Searching for Chemical Signatures of Brown Dwarf Formation
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Helsinki in Early Twentieth-Century Literature Urban Experiences in Finnish Prose Fiction 1890–1940
lieven ameel Helsinki in Early Twentieth-Century Literature Urban Experiences in Finnish Prose Fiction 1890–1940 Studia Fennica Litteraria The Finnish Literature Society (SKS) was founded in 1831 and has, from the very beginning, engaged in publishing operations. It nowadays publishes literature in the fields of ethnology and folkloristics, linguistics, literary research and cultural history. The first volume of the Studia Fennica series appeared in 1933. Since 1992, the series has been divided into three thematic subseries: Ethnologica, Folkloristica and Linguistica. Two additional subseries were formed in 2002, Historica and Litteraria. The subseries Anthropologica was formed in 2007. In addition to its publishing activities, the Finnish Literature Society maintains research activities and infrastructures, an archive containing folklore and literary collections, a research library and promotes Finnish literature abroad. Studia fennica editorial board Pasi Ihalainen, Professor, University of Jyväskylä, Finland Timo Kaartinen, Title of Docent, Lecturer, University of Helsinki, Finland Taru Nordlund, Title of Docent, Lecturer, University of Helsinki, Finland Riikka Rossi, Title of Docent, Researcher, University of Helsinki, Finland Katriina Siivonen, Substitute Professor, University of Helsinki, Finland Lotte Tarkka, Professor, University of Helsinki, Finland Tuomas M. S. Lehtonen, Secretary General, Dr. Phil., Finnish Literature Society, Finland Tero Norkola, Publishing Director, Finnish Literature Society Maija Hakala, Secretary of the Board, Finnish Literature Society, Finland Editorial Office SKS P.O. Box 259 FI-00171 Helsinki www.finlit.fi Lieven Ameel Helsinki in Early Twentieth- Century Literature Urban Experiences in Finnish Prose Fiction 1890–1940 Finnish Literature Society · SKS · Helsinki Studia Fennica Litteraria 8 The publication has undergone a peer review. The open access publication of this volume has received part funding via a Jane and Aatos Erkko Foundation grant. -
Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55 -
11080271.Pdf (355.0Kb)
PROGRAMA FONDECYT INFORME FINAL ETAPA 2010 COMISIÓN NACIONAL DE INVESTIGACION CIENTÍFICA Y TECNOLÓGICA VERSION OFICIAL FECHA: 02/11/2011 Nº PROYECTO : 11080271 DURACIÓN : 3 años AÑO ETAPA : 2010 TÍTULO PROYECTO : GROUND-BASED CHARACTERIZATION OF EXTRASOLAR PLANETS AND SYSTEMS DISCIPLINA PRINCIPAL : ASTRONOMIA GRUPO DE ESTUDIO : ASTRON.,COSMOL.Y PAR INVESTIGADOR(A) RESPONSABLE : PATRICIO ROJO ROJO RUBKE DIRECCIÓN : COMUNA : CIUDAD : SANTIAGO REGIÓN : METROPOLITANA FONDO NACIONAL DE DESARROLLO CIENTIFICO Y TECNOLOGICO (FONDECYT) Moneda 1375, Santiago de Chile - casilla 297-V, Santiago 21 Telefono: 2435 4350 FAX 2365 4435 Email: [email protected] INFORME FINAL PROYECTO FONDECYT INICIACION OBJETIVOS Cumplimiento de los Objetivos planteados en la etapa final, o pendientes de cumplir. Recuerde que en esta sección debe referirse a objetivos desarrollados, NO listar actividades desarrolladas. Nº OBJETIVOS CUMPLIMIENTO FUNDAMENTO 1 Preliminary analysis for our extend sample for the TOTAL The pilot program for our phase-velocity pilot phase velocity technique will be presented in was succesfully published (Cubillos et al 2011, conferences and journals. A&A 529, 88). Unfortunately, the conclusions is that will be better to wait for the next generation of instrumentation before expanding this technique to new systems. 2 Transit timing results for our extended sample TOTAL As part of his dissertation work, Sergio Hoyer will be presented in conferences and journals. monitored over a dozen planets collecting more than 60 transits to perform Transit timing analysis. Our first paper is already published on the planet OGLE-TR-111b (Hoyer et al 2011, ApJ 733, 53) and a second paper has just been accepted for the planet WASP-5b (Hoyer et al, ApJ accepted). -
