work of cataloguing Spectroscopy. I have been obliged to leave Astronomical Spectroscopy incomplete, for want of space. In other respects I hope this second volume will be con- sidered an improvement on the first. Alfred Tuckerman. New York, Feb. 3, 1902 INDEX TO THE LITERATURE OF THE SPECTROSCOPE. 1887 TO 1900 (both inclusive). By Alfred Tuckerman. PART I.—AUTHOR-INDEX. Abati, G. Sul potere rifrangente e dispersive del silicio. Gazz. chim. 27 (1897), 437-455; Beibl. (1898) 397. Abbe, C. Observations of twilight and zodiacal light. Nature 38 (1889), 519-521; Beibl. (1890) 38. On the height of the aurora. Proc. Amer. Phil. Soc. (1898); Nature 58 (1898) 603; Beibl. (1899) 178. Abbot, Ch. G., and F. E. Fowle. Longitudinal deviation in prisms. Beibl. Amer. J. Sci. (4) 2 (1896) 255-257; (1897) 407. Abetti. Osservazioni dei satelliti di Giove. Astron. Nachr. 141 (1896) 134-135- Abney, W. deW., and E. Festing. Intensity of radiation through turbid media. Proc. Roy. Soc. 40 (1886) 378-380; Jahresb. (1886) 288. • . Colour photometry. Phil. Trans. 177 (1886) 423-456; 179 (1888) 547-570; 183 (1892) 521-566; Beibl. (1888) 340; (1889) 679. The solar spectrum A 7150 to X loooo. Phil. Trans. 177 (1886) 459-469; Beibl. (1888) 351, -. Transmission of sunlight through the earth's atmosphere. Phil. Trans. 179 II (1887) 251-283; 184 (1893) 1-42; Beibl. (1888) 350; (1895) 242. Measurement of the luminosity and intensity of light reflected from coloured surfaces. Phil. Mag. (5) 27 (1889) 62-69. 2 LITERATURE OF THE SPECTROSCOPE. Abney, W. deW., and T. E. Thorpe. Determination of the photo- metric intensity of the coronal Hght. Proc. Roy. Soc. 46 (1889) 354- and G. S. Edwards. Effect of the spectrum on the haloid salts of silver. Proc. Roy. Soc. 47 (1890) 249; Jahresb. (1890) 407. Numerical registration of colours. Proc. Roy. Soc. 49 (1891) 227-233; 50 (1891) 369-372; Beibl. (1891) 512. Limit of visibility of the various rays. Proc. Roy. Soc. 49 (1891) 509-521; Beibl. (1892) 741. , Sensitiveness of the eye to light and colour. Nature 47 (1893) 538-542; Beibl. (1893) 57i- Measurement of colour produced by contrast. Proc. Roy. Soc. 56 (1894) 221-229; Beibl. (1895) 179. Photographs of flames. Chem. News 70 (1894) 10. Note on photographing sources of light with monochro- matic rays. Proc. Roy. Soc. 60 (1896) 13-15; Beibl. (1897) 981. and T. E. Thorpe. Determination of the photometric in- tensity of the coronal light. Phil. Trans. 186 (1896) part I; Astrophys. J. 4 (1896) 375. Sensitiveness of the retina to light and colours. Proc. Roy. Soc. 61 (1897) 330; Beibl. (1898) 409. Ueber die Zerlegung des Spektrums des elektrischen Lichtes in Leuchtkraftmengen von drei Farben. Jahrb. f. Photogr. (1899) 338-350- Acroyd, \V. Law of colour in relation to chemical constitution. Chem. News 65 (1892) 202-203, 205; Beibl. (1892) 534. On the origin of colour. Chem. News 67 (1893) 27-28, 64, 111-112, 147; Beibl. (1893) 445; (1894) 756. Adeney, W. E., and /. Carson. The great Rowland spectrometer in the Roy. University of Ireland. Phil. Mag. (5) 46 (1898) 223-227. Agafonoff, V. Sur 1' absorption du spectre ultraviolet par les corps cristallises. C.