Searching for Chemical Signatures of Brown Dwarf Formation? J
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Maio - 2017 Francisco Jânio Cavalcante
UNIVERSIDADE FEDERAL DO RIO GRANDE DO NORTE CENTRO DE CIÊNCIAS EXATAS E DA TERRA DEPARTAMENTO DE FÍSICA TEÓRICA E EXPERIMENTAL PROGRAMA DE PÓS-GRADUAÇÃO EM FÍSICA EVOLUÇÃO DO ÍNDICE DE FREIO MAGNÉTICO PARA ESTRELAS DO TIPO SOLAR FRANCISCO JÂNIO CAVALCANTE NATAL (RN) MAIO - 2017 FRANCISCO JÂNIO CAVALCANTE EVOLUÇÃO DO ÍNDICE DE FREIO MAGNÉTICO PARA ESTRELAS DO TIPO SOLAR Tese de Doutorado apresentada ao Programa de Pós-Graduação em Física do Departamento de Física Teórica e Experimental da Universidade Federal do Rio Grande do Norte como requisito parcial para a obtenção do grau de Doutor em Física. Orientador: Dr. Daniel Brito de Freitas NATAL (RN) MAIO - 2017 UFRN / Biblioteca Central Zila Mamede Catalogação da Publicação na Fonte Cavalcante, Francisco Jânio. Evolução do índice de freio magnético para estrelas do tipo solar / Francisco Jânio Cavalcante. - 2017. 166 f. : il. Tese (doutorado) - Universidade Federal do Rio Grande do Norte, Centro de Ciências Exatas e da Terra, Programa de Pós-Graduação em Física. Natal, RN, 2017. Orientador: Prof. Dr. Daniel Brito de Freitas. 1. Rotação estelar - Tese. 2. Freio magnético - Tese. 3. Distribuição e estatística - Tese. I. Freitas, Daniel Brito de. II. Título. RN/UF/BCZM CDU 524.3 Para Pessoas Especiais: A minha avó, minha mãe e minha namorada Ester Saraiva da Silva (in memorian) Cleta Carneiro Cavalcante Simone Santos Martins Agradecimentos Agradeço ao bom e generoso Deus, quem me deu muitas coisas no decorrer da minha vida. Deu-me compreensão e amparo nos momento de aflição e tristeza, saúde para continuar nesta caminhada. Ofereceu-me sua luz no momento em que a escuridão sufocava meu espírito. -
Arxiv:1305.7264V2 [Astro-Ph.EP] 21 Apr 2014 Spain
Draft version September 18, 2018 Preprint typeset using LATEX style emulateapj v. 08/22/09 THE MOVING GROUP TARGETS OF THE SEEDS HIGH-CONTRAST IMAGING SURVEY OF EXOPLANETS AND DISKS: RESULTS AND OBSERVATIONS FROM THE FIRST THREE YEARS Timothy D. Brandt1, Masayuki Kuzuhara2, Michael W. McElwain3, Joshua E. Schlieder4, John P. Wisniewski5, Edwin L. Turner1,6, J. Carson7,4, T. Matsuo8, B. Biller4, M. Bonnefoy4, C. Dressing9, M. Janson1, G. R. Knapp1, A. Moro-Mart´ın10, C. Thalmann11, T. Kudo12, N. Kusakabe13, J. Hashimoto13,5, L. Abe14, W. Brandner4, T. Currie15, S. Egner12, M. Feldt4, T. Golota12, M. Goto16, C. A. Grady3,17, O. Guyon12, Y. Hayano12, M. Hayashi18, S. Hayashi12, T. Henning4, K. W. Hodapp19, M. Ishii12, M. Iye13, R. Kandori13, J. Kwon13,22, K. Mede18, S. Miyama20, J.-I. Morino13, T. Nishimura12, T.-S. Pyo12, E. Serabyn21, T. Suenaga22, H. Suto13, R. Suzuki13, M. Takami23, Y. Takahashi18, N. Takato12, H. Terada12, D. Tomono12, M. Watanabe24, T. Yamada25, H. Takami12, T. Usuda12, M. Tamura13,18 Draft version September 18, 2018 ABSTRACT We present results from the first three years of observations of moving group targets in the SEEDS high-contrast imaging survey of exoplanets and disks using the Subaru telescope. We achieve typical contrasts of ∼105 at 100 and ∼106 beyond 200 around 63 proposed members of nearby kinematic moving groups. We review each of the kinematic associations to which our targets belong, concluding that five, β Pictoris (∼20 Myr), AB Doradus (∼100 Myr), Columba (∼30 Myr), Tucana-Horogium (∼30 Myr), and TW Hydrae (∼10 Myr), are sufficiently well-defined to constrain the ages of individual targets. -
Nested Sampling
Probabilistic Source Detection Farhan Feroz [email protected] Cavendish Astrophysics Source/Object Detection: Problem Definition • Aim: Detect and characterize discrete sources in a background • Each source described by a template f(p) with parameters p. • With source and noise contributions being additive and Ns source Ns d=++ bq() nr ()∑ f ( pk ) k =1 • Inference goal: Use data d to constrain source parameters Ns, pk (k = 1, 2, …, Ns). Margnialize over background and noise parameters (q and r). Probabilistic Source/Object Detection • Problems in Object Detection – Identification – Quantifying Detection – Characterization Textures in CMB Bayesian Parameter Estimation • Collect a set of N data points Di (i = 1, 2, …, N), denoted collectively as data vector D. • Propose some model (or hypothesis) H for the data, depending on a set of M parameter θi (i = 1, 2, …, N), denoted collectively as parameter vector θ. • Bayes’ Theorem: Likelihood Prior P(D | θ, H )P(θ | H ) L(θ)π(θ) P(θ | D, H ) = → P(θ) = P(D | H) Z Posterior Evidence • Parameter Estimation: P(θ) α L(θ)π(θ) posterior α likelihood x prior Bayesian Model Selection P(D | θ, H )P(θ | H ) P(D | H )P(H ) P(θ | D, H ) = → P(H | D) = P(D | H) P(D) Bayes Factor • Consider two models H0 and H1 Prior P(H | D) P(D | H )P(H ) Z P(H ) Odds R = 1 = 1 1 = 1 1 P(H 0 | D) P(D | H 0 )P(H 0 ) Z0 P(H 0 ) • Bayesian Evidence Z = P(D|H) = ∫ L ( θ ) π ( θ ) d θ plays the central role in Bayesian Model Selection. -
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. -
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. -
Guide Du Ciel Profond
Guide du ciel profond Olivier PETIT 8 mai 2004 2 Introduction hjjdfhgf ghjfghfd fg hdfjgdf gfdhfdk dfkgfd fghfkg fdkg fhdkg fkg