Detection of Planetary and Stellar Companions to Neighboring Stars Via a Combination of Radial Velocity and Direct Imaging Techniques
Draft version May 24, 2019 Preprint typeset using LATEX style AASTeX6 v. 1.0 DETECTION OF PLANETARY AND STELLAR COMPANIONS TO NEIGHBORING STARS VIA A COMBINATION OF RADIAL VELOCITY AND DIRECT IMAGING TECHNIQUES Stephen R. Kane1, Paul A. Dalba1, Zhexing Li1, Elliott P. Horch2, Lea A. Hirsch3, Jonathan Horner4, Robert A. Wittenmyer4, Steve B. Howell5, Mark E. Everett6, R. Paul Butler7, Christopher G. Tinney8, Brad D. Carter4, Duncan J. Wright4, Hugh R.A. Jones9, Jeremy Bailey8, Simon J. O'Toole10,11 1Department of Earth and Planetary Sciences, University of California, Riverside, CA 92521, USA 2Department of Physics, Southern Connecticut State University, New Haven, CT 06515, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Centre for Astrophysics, University of Southern Queensland, Toowoomba, QLD 4350, Australia 5NASA Ames Research Center, Moffett Field, CA 94035, USA 6National Optical Astronomy Observatory, 950 N. Cherry Ave, Tucson, AZ 85719, USA 7Department of Terrestrial Magnetism, Carnegie Institution of Washington, NW, Washington, DC, 20015-1305, USA 8School of Physics and Australian Centre for Astrobiology, University of New South Wales, Sydney 2052, Australia 9Centre for Astrophysics Research, University of Hertfordshire, Hatfield, Herts AL10 9AB, UK 10Australian Astronomical Observatory, North Ryde, NSW 2113, Australia 11Australian Astronomical Optics, Faculty of Science and Engineering, Macquarie University, North Ryde, NSW 2113, Australia ABSTRACT The sensitivities of radial velocity (RV) surveys for exoplanet detection are extending to increasingly long orbital periods, where companions with periods of several years are now being regularly discov- ered. Companions with orbital periods that exceed the duration of the survey manifest in the data as an incomplete orbit or linear trend, a feature that can either present as the sole detectable com- panion to the host star, or as an additional signal overlain on the signatures of previously discovered companion(s). -
Search for Brown-Dwarf Companions of Stars⋆⋆⋆
A&A 525, A95 (2011) Astronomy DOI: 10.1051/0004-6361/201015427 & c ESO 2010 Astrophysics Search for brown-dwarf companions of stars, J. Sahlmann1,2, D. Ségransan1,D.Queloz1,S.Udry1,N.C.Santos3,4, M. Marmier1,M.Mayor1, D. Naef1,F.Pepe1, and S. Zucker5 1 Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland e-mail: [email protected] 2 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany 3 Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 4 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Portugal 5 Department of Geophysics and Planetary Sciences, Tel Aviv University, Tel Aviv 69978, Israel Received 19 July 2010 / Accepted 23 September 2010 ABSTRACT Context. The frequency of brown-dwarf companions in close orbit around Sun-like stars is low compared to the frequency of plane- tary and stellar companions. There is presently no comprehensive explanation of this lack of brown-dwarf companions. Aims. By combining the orbital solutions obtained from stellar radial-velocity curves and Hipparcos astrometric measurements, we attempt to determine the orbit inclinations and therefore the masses of the orbiting companions. By determining the masses of poten- tial brown-dwarf companions, we improve our knowledge of the companion mass-function. Methods. The radial-velocity solutions revealing potential brown-dwarf companions are obtained for stars from the CORALIE and HARPS planet-search surveys or from the literature. The best Keplerian fit to our radial-velocity measurements is found using the Levenberg-Marquardt method. -
2017 Publication Year 2020-08-04T11:06:43Z Acceptance
