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Dynamics and Stability of Resonant Rings in Galaxies B
Astronomy Reports, Vol. 44, No. 5, 2000, pp. 279–285. Translated from Astronomicheskiœ Zhurnal, Vol. 77, No. 5, 2000, pp. 323–330. Original Russian Text Copyright © 2000 by Kondrat’ev. Dynamics and Stability of Resonant Rings in Galaxies B. P. Kondrat’ev Udmurt State University, Krasnoarmeœskaya ul. 71, Izhevsk, 426034 Russia Received December 24, 1998 Abstract—We have developed a model for a spheroidal, ring-shaped galaxy. The stars move in a ring with an elliptical cross section at the 1 : 1 frequency resonance. The shape of the cross section of the equilibrium ring depends on the oblateness of the galaxy itself, so that the ellipse of the ring cross section is radially extended when the oblateness of the galaxy is small. If the oblateness of galaxy exceeds some critical value, the ellipse cross section is extended along the Ox3 axis. The shape of the ring cross section is circular for a galaxy with critical eccentricity. The stability of the ring over a wide range of perturbations is studied. A fundamental bicu- bic dispersion equation for the frequencies of small oscillations of a perturbed ring is derived. Application of the model to the ring galaxy NGC 7020 shows that its ring cross section should be approximately circular. Anal- ysis of the dispersion equation demonstrates that stellar orbits in the arm are unstable (but the instability incre- ment is small). We conclude that stars in the ring of this galaxy should drift from the 1 : 1 resonance, and the ring itself should evolve. © 2000 MAIK “Nauka/Interperiodica”. 1. INTRODUCTION appearance of various commensurability ratios. -
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A&A 562, A92 (2014) Astronomy DOI: 10.1051/0004-6361/201321493 & c ESO 2014 Astrophysics Li depletion in solar analogues with exoplanets Extending the sample, E. Delgado Mena1,G.Israelian2,3, J. I. González Hernández2,3,S.G.Sousa1,2,4, A. Mortier1,4,N.C.Santos1,4, V. Zh. Adibekyan1, J. Fernandes5, R. Rebolo2,3,6,S.Udry7, and M. Mayor7 1 Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: [email protected] 2 Instituto de Astrofísica de Canarias, C/ Via Lactea s/n, 38200 La Laguna, Tenerife, Spain 3 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain 4 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, 4169-007 Porto, Portugal 5 CGUC, Department of Mathematics and Astronomical Observatory, University of Coimbra, 3049 Coimbra, Portugal 6 Consejo Superior de Investigaciones Científicas, CSIC, Spain 7 Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland Received 18 March 2013 / Accepted 25 November 2013 ABSTRACT Aims. We want to study the effects of the formation of planets and planetary systems on the atmospheric Li abundance of planet host stars. Methods. In this work we present new determinations of lithium abundances for 326 main sequence stars with and without planets in the Teff range 5600–5900 K. The 277 stars come from the HARPS sample, the remaining targets were observed with a variety of high-resolution spectrographs. Results. We confirm significant differences in the Li distribution of solar twins (Teff = T ± 80 K, log g = log g ± 0.2and[Fe/H] = [Fe/H] ±0.2): the full sample of planet host stars (22) shows Li average values lower than “single” stars with no detected planets (60). -
Keck HIRES Spectroscopy of Four Candidate Solar Twins Jeremy R