-R. 123 (1896) 490-492; Chem. News 74 (1896) 204; Beibl. (1897) 227. Comparison de I'absorption, par les milieux cristallises, des rayons lumineux et des rayons Rontgen. C.-R. 124 (1897) 855-^57; 125 (1897) 87-90; Beibl. (1898) 781. Aitken, R. G. Variations in the spectrum of the Orion Nebula. Astro- phys. J. 6 (1897) 365. Almy, J. E. Accidental refraction in liquids. Phil. Mag. (5) 44 (1897'! 499-503; Beibl. (1898) 156. PART I. —AUTHOR-INDEX. 3 AWiaiisse, M., und G. Krucss. Beziehungen zwischen Zusammen- setzung und Absorptionsspectrum organischer Verbindungen. Ber. cliem. Ges. 22 (1889) 2065-2070; Beibl. (1889) 945. Amhronn, H. Das optische Verhalten markhaltiger und markloser Nervenfasern. Ber. sachs. Ges. d. Wiss. (1890) 419-429. Uber den Glanz der Sapphirinen. Beibl. (1890) 990. Optische Eigenschaften sehr enger Spalten. Ann. Phys. n. F. 48 (1893) 717. Ames, y. 5. The Concave Grating in theory and practice. Phil. Mag. (5) 27 (1889) 369-384; Beibl. (1889) 673. Relations between the lines of various spectra, with spe- cial reference to those of cadmium and zinc, and a redetermi- nation of their wave-lengths. Phil. Mag. (5) 30 (1890) 33-48; Jahresb. (1890) 397.—See Grunwald, Jahresb. (1887) 344; Bois- baudran, Jahresb. (1869) 174; Balmer, Jahresb. (1885) 319. '. Spectra of some gases, hydrogen and nitrogen. Phil. — Mag. (5) 30 (1890) 48-58; Beibl. (1890) 1099. Probable spectrum of sulphur. Astron. and Astrophys. 12 (1893) 50-51; Beibl. (1893) 827. — . Rontgen's X Rays. Astrophys. J. 3 (1896) 294-295. and W. J. HitinpJireys. Note on the effect of pressure upon the series in the spectrum of an element. Johns Hopkins Univ. Cir. 16 (1897); Phil. Mag. 44 (1897) 119-122; Beibl. (1897) 974- — and R. F. EarJiart. Some notes on the Zeeman effect. Johns Hopkins Univ. Cir. 17 (1898); Beibl. (1898) 892. Prismatic and Diffraction Spectra. New York, 1898, 68 pp., Harper & Bros.; Astrophys. J. 9 (1899) 277-278, rev. Amslcr, J. S. Zur Erklarung des Alpengliihens. Ztsch. phys. chem. Unterr. 8 (1895) 6, 319-320. Anderson, A. Maximum deviation of a ray of light by a prism. Cambridge Proc. 9 (1896) 195-198. Anderson, T. D. New variable star in Delphinus. Astron. Nachr. 139 (189s) 27-29. New variable in Hercules. Astron. Nachr. 141 (1896) 104. New variables in Andromeda; in Pegasus; in Hercules. Astron. Nachr. 139 (1895) 118-119. See Copeland, ibid. 115-117. New yariable in Lyra. Astron. Nachr. 139 (1896) 269. New variables in Andromeda and Hercules. Astron. Nachr. 141 (1896) 419; 142 (1897) 159. 4 LITERATURE OF THE SPECTROSCOPE. Anderson, W. Observations of the Leonids. Mon. Not. 57 (1S96) 68-69. Anding, E. Die Seeliger 'sche Theorie des Saturnringes und der Be- leuchtung der grossen Planeten tiberhaupt. Astron. Nachr. 121 (1888) 1-16. Ueber die Lichtvertheilung auf einer unvollstandig beleuch- teten Planetenscheide. Astron. Nachr. 129 (1892) 377-388. Einfluss der Sternvertheilung auf die Bestimmung des Son- nenapex nach der Bessel' schen Methode. Astron. Nachr. 