Publication Year 2017 Acceptance in OA@INAF 2020-08-04T11:06:43Z Title Searching for chemical signatures of brown dwarf formation Authors MALDONADO PRADO, Jesus; Villaver, E. DOI 10.1051/0004-6361/201630120 Handle http://hdl.handle.net/20.500.12386/26692 Journal ASTRONOMY & ASTROPHYSICS Number 602 A&A 602, A38 (2017) DOI: 10.1051/0004-6361/201630120 Astronomy c ESO 2017 & Astrophysics Searching for chemical signatures of brown dwarf formation? J. Maldonado1 and E. Villaver2 1 INAF–Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy e-mail: [email protected] 2 Universidad Autónoma de Madrid, Dpto. Física Teórica, Módulo 15, Facultad de Ciencias, Campus de Cantoblanco, 28049 Madrid, Spain Received 22 November 2016 / Accepted 9 February 2017 ABSTRACT Context. Recent studies have shown that close-in brown dwarfs in the mass range 35–55 MJup are almost depleted as companions to stars, suggesting that objects with masses above and below this gap might have di↵erent formation mechanisms. Aims. We aim to test whether stars harbouring massive brown dwarfs and stars with low-mass brown dwarfs show any chemical peculiarity that could be related to di↵erent formation processes. Methods. Our methodology is based on the analysis of high-resolution échelle spectra (R 57 000) from 2–3 m class telescopes. We determine the fundamental stellar parameters, as well as individual abundances of C, O,⇠ Na, Mg, Al, Si, S, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, and Zn for a large sample of stars known to have a substellar companion in the brown dwarf regime. -
The CORALIE Survey for Southern Extrasolar Planets XVII
Astronomy & Astrophysics manuscript no. coralieXVII c ESO 2019 July 1, 2019 The CORALIE survey for southern extrasolar planets XVII. New and updated long period and massive planets ? ?? M. Marmier1, D. Segransan´ 1, S. Udry1, M. Mayor1, F. Pepe1, D. Queloz1, C. Lovis1, D. Naef1, N.C. Santos2;3;1, R. Alonso4;5;1, S. Alves8;1, S. Berthet1, B. Chazelas1, B-O. Demory9;1, X. Dumusque1, A. Eggenberger1, P. Figueira2;1, M. Gillon6;1, J. Hagelberg1, M. Lendl1, R. A. Mardling7;1, D. Megevand´ 1, M. Neveu1, J. Sahlmann1, D. Sosnowska1, M. Tewes10, and A. H.M.J. Triaud1 1 Observatoire astronomique de l’Universite´ de Geneve,` 51 ch. des Maillettes - Sauverny -, CH-1290 Versoix, Switzerland 2 Centro de Astrof´ısica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 3 Departamento de F´ısica e Astronomia, Faculdade de Ciencias,ˆ Universidade do Porto, Rua do Campo Alegre, 4169-007 Porto, Portugal 4 Instituto de Astrof´ısica de Canarias, C/ V´ıa Lactea´ S/N, E-38200 La Laguna, Spain 5 Departamento de Astrof´ısica, Universidad de La Laguna, E-38205 La Laguna, Spain 6 Universite´ de Liege,` Allee´ du 6 aoutˆ 17, Sart Tilman, Liege` 1, Belgium 7 School of Mathematical Sciences, Monash University, Victoria, 3800, Australia 8 Departamento de F´ısica, Universidade Federal do Rio Grande do Norte, 59072-970, Natal, RN., Brazil 9 Department of Earth, Atmospheric and Planetary Sciences, Department of Physics, Massachusetts Institute of Technology, 77 Massachusetts Ave., Cambridge, MA 02139, USA 10 Laboratoire d’astrophysique, Ecole Polytechnique Fed´ erale´ de Lausanne (EPFL), Observatoire de Sauverny, CH-1290 Versoix, Switzerland Received month day, year; accepted month day, year ABSTRACT Context. -
Exoplanet.Eu Catalog Page 1 Star Distance Star Name Star Mass