Clemson University TigerPrints Publications Physics and Astronomy 11-1-2005 Keck HIRES Spectroscopy of Four Candidate Solar Twins Jeremy R. King Clemson University, [email protected] Ann M. Boesgaard University of Hawaii Simon C. Schuler Clemson University Follow this and additional works at: https://tigerprints.clemson.edu/physastro_pubs Recommended Citation Please use publisher's recommended citation. This Article is brought to you for free and open access by the Physics and Astronomy at TigerPrints. It has been accepted for inclusion in Publications by an authorized administrator of TigerPrints. For more information, please contact [email protected]. The Astronomical Journal, 130:2318–2325, 2005 November # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. KECK HIRES SPECTROSCOPY OF FOUR CANDIDATE SOLAR TWINS Jeremy R. King Department of Physics and Astronomy, Clemson University, 118 Kinard Laboratory, Clemson, SC 29634-0978; [email protected] Ann M. Boesgaard1 Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822; [email protected] and Simon C. Schuler Department of Physics and Astronomy, Clemson University, 118 Kinard Laboratory, Clemson, SC 29634-0978; [email protected] Received 2005 June 24; accepted 2005 July 13 ABSTRACT We use high signal-to-noise ratio, high-resolution Keck HIRES spectroscopy of four solar twin candidates (HIP 71813, 76114, 77718, and 78399) pulled from our Hipparcos-based Ca ii H and K survey to carry out parameter and abundance analyses of these objects. Our spectroscopic Teff estimates are 100 K hotter than the photometric scale of the recent Geneva-Copenhagen survey; several lines of evidence suggest the photometric temperatures are too cool at solar Teff. -
A Photometric and Spectroscopic Survey of Solar Twin Stars Within 50 Parsecs of the Sun I
A&A 563, A52 (2014) Astronomy DOI: 10.1051/0004-6361/201322277 & c ESO 2014 Astrophysics A photometric and spectroscopic survey of solar twin stars within 50 parsecs of the Sun I. Atmospheric parameters and color similarity to the Sun G. F. Porto de Mello1,R.daSilva1,, L. da Silva2, and R. V. de Nader1, 1 Universidade Federal do Rio de Janeiro, Observatório do Valongo, Ladeira do Pedro Antonio 43, CEP: 20080-090 Rio de Janeiro, Brazil e-mail: [gustavo;rvnader]@astro.ufrj.br, [email protected] 2 Observatório Nacional, rua Gen. José Cristino 77, CEP: 20921-400, Rio de Janeiro, Brazil e-mail: [email protected] Received 14 July 2013 / Accepted 18 September 2013 ABSTRACT Context. Solar twins and analogs are fundamental in the characterization of the Sun’s place in the context of stellar measurements, as they are in understanding how typical the solar properties are in its neighborhood. They are also important for representing sunlight observable in the night sky for diverse photometric and spectroscopic tasks, besides being natural candidates for harboring planetary systems similar to ours and possibly even life-bearing environments. Aims. We report a photometric and spectroscopic survey of solar twin stars within 50 parsecs of the Sun. Hipparcos absolute mag- nitudes and (B − V)Tycho colors were used to define a 2σ box around the solar values, where 133 stars were considered. Additional stars resembling the solar UBV colors in a broad sense, plus stars present in the lists of Hardorp, were also selected. All objects were ranked by a color-similarity index with respect to the Sun, defined by uvby and BV photometry. -
Accurate Fundamental Parameters for Lower Main Sequence Stars 3
Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 1 August 2018 (MN LATEX style file v2.2) Accurate fundamental parameters for Lower Main Sequence Stars. Luca Casagrande1⋆, Laura Portinari1 and Chris Flynn1,2 1 Tuorla Observatory, V¨ais¨al¨antie 20, FI-21500 Piikki¨o, Finland 2 Mount Stromlo Observatory, Cotter Road, Weston, ACT, Australia 1 August 2018 ABSTRACT We derive an empirical effective temperature and bolometric luminosity calibra- tion for G and K dwarfs, by applying our own implementation of the InfraRed Flux Method to multi–band photometry. Our study is based on 104 stars for which we have excellent BV (RI)C JHKS photometry, excellent parallaxes and good metallicities. Colours computed from the most recent synthetic libraries (ATLAS9 and MARCS) are found to be in good agreement with the empirical colours in the optical bands, but some discrepancies still remain in the infrared. Synthetic and empirical bolometric corrections also show fair agreement. A careful comparison to temperatures, luminosities and angular diameters ob- tained with other methods in literature shows that systematic effects still exist in the calibrations at the level of a few percent. Our InfraRed Flux Method temperature scale is 100 K hotter than recent analogous determinations in the literature, but is in agreement with spectroscopically calibrated temperature scales and fits well the colours of the Sun. Our angular diameters are typically 3% smaller when compared to other (indirect) determinations of angular diameter for such stars, but are consistent with the limb-darkening corrected predictions of the latest 3D model atmospheres and also with the results of asteroseismology. -