140 (1896) 1-17. Andrews, L. Some characteristics of the solutions of sulpho-cyanide of iron. Proc. Iowa Acad. I. (1894) part 4; Chem. News 70 (1894) 165-166. Angstrom, K. Sur une nouvelle methode de faire des mesures abso- lues de la chaleur rayonnante. Jahresb. (1888) 320; Nova Acta Upsal. 8 (1887) 1-17. Durchstrahlung von Warme verschiedener Wellenlange durch trlibe Medien. Ann. Phys. n. F. 36 (1889) 715-725. Nyare studier ofvor det ultrarode spektrum. Svensk. Kemisk Tidskrift (1889) 98-108; Beibl. (1893) 332; Defverd. Vet. Akad. Forh. 46 (1889) 539-557; 47 (1890) 331-352- . Beobachtung uber die Strahlung der Sonne. Bih. Svensk. Vet. Akad. Handl. 15 (1889) No. 10, 19 pp. L'intensite de la radiation des gaz sous I'infiuence de la decharge ^lectrique. Vet. Akad. Forh. 48 (1891) 373-379. Bolometrische Untersuchungen liber die Starke der Strah- lung verdlinnter Gase unter dem Einflusse der elektrischen Entla- dung. Verh. d. Ges. d. Wiss. Upsala 9. April 1892; Ann. Phys. n. F. 48 (1893)493. och Palmer. Le spectre infra-rouge du chlore et de 1' acide chlorhydrique. Stockholm Akad. Forh. 50 (1893) 389-396. Bolometrische Arbeiten von Fr. Paschen. Ann. Phys. n. F. 52 (1894) 509. Bolometrische Untersuchungen. Nov. Act. Upsala, 1895. Einfache Methode zur photographischen Darstellung des in- fraroten Spektrums. Nova Acta Upsala (1895) 4 pp.; Beibl. (1896) 196. Absorptionsvermogen einer beriissten Flache. Stockholm Akad. Forh. 55 (1898) 283-295; Beibl. (1899) 97-98. Anonymous. Height of the Aurora. Nature 60 (1899) 130-133. Argon, the newly discovered gaseous constituent of the at- mosphere. Chem. News 70 (1894) 296. PART I. AUTHOR-INDEX. 5 Anioiiiadi, E. M. Aurorae of September 1894. Jour. But. A. 5 (1894) 106-107. Nouvelles observations sur Jupiter. Bull. Soc. astron. de France 2 (1896) 28-30. Saturneeni895. Bull. Soc. astron. France 1 (1896)271-273. The Hour-Glass Sea on Mars. Knowledge 20 (1897) 169. Antrick, 0. Das optische Verhalten des Cocains. Ber. chem. Ges. (1887)310. Archenhold, F. S. Ein ausgedehnter Nebel bei $ Persie. Beibl. (1893) 129. Arcimis, A. The Great Madrid Meteor. Nature 53 (1896) 395. Arendt, Th. Die Schwankungen im Wasserdampfgehalte der At- mosphare auf Grund spektroskopischer Untersuchungen. Ann. Phys. n. F. 58 (1896) 171-204. Armstrong, H. E. Origin of colour. Chem. News 65 (1892) 284; 66 (1892) 143, 155, 288, 297-300, 311-314; 67 (1893) 143-145- 255; Beibl. (1893) 206; (1894)756. Arno, R. Transparenz des Ebonits. Atti Accad. Torino (1892-1893) 414-416; Beibl. (1894) 455. La radiazione di Rontgen con tubi di Hittorf ad hidrogens rarefatto. Atti Accad. Torino 31 (1895-1896) 418-421. Arrhenms, Sv. Ueber den Einfiuss der Sonnenstrahlung auf die elek- trischen Erscheinungen in der Erdatmosphare. Meteorol. Zetsch. (1888) 297-304. Ueber den Einfiuss der Kohlensaure in der Luft auf die Temperatur des Erdbodens. Beibl. (1896) 979; Verb, deutsch. Naturf. (1895); Phil. Mag. (5) 41 (1896) 237-276. Einfiuss des atmospharischen Kohlensauregehaltes auf die Temperatur der Erdoberflache.
Recommended publications
  • Winter Constellations