exoplanet.eu_catalog star_distance star_name star_mass Planet name mass 1.3 Proxima Centauri 0.120 Proxima Cen b 0.004 1.3 alpha Cen B 0.934 alf Cen B b 0.004 2.3 WISE 0855-0714 WISE 0855-0714 6.000 2.6 Lalande 21185 0.460 Lalande 21185 b 0.012 3.2 eps Eridani 0.830 eps Eridani b 3.090 3.4 Ross 128 0.168 Ross 128 b 0.004 3.6 GJ 15 A 0.375 GJ 15 A b 0.017 3.6 YZ Cet 0.130 YZ Cet d 0.004 3.6 YZ Cet 0.130 YZ Cet c 0.003 3.6 YZ Cet 0.130 YZ Cet b 0.002 3.6 eps Ind A 0.762 eps Ind A b 2.710 3.7 tau Cet 0.783 tau Cet e 0.012 3.7 tau Cet 0.783 tau Cet f 0.012 3.7 tau Cet 0.783 tau Cet h 0.006 3.7 tau Cet 0.783 tau Cet g 0.006 3.8 GJ 273 0.290 GJ 273 b 0.009 3.8 GJ 273 0.290 GJ 273 c 0.004 3.9 Kapteyn's 0.281 Kapteyn's c 0.022 3.9 Kapteyn's 0.281 Kapteyn's b 0.015 4.3 Wolf 1061 0.250 Wolf 1061 d 0.024 4.3 Wolf 1061 0.250 Wolf 1061 c 0.011 4.3 Wolf 1061 0.250 Wolf 1061 b 0.006 4.5 GJ 687 0.413 GJ 687 b 0.058 4.5 GJ 674 0.350 GJ 674 b 0.040 4.7 GJ 876 0.334 GJ 876 b 1.938 4.7 GJ 876 0.334 GJ 876 c 0.856 4.7 GJ 876 0.334 GJ 876 e 0.045 4.7 GJ 876 0.334 GJ 876 d 0.022 4.9 GJ 832 0.450 GJ 832 b 0.689 4.9 GJ 832 0.450 GJ 832 c 0.016 5.9 GJ 570 ABC 0.802 GJ 570 D 42.500 6.0 SIMP0136+0933 SIMP0136+0933 12.700 6.1 HD 20794 0.813 HD 20794 e 0.015 6.1 HD 20794 0.813 HD 20794 d 0.011 6.1 HD 20794 0.813 HD 20794 b 0.009 6.2 GJ 581 0.310 GJ 581 b 0.050 6.2 GJ 581 0.310 GJ 581 c 0.017 6.2 GJ 581 0.310 GJ 581 e 0.006 6.5 GJ 625 0.300 GJ 625 b 0.010 6.6 HD 219134 HD 219134 h 0.280 6.6 HD 219134 HD 219134 e 0.200 6.6 HD 219134 HD 219134 d 0.067 6.6 HD 219134 HD -
Direct Imaging of Radial Velocity Exoplanets WFIRST-AFTA Coronagraph Study
Direct Imaging of Radial Velocity Exoplanets WFIRST-AFTA Coronagraph Study 12/18/2014 Aastha Acharya, aa533 Advisor: Dmitry Savransky, ds264 Contents Abstract .................................................................................................................................................. 2 Introduction ............................................................................................................................................ 3 Literature Review .................................................................................................................................... 4 Exoplanet Background ......................................................................................................................... 4 Detection Methods .............................................................................................................................. 4 Radial Velocity Detection Method ....................................................................................................... 7 Orbital Mechanics.............................................................................................................................. 10 Coronagraph Specification ................................................................................................................. 11 Methodology ......................................................................................................................................... 13 Results and Discussion .......................................................................................................................... -
Searching for Chemical Signatures of Brown Dwarf Formation? J
A&A 602, A38 (2017) Astronomy DOI: 10.1051/0004-6361/201630120 & c ESO 2017 Astrophysics Searching for chemical signatures of brown dwarf formation? J. Maldonado1 and E. Villaver2 1 INAF–Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy e-mail: [email protected] 2 Universidad Autónoma de Madrid, Dpto. Física Teórica, Módulo 15, Facultad de Ciencias, Campus de Cantoblanco, 28049 Madrid, Spain Received 22 November 2016 / Accepted 9 February 2017 ABSTRACT Context. Recent studies have shown that close-in brown dwarfs in the mass range 35–55 MJup are almost depleted as companions to stars, suggesting that objects with masses above and below this gap might have different formation mechanisms. Aims. We aim to test whether stars harbouring massive brown dwarfs and stars with low-mass brown dwarfs show any chemical peculiarity that could be related to different formation processes. Methods. Our methodology is based on the analysis of high-resolution échelle spectra (R ∼ 57 000) from 2–3 m class telescopes. We determine the fundamental stellar parameters, as well as individual abundances of C, O, Na, Mg, Al, Si, S, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, and Zn for a large sample of stars known to have a substellar companion in the brown dwarf regime. The sample is divided into stars hosting massive and low-mass brown dwarfs. Following previous works, a threshold of 42.5 MJup was considered. The metallicity and abundance trends of the two subsamples are compared and set in the context of current models of planetary and brown dwarf formation. -