The HARPS Search for Southern Extra-Solar Planets
The HARPS search for southern extra-solar planets. III. Three Saturn-mass planets around HD 93083, HD 101930 and HD 102117 C. Lovis, M. Mayor, François Bouchy, F. Pepe, D. Queloz, N. C. Santos, S. Udry, W. Benz, Jean-Loup Bertaux, C. Mordasini, et al. To cite this version: C. Lovis, M. Mayor, François Bouchy, F. Pepe, D. Queloz, et al.. The HARPS search for southern extra-solar planets. III. Three Saturn-mass planets around HD 93083, HD 101930 and HD 102117. Astronomy and Astrophysics - A&A, EDP Sciences, 2005, 437 (3), pp.1121-1126. 10.1051/0004- 6361:20052864. hal-00017981 HAL Id: hal-00017981 https://hal.archives-ouvertes.fr/hal-00017981 Submitted on 17 Jan 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. A&A 437, 1121–1126 (2005) Astronomy DOI: 10.1051/0004-6361:20052864 & c ESO 2005 Astrophysics The HARPS search for southern extra-solar planets III. Three Saturn-mass planets around HD 93083, HD 101930 and HD 102117 C. Lovis1, M. Mayor1, F. Bouchy2,F.Pepe1,D.Queloz1,N.C.Santos3,1, S. Udry1,W.Benz4, J.-L. Bertaux5, C. -
SCIENCE CHINA Spectral Analysis of Two Solar Twins and the Colors of The
SCIENCE CHINA Physics, Mechanics & Astronomy • Research Paper • March 2010 Vol.53 No.3: 579–585 doi: 10.1007/s11433-009-0228-5 Spectral analysis of two solar twins and the colors of the Sun ZHAO ZhengShi1,2, CHEN YuQin1, ZHAO JingKun1 & ZHAO Gang1* 1 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; 2 Graduate University of Chinese Academy of Sciences, Beijing 100049, China Received April 24, 2009; accepted June 8, 2009 High resolution (R~40,000) and high signal-to-noise ratio (>150) spectra of two solar twins, HD146233 and HD195034, are obtained with the Coude Echelle Spectrograph at the 2.16 m telescope of the National Astronomical Observatories of Chinese Academy of Sciences (Xinglong, China). Based on the detailed spectrum match, comparisons of chemical composition and chromospheric activity, HD146233 and HD195034 are confirmed that they are similar to the Sun except for lithium abundance, which is higher than the solar value. Moreover, among nine solar twin candidates (including HD146233 and HD195034) found in the previous works, we have picked out six good solar twin candidates based on newly-derived homogenous parameters, and collected their colors in the Johnson/Cousins, Tycho, 2MASS and StrÖmgren system from the literature. The average color are (B-V)⊙=0.644 mag, (V-Ic)⊙=0.707 mag, (BT-VT)⊙=0.725 mag, (J-H)⊙=0.288 mag, (H-K)⊙=0.066 mag, (v-y)⊙=1.028 mag, (v-b)⊙=0.619 mag, (u-v)⊙=0.954 mag and (b-y)⊙=0.409 mag, which represent the solar colors with higher precision than pre- vious works. -
Annual Report / Rapport Annuel / Jahresbericht 1982
COVER PICTURE PHOTOGRAPHIE OE UMSCHLAGSPHOTO COUVERTURE The southern barred galaxy NGC 1365 La galaxie bamie australe NGC 1365 Die südliche Balkengalaxie NGC 1365 as photographed with the Schmidt tele prise avec le tetescope de Schmidt. Cette auJgenommen mit dem Schmidt-Tele scope. This galaxy at a distance oJ about galaxie, distante d'environ 100.000.000 skop. Die etwa 100.000.000 Lichtjahre 100,000,000 light years is also an X-ray annees-lumiere, est aussi une saurce X; entJernte Galaxie ist auch eine Röntgen• saurce; it has been investigated exten elle a ete etudiee intensivement avec le quelle; sie ist mit dem 3,6-m-Teleskop sively with the 3.6 m telescope. The blue telescope de 3,6 m. Les parties bleues sont eingehend untersucht worden. Die blau parts are populated by young massive