    Winter Constellations

    Winter Constellations *Orion *Canis Major *Monoceros *Canis Minor *Gemini *Auriga *Taurus *Eradinus *Lepus *Monoceros *Cancer *Lynx *Ursa Major *Ursa Minor *Draco *Camelopardalis *Cassiopeia *Cepheus *Andromeda *Perseus *Lacerta *Pegasus *Triangulum *Aries *Pisces *Cetus *Leo (rising) *Hydra (rising) *Canes Venatici (rising) Orion--Myth: Orion, the great ​ ​ hunter. In one myth, Orion boasted he would kill all the wild animals on the earth. But, the earth goddess Gaia, who was the protector of all animals, produced a gigantic scorpion, whose body was so heavily encased that Orion was unable to pierce through the armour, and was himself stung to death. His companion Artemis was greatly saddened and arranged for Orion to be immortalised among the stars. Scorpius, the scorpion, was placed on the opposite side of the sky so that Orion would never be hurt by it again. To this day, Orion is never seen in the sky at the same time as Scorpius. DSO’s ● ***M42 “Orion Nebula” (Neb) with Trapezium A stellar ​ ​ ​ nursery where new stars are being born, perhaps a thousand stars. These are immense clouds of interstellar gas and dust collapse inward to form stars, mainly of ionized hydrogen which gives off the red glow so dominant, and also ionized greenish oxygen gas. The youngest stars may be less than 300,000 years old, even as young as 10,000 years old (compared to the Sun, 4.6 billion years old). 1300 ly. ​ ​ 1 ● *M43--(Neb) “De Marin’s Nebula” The star-forming ​ “comma-shaped” region connected to the Orion Nebula. ● *M78--(Neb) Hard to see. A star-forming region connected to the ​ Orion Nebula.
  • Naming the Extrasolar Planets

    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.
  • La Constellation Du Cocher Ou Auriga ( Latin )

    La Constellation Du Cocher Ou Auriga ( Latin )

    DansDans lala ss éérierie lesles constellationsconstellations lala constellationconstellation dudu CocherCocher ouou AurigaAuriga (( LatinLatin )) - Repérage - Caractéristiques - Histoire Constellation d’hiver, le Cocher fait partie des 48 constellations originellement répertoriées par Ptolémée dans son Almageste*. Superficie 657 deg² à comparer aux 1 255 deg² d’Hercule par exemple… * L'Almageste (qui est l'arabisation du grec ancien megistos (byblos) signifiant grand (livre)) est une œuvre de Claude Ptolémée datant du IIe siècle étant la somme des connaissances les plus avancées de son époque Patrice D écembre 2008 en mathématiques et en astronomie. L'Almageste contient également un catalogue d'étoiles. LocalisationLocalisation RepRep ééragerage • Le Cocher est une constellation très étendue traversée par la Voie Lactée et riche en amas d'étoiles, la constellation du Cocher se signale d'abord par son étoile principale, Capella. • Si la Grande Ourse est visible, Capella se situe dans la direction pointée par le grand chariot, à une vingtaine de degrés vers l’ Est. • Capella - Presque aussi brillante que Véga de la Lyre et d'une luminosité supérieure à celle de Rigel d'Orion. FormeForme • Partiellement circumpolaire, observée depuis une latitude de 45° Nord, la constellation dessine sensiblement un pentagone formé dans le sens des aiguilles d'une montre par Capella α Aur, ς Aur, ß du Taureau située juste à la limite sud de la constellation, puis en remontant vers le nord, θ Aur et ß Aur. • L'autre élément remarquable de la constellation est formé par les trois petites "chevrettes" η, ζ et ε Aur, qui forment un triangle serré au Sud de Capella. CaractCaract ééristiquesristiques CapellaCapella Capella (α Aurigae) appartient au groupe de tête des étoiles les plus éclatantes de nos nuits.
  • The Observer's Handbook for 1915

    The Observer's Handbook for 1915

    T he O b s e r v e r ’s H a n d b o o k FOR 1915 PUBLISHED BY The Royal Astronomical Society Of Canada E d i t e d b y C . A. CHANT SEVENTH YEAR OF PUBLICATION TORONTO 198 C o l l e g e S t r e e t Pr in t e d f o r t h e S o c ie t y CALENDAR 1915 T he O bserver' s H andbook FOR 1915 PUBLISHED BY The Royal Astronomical Society Of Canada E d i t e d b y C. A. CHANT SEVENTH YEAR OF PUBLICATION TORONTO 198 C o l l e g e S t r e e t Pr in t e d f o r t h e S o c ie t y 1915 CONTENTS Preface - - - - - - 3 Anniversaries and Festivals - - - - - 3 Symbols and Abbreviations - - - - -4 Solar and Sidereal Time - - - - 5 Ephemeris of the Sun - - - - 6 Occultation of Fixed Stars by the Moon - - 8 Times of Sunrise and Sunset - - - - 8 The Sky and Astronomical Phenomena for each Month - 22 Eclipses, etc., of Jupiter’s Satellites - - - - 46 Ephemeris for Physical Observations of the Sun - - 48 Meteors and Shooting Stars - - - - - 50 Elements of the Solar System - - - - 51 Satellites of the Solar System - - - - 52 Eclipses of Sun and Moon in 1915 - - - - 53 List of Double Stars - - - - - 53 List of Variable Stars- - - - - - 55 The Stars, their Magnitude, Velocity, etc. - - - 56 The Constellations - - - - - - 64 Comets of 1914 - - - - - 76 PREFACE The H a n d b o o k for 1915 differs from that for last year chiefly in the omission of the brief review of astronomical pro­ gress, and the addition of (1) a table of double stars, (2) a table of variable stars, and (3) a table containing 272 stars and 5 nebulae.
  • Gaia Data Release 2 Special Issue

    Gaia Data Release 2 Special Issue

    A&A 623, A110 (2019) Astronomy https://doi.org/10.1051/0004-6361/201833304 & © ESO 2019 Astrophysics Gaia Data Release 2 Special issue Gaia Data Release 2 Variable stars in the colour-absolute magnitude diagram?,?? Gaia Collaboration, L. Eyer1, L. Rimoldini2, M. Audard1, R. I. Anderson3,1, K. Nienartowicz2, F. Glass1, O. Marchal4, M. Grenon1, N. Mowlavi1, B. Holl1, G. Clementini5, C. Aerts6,7, T. Mazeh8, D. W. Evans9, L. Szabados10, A. G. A. Brown11, A. Vallenari12, T. Prusti13, J. H. J. de Bruijne13, C. Babusiaux4,14, C. A. L. Bailer-Jones15, M. Biermann16, F. Jansen17, C. Jordi18, S. A. Klioner19, U. Lammers20, L. Lindegren21, X. Luri18, F. Mignard22, C. Panem23, D. Pourbaix24,25, S. Randich26, P. Sartoretti4, H. I. Siddiqui27, C. Soubiran28, F. van Leeuwen9, N. A. Walton9, F. Arenou4, U. Bastian16, M. Cropper29, R. Drimmel30, D. Katz4, M. G. Lattanzi30, J. Bakker20, C. Cacciari5, J. Castañeda18, L. Chaoul23, N. Cheek31, F. De Angeli9, C. Fabricius18, R. Guerra20, E. Masana18, R. Messineo32, P. Panuzzo4, J. Portell18, M. Riello9, G. M. Seabroke29, P. Tanga22, F. Thévenin22, G. Gracia-Abril33,16, G. Comoretto27, M. Garcia-Reinaldos20, D. Teyssier27, M. Altmann16,34, R. Andrae15, I. Bellas-Velidis35, K. Benson29, J. Berthier36, R. Blomme37, P. Burgess9, G. Busso9, B. Carry22,36, A. Cellino30, M. Clotet18, O. Creevey22, M. Davidson38, J. De Ridder6, L. Delchambre39, A. Dell’Oro26, C. Ducourant28, J. Fernández-Hernández40, M. Fouesneau15, Y. Frémat37, L. Galluccio22, M. García-Torres41, J. González-Núñez31,42, J. J. González-Vidal18, E. Gosset39,25, L. P. Guy2,43, J.-L. Halbwachs44, N. C. Hambly38, D.
  • Astronomy 111 Recitation #1

    Astronomy 111 Recitation #1

    Astronomy 142 Recitation #10 5 April 2013 Formulas to remember Leavitt's Law (classical Cepheid variables): MV =−2.77 log Π− 1.69 d mMVV−=5log 10 pc Hubble’s Law (galaxies in the uniform Universal expansion): vr = Hd0 -1 -1 -1 -1 H0 = 74.2 km sec Mpc= 22.8 km sec Mly Redshift z =(λλ − 00) λ SN Ia magnitude(dereddened) 00 d mMVV=++5log 25 Mpc 0 MV = −19.14 dE dm Black hole accretion Lc= = εε2 , ≈ 0.1. dt dt Eddington luminosity 25 4 3GMmpe m c 2eL LL<= ; M> E 4 25 23e Gmpe m c Workshop problems Warning! The workshop problems you will do in groups in Recitation are a crucial part of the process of building up your command of the concepts important in AST 142 and subsequent courses. Do not, therefore, do your work on scratch paper and discard it. Better for each of you to keep your own account of each problem, in some sort of bound notebook. 1. (Team discussion) A type Ia supernova happens when a the mass of a white dwarf, accreting material from a close-by normal or giant stellar companions, approaches the Stoner-Anderson- Chandrasekhar mass, MM= 1.4 . Review your previous experience with degenerate stars and answer the following questions, in order. a. If mass is added to a white dwarf, does its radius get larger, smaller, or stay the same? Is this different from what happens when mass is added to an ordinary, nondegenerate star? 2013 University of Rochester 1 All rights reserved Astronomy 142, Spring 2013 b.
  • A Guide to Smartphone Astrophotography National Aeronautics and Space Administration

    A Guide to Smartphone Astrophotography National Aeronautics and Space Administration

    National Aeronautics and Space Administration A Guide to Smartphone Astrophotography National Aeronautics and Space Administration A Guide to Smartphone Astrophotography A Guide to Smartphone Astrophotography Dr. Sten Odenwald NASA Space Science Education Consortium Goddard Space Flight Center Greenbelt, Maryland Cover designs and editing by Abbey Interrante Cover illustrations Front: Aurora (Elizabeth Macdonald), moon (Spencer Collins), star trails (Donald Noor), Orion nebula (Christian Harris), solar eclipse (Christopher Jones), Milky Way (Shun-Chia Yang), satellite streaks (Stanislav Kaniansky),sunspot (Michael Seeboerger-Weichselbaum),sun dogs (Billy Heather). Back: Milky Way (Gabriel Clark) Two front cover designs are provided with this book. To conserve toner, begin document printing with the second cover. This product is supported by NASA under cooperative agreement number NNH15ZDA004C. [1] Table of Contents Introduction.................................................................................................................................................... 5 How to use this book ..................................................................................................................................... 9 1.0 Light Pollution ....................................................................................................................................... 12 2.0 Cameras ................................................................................................................................................
  • Arxiv:0908.2624V1 [Astro-Ph.SR] 18 Aug 2009

    Arxiv:0908.2624V1 [Astro-Ph.SR] 18 Aug 2009

    Astronomy & Astrophysics Review manuscript No. (will be inserted by the editor) Accurate masses and radii of normal stars: Modern results and applications G. Torres · J. Andersen · A. Gim´enez Received: date / Accepted: date Abstract This paper presents and discusses a critical compilation of accurate, fun- damental determinations of stellar masses and radii. We have identified 95 detached binary systems containing 190 stars (94 eclipsing systems, and α Centauri) that satisfy our criterion that the mass and radius of both stars be known to ±3% or better. All are non-interacting systems, so the stars should have evolved as if they were single. This sample more than doubles that of the earlier similar review by Andersen (1991), extends the mass range at both ends and, for the first time, includes an extragalactic binary. In every case, we have examined the original data and recomputed the stellar parameters with a consistent set of assumptions and physical constants. To these we add interstellar reddening, effective temperature, metal abundance, rotational velocity and apsidal motion determinations when available, and we compute a number of other physical parameters, notably luminosity and distance. These accurate physical parameters reveal the effects of stellar evolution with un- precedented clarity, and we discuss the use of the data in observational tests of stellar evolution models in some detail. Earlier findings of significant structural differences between moderately fast-rotating, mildly active stars and single stars, ascribed to the presence of strong magnetic and spot activity, are confirmed beyond doubt. We also show how the best data can be used to test prescriptions for the subtle interplay be- tween convection, diffusion, and other non-classical effects in stellar models.
  • Arxiv:2006.10868V2 [Astro-Ph.SR] 9 Apr 2021 Spain and Institut D’Estudis Espacials De Catalunya (IEEC), C/Gran Capit`A2-4, E-08034 2 Serenelli, Weiss, Aerts Et Al

    Arxiv:2006.10868V2 [Astro-Ph.SR] 9 Apr 2021 Spain and Institut D’Estudis Espacials De Catalunya (IEEC), C/Gran Capit`A2-4, E-08034 2 Serenelli, Weiss, Aerts Et Al

    Noname manuscript No. (will be inserted by the editor) Weighing stars from birth to death: mass determination methods across the HRD Aldo Serenelli · Achim Weiss · Conny Aerts · George C. Angelou · David Baroch · Nate Bastian · Paul G. Beck · Maria Bergemann · Joachim M. Bestenlehner · Ian Czekala · Nancy Elias-Rosa · Ana Escorza · Vincent Van Eylen · Diane K. Feuillet · Davide Gandolfi · Mark Gieles · L´eoGirardi · Yveline Lebreton · Nicolas Lodieu · Marie Martig · Marcelo M. Miller Bertolami · Joey S.G. Mombarg · Juan Carlos Morales · Andr´esMoya · Benard Nsamba · KreˇsimirPavlovski · May G. Pedersen · Ignasi Ribas · Fabian R.N. Schneider · Victor Silva Aguirre · Keivan G. Stassun · Eline Tolstoy · Pier-Emmanuel Tremblay · Konstanze Zwintz Received: date / Accepted: date A. Serenelli Institute of Space Sciences (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E- 08193, Spain and Institut d'Estudis Espacials de Catalunya (IEEC), Carrer Gran Capita 2, Barcelona, E-08034, Spain E-mail: [email protected] A. Weiss Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany C. Aerts Institute of Astronomy, Department of Physics & Astronomy, KU Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium and Department of Astrophysics, IMAPP, Radboud University Nijmegen, Heyendaalseweg 135, 6525 AJ Nijmegen, the Netherlands G.C. Angelou Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany D. Baroch J. C. Morales I. Ribas Institute of· Space Sciences· (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E-08193, arXiv:2006.10868v2 [astro-ph.SR] 9 Apr 2021 Spain and Institut d'Estudis Espacials de Catalunya (IEEC), C/Gran Capit`a2-4, E-08034 2 Serenelli, Weiss, Aerts et al.
  • Metodología Para La Detecci´On De Estrellas Variables

    Metodología Para La Detecci´On De Estrellas Variables

    METODOLOG´IA PARA LA DETECCION´ DE ESTRELLAS VARIABLES EN CUMULOS´ ESTELARES A PARTIR DE ANALISIS´ FOTOMETRICO´ LUISA FERNANDA CARDONA TORRES DANIELA SANCHEZ´ GIRALDO UNIVERSIDAD TECNOLOGICA´ DE PEREIRA Facultad de Ingenier´ıas Programa de Ingenier´ıaF´ısica Pereira, Noviembre de 2016 METODOLOG´IA PARA LA DETECCION´ DE ESTRELLAS VARIABLES EN CUMULOS´ ESTELARES A PARTIR DE ANALISIS´ FOTOMETRICO´ Trabajo de grado presentado por LUISA FERNANDA CARDONA TORRES DANIELA SANCHEZ´ GIRALDO COMO REQUISITO PARCIAL PARA OPTAR POR EL T´ITULO DE INGENIERO F´ISICO DIRECTOR DEL TRABAJO DE GRADO MsC. Edwin Andr´esQuintero S. UNIVERSIDAD TECNOLOGICA´ DE PEREIRA Facultad de Ingenier´ıas Programa de Ingenier´ıaF´ısica Pereira, Noviembre de 2016 2 Dedicatoria Dedicado a mis padres que lo han dado todo por verme crecer, a quien desde la oscuridad de mi vientre, ilumin´omis noches: Angel´ Garc´ıa, y a su padre. Daniela S´anchez Dedicado a quienes acompa~naron las noches de observaci´ony noches nubladas, y a mi familia que esperaba en casa. Luisa Cardona I II Dedicatoria Agradecimientos Agradecemos a los miembros del grupo de investigaci´onen Astroingenier´ıaAlfa-Ori´onpor apoyar las noches de observaci´onrealizadas para la elaboraci´onde ´esteproyecto, en especial al profesional investigador Jairo A. Aguirre, quien estuvo pendiente de cualquier dificultad t´ecnicae instrumental. Al director del proyecto M.Sc. Edwin Andr´esQuintero, por creer y hacer posible la fotometr´ıa en el Observatorio Astron´omicode la Universidad Tecnol´ogicade Pereira; por su gesti´ony paciencia para la adquisici´ony reparaci´onde instrumentos necesar- ios para ´esta´area;adem´asde capacitarnos y orientarnos en esta maravillosa ciencia que es la astronom´ıa.
  • GEORGE HERBIG and Early Stellar Evolution

    GEORGE HERBIG and Early Stellar Evolution

    GEORGE HERBIG and Early Stellar Evolution Bo Reipurth Institute for Astronomy Special Publications No. 1 George Herbig in 1960 —————————————————————– GEORGE HERBIG and Early Stellar Evolution —————————————————————– Bo Reipurth Institute for Astronomy University of Hawaii at Manoa 640 North Aohoku Place Hilo, HI 96720 USA . Dedicated to Hannelore Herbig c 2016 by Bo Reipurth Version 1.0 – April 19, 2016 Cover Image: The HH 24 complex in the Lynds 1630 cloud in Orion was discov- ered by Herbig and Kuhi in 1963. This near-infrared HST image shows several collimated Herbig-Haro jets emanating from an embedded multiple system of T Tauri stars. Courtesy Space Telescope Science Institute. This book can be referenced as follows: Reipurth, B. 2016, http://ifa.hawaii.edu/SP1 i FOREWORD I first learned about George Herbig’s work when I was a teenager. I grew up in Denmark in the 1950s, a time when Europe was healing the wounds after the ravages of the Second World War. Already at the age of 7 I had fallen in love with astronomy, but information was very hard to come by in those days, so I scraped together what I could, mainly relying on the local library. At some point I was introduced to the magazine Sky and Telescope, and soon invested my pocket money in a subscription. Every month I would sit at our dining room table with a dictionary and work my way through the latest issue. In one issue I read about Herbig-Haro objects, and I was completely mesmerized that these objects could be signposts of the formation of stars, and I dreamt about some day being able to contribute to this field of study.
  • Tabetha Boyajian's CV

    Tabetha Boyajian's CV

    Dr. Tabetha Boyajian Yale University, Department of Astronomy, 52 Hillhouse Ave., New Haven, CT 06520 USA [email protected] • +1 (404) 849-4848 • http://www.astro.yale.edu/tabetha PROFESSIONAL Yale University, Department of Astronomy, New Haven, Connecticut, USA EXPERIENCE Postdoctoral Fellow 2012 – present • Supervisor: Dr. Debra Fischer Center for high Angular Resolution Astronomy (CHARA), Georgia State University Hubble Fellow 2009 – 2012 • Supervisor: Dr. Harold McAlister EDUCATION Georgia State University, Department of Physics and Astronomy, Atlanta, Georgia, USA Doctor of Philosophy (Ph.D.) in Astronomy 2005 – 2009 • Adviser: Dr. Harold McAlister Master of Science (M.S.) in Physics 2003 – 2005 • Adviser: Dr. Douglas Gies College of Charleston, Charleston, South Carolina, USA Bachelor of Science (B.S.) in Physics with concentration in astronomy 1998 – 2003 • Graduated with Departmental Honors PROFESSIONAL Secretary, International Astronomical Union, Division G 2015 – 2018 SERVICE Steering Committee, International Astronomical Union, Division G 2015 – 2018 Review panel member NASA Kepler Guest Observer program, NASA K2 Guest Observer program, NSF-AAG program Referee The Astronomical Journal, Astronomy & Astrophysics, PASA Telescope time allocation committee member CHARA, OPTICON (external) AREAS OF Fundamental properties of stars: diameters, temperatures, exoplanet detection and characterization, SPECIALIZATION Optical/IR interferometry, stellar spectroscopy (radial velocities, abundances, activity), absolute AND INTEREST