Archival VLT/Naco Multiplicity Investigation of Exoplanet Host Stars J
Astronomy & Astrophysics manuscript no. final_version c ESO 2018 November 27, 2018 Archival VLT/NaCo multiplicity investigation of exoplanet host stars J. Dietrich1; 2 and C. Ginski1; 3 1 Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, The Netherlands e-mail: [email protected] 2 Harvard University, Cambridge, MA 02138, United States 3 Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands Received June XX, 2017; accepted YYY ABSTRACT Context. The influence of stellar multiplicity on planet formation is not yet well determined. Most planets are found using indirect detection methods via the small radial velocity or photometric variations of the primary star. These indirect detection methods are not sensitive to wide stellar companions. High-resolution imaging is thus needed to identify potential (sub)stellar companions to these stars. Aims. In this study we aim to determine the (sub)stellar multiplicity status of exoplanet host stars, that were not previously investigated for stellar multiplicity in the literature. For systems with non-detections we provide detailed detection limits to make them accessible for further statistical analysis. Methods. For this purpose we have employed previously unpublished high-resolution imaging data taken with VLT/NACO in a wide variety of different scientific programs and publicly accessible in the ESO archive. We used astrometric and theoretical population synthesis to determine whether detected companion candidates are likely to be bound or are merely chance-projected background objects. Results. We provide detailed detection limits for 39 systems and investigate 29 previously unknown companion candidates around five systems. -
COMMISSIONS 27 and 42 of the I.A.U. INFORMATION BULLETIN on VARIABLE STARS Nos. 4101{4200 1994 October { 1995 May EDITORS: L. SZ
COMMISSIONS AND OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS Nos Octob er May EDITORS L SZABADOS and K OLAH TECHNICAL EDITOR A HOLL TYPESETTING K ORI KONKOLY OBSERVATORY H BUDAPEST PO Box HUNGARY IBVSogyallakonkolyhu URL httpwwwkonkolyhuIBVSIBVShtml HU ISSN 2 CONTENTS 1994 No page E F GUINAN J J MARSHALL F P MALONEY A New Apsidal Motion Determination For DI Herculis ::::::::::::::::::::::::::::::::::::: D TERRELL D H KAISER D B WILLIAMS A Photometric Campaign on OW Geminorum :::::::::::::::::::::::::::::::::::::::::::: B GUROL Photo electric Photometry of OO Aql :::::::::::::::::::::::: LIU QUINGYAO GU SHENGHONG YANG YULAN WANG BI New Photo electric Light Curves of BL Eridani :::::::::::::::::::::::::::::::::: S Yu MELNIKOV V S SHEVCHENKO K N GRANKIN Eclipsing Binary V CygS Former InsaType Variable :::::::::::::::::::: J A BELMONTE E MICHEL M ALVAREZ S Y JIANG Is Praesep e KW Actually a Delta Scuti Star ::::::::::::::::::::::::::::: V L TOTH Ch M WALMSLEY Water Masers in L :::::::::::::: R L HAWKINS K F DOWNEY Times of Minimum Light for Four Eclipsing of Four Binary Systems :::::::::::::::::::::::::::::::::::::::::: B GUROL S SELAN Photo electric Photometry of the ShortPeriod Eclipsing Binary HW Virginis :::::::::::::::::::::::::::::::::::::::::::::: M P SCHEIBLE E F GUINAN The Sp otted Young Sun HD EK Dra ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::::::::: M BOS Photo electric Observations of AB Doradus ::::::::::::::::::::: YULIAN GUO A New VR Cyclic Change of H in Tau ::::::::::::::