peuplees d'etoiles jeunes de grande masse, en Regionen sind von jungen, massereI stars and gas, while the yellow light et de gas, tandis que la lumiere jaune chen Sternen und Gas bevölkert, wäh• comes Jrom older stars oJ lower mass. provient d'Ctoiles plus vieilles et de masses rend das gelbe Licht von älteren und (Schmidt photographs by H-E. Schuster; plus Jaibles. masseärmeren Sternen kommt. colour composite by C. Madsen.) (Cliches Schmidt pris par H-E. Schuster; (Schmidt-AuJnahmen: H-E. Schuster; tirage couleur: C. Madsen.) Farbmontage: C. Madsen.) Annual Report / Rapport annuel / Jahresbericht 1982 presented to the Council by the Director General presente au Conseil par le Directeur general dem Rat vorgelegt vom Generaldirektor Prof. Dr. L. Woltjer EUROPEAN SOUTHERN OBSERVATORY Organisation Europeenne pour des Recherches Astronomiques dans l'Hemisphere Austral Europäische Organisation für astronomische Forschung in der südlichen Hemisphäre Table Table des Inhalts of Contents matleres" verzeichnis INTRODUCTION ,. -
On the Mass Estimation for FGK Stars: Comparison of Several Methods
Mon. Not. R. Astron. Soc. 000, 1–?? (2002) Printed 29 August 2014 (MN LATEX style file v2.2) On the mass estimation for FGK stars: comparison of several methods F. J. G. Pinheiro1,2⋆, J. M. Fernandes1,2,3, M. S. Cunha4,5, M. J. P. F. G. Monteiro4,5,6, N. C. Santos4,5,6, S. G. Sousa4,5,6, J. P. Marques7, J.-J. Fang8, A. Mortier9 and J. Sousa4,5 1Centro de Geofísica da Universidade de Coimbra 2Observatório Geofísico e Astronómico da Universidade de Coimbra 3Departamento de Matemática da Universidade de Coimbra, Largo D. Dinis, P-3001-454 Coimbra, Portugal 4Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, PT4150-762 Porto, Portugal 5Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 6Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Portugal 7The Institut d’Astrophysique Spatiale, Orsay, France 8Centro de Física Computacional, Department of Physics, University of Coimbra, P-3004-516 Coimbra, Portugal 9SUPA, School of Physics and Astronomy, University of St Andrews, St Andrews KY16 9SS, UK Accepted . Received ABSTRACT Stellar evolutionary models simulate well binary stars when individual stellar mass and system metallicity are known. The mass can be derived directly from observations only in the case of multiple stellar systems, mainly binaries. Yet the number of such stars for which ls accurate stellar masses are available is rather small. The main goal of this project is to provide realistic mass estimates for an homogeneous sample of about a thousand FGK single stars, using four different methods and techniques. -
The Anglo-Australian Planet Search XXIV: the Frequency of Jupiter
The Anglo-Australian Planet Search XXIV: The Frequency of Jupiter Analogs Robert A. Wittenmyer1,2,3, R.P. Butler4, C.G. Tinney1,2, Jonathan Horner3,2, B.D. Carter3, D.J. Wright1,2, H.R.A. Jones5, J. Bailey1,2, Simon J. O’Toole6 [email protected] ABSTRACT We present updated simulations of the detectability of Jupiter analogs by the 17- year Anglo-Australian Planet Search. The occurrence rate of Jupiter-like planets that have remained near their formation locations beyond the ice line is a critical datum necessary to constrain the details of planet formation. It is also vital in our quest to fully understand how common (or rare) planetary systems like our own are in the Galaxy. From a sample of 202 solar-type stars, and correcting for +2.8 imperfect detectability on a star-by-star basis, we derive a frequency of 6.2−1.6% for giant planets in orbits from 3-7 AU. When a consistent definition of “Jupiter analog” is used, our results are in agreement with those from other legacy radial velocity surveys. Subject headings: planetary systems — techniques: radial velocities 1. Introduction Much attention has been brought to bear in recent years on the occurrence rate of Earth-like planets (e.g. Howard et al. 2012; Wittenmyer et al. 2011b; Kopparapu 2013). arXiv:1601.05465v1 [astro-ph.EP] 20 Jan 2016 1School of Physics, University of New South Wales, Sydney 2052, Australia 2Australian Centre for Astrobiology, University of New South Wales, Sydney 2052, Australia 3Computational Engineering and Science Research Centre, University of Southern Queensland, Toowoomba, Queensland 4350, Australia 4Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, NW, Washington, DC 20015-1305, USA 5Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, Herts AL10 9AB, UK 6Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia –2– This is due in large part to the flood of data from the Kepler spacecraft mission, which has provided evidence that small planets are exceedingly common (e.g. -
The HARPS Search for Southern Extra-Solar Planets. III. Three Saturn
Astronomy & Astrophysics manuscript no. 2864 November 14, 2018 (DOI: will be inserted by hand later) The HARPS search for southern extra-solar planets⋆ III. Three Saturn-mass planets around HD 93083, HD 101930 and HD 102117 C. Lovis1, M. Mayor1, F. Bouchy2, F. Pepe1, D. Queloz1, N.C. Santos3,1, S. Udry1, W. Benz4, J.-L. Bertaux5, C. Mordasini4, and J.-P. Sivan2 1 Observatoire de Gen`eve, 51 ch. des Maillettes, 1290 Sauverny, Switzerland e-mail: [email protected] 2 Laboratoire d’Astrophysique de Marseille, Traverse du Siphon, 13013 Marseille, France 3 Centro de Astronomia e Astrof´isica da Universidade de Lisboa, Observat´orio Astron´omico de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal 4 Physikalisches Institut Universit¨at Bern, Sidlerstrasse 5, 3012 Bern, Switzerland 5 Service d’A´eronomie du CNRS, BP 3, 91371 Verri`eres-le-Buisson, France Received 11 February 2005 / Accepted 16 March 2005 Abstract. We report on the detection of three Saturn-mass planets discovered with the HARPS instrument. HD 93083 shows radial-velocity (RV) variations best explained by the presence of a companion of 0.37 MJup orbiting in 143.6 days. HD 101930 b has an orbital period of 70.5 days and a minimum mass of 0.30 MJup. For HD 102117, we present the independent detection of a companion with m2 sin i = 0.14 MJup and orbital period P = 20.7 days. This planet was recently detected by Tinney et al. (2004). Activity and bisector indicators exclude any significant RV perturbations of stellar origin, reinforcing the planetary interpreta- tion of the RV variations. -
Non-LTE Analysis of K I in Late-Type Stars? Henrique Reggiani1,2, Anish M
A&A 627, A177 (2019) Astronomy https://doi.org/10.1051/0004-6361/201935156 & © ESO 2019 Astrophysics Non-LTE analysis of K I in late-type stars? Henrique Reggiani1,2, Anish M. Amarsi2, Karin Lind2,3, Paul S. Barklem4, Oleg Zatsarinny5, Klaus Bartschat5, Dmitry V. Fursa6, Igor Bray6, Lorenzo Spina7, and Jorge Meléndez1 1 Universidade de São Paulo, Instituto de Astronomia, Geofísica e Ciências Atmosféricas, IAG, Departamento de Astronomia, Rua do Matão 1226, Cidade Universitária, 05508-900 SP, Brazil e-mail: [email protected] 2 Max-Planck Institute for Astronomy, Konigstuhl 17, 69117 Heidelberg, Germany 3 Observational Astrophysics, Department of Physics and Astronomy, Uppsala University, Box 516, 751 20 Uppsala, Sweden 4 Theoretical Astrophysics, Department of Physics and Astronomy, Uppsala University, Box 516, 751 20 Uppsala, Sweden 5 Department of Physics and Astronomy, Drake University, Des Moines, Iowa 50311, USA 6 Curtin Institute for Computation and Department of Physics and Astronomy, Kent Street, Bentley, Perth, Western Australia 6102, Australia 7 Monash Centre for Astrophysics, School of Physics and Astronomy, Monash University, VIC 3800, Australia Received 29 January 2019 / Accepted 7 June 2019 ABSTRACT Context. Older models of Galactic chemical evolution (GCE) predict [K/Fe] ratios as much as 1 dex lower than those inferred from stellar observations. Abundances of potassium are mainly based on analyses of the 7698 Å resonance line, and the discrepancy between GCE models and observations is in part caused by the assumption of local thermodynamic equilibrium (LTE) in spectroscopic analyses. Aims. We study the statistical equilibrium of K I, focusing on the non-LTE effects on the 7698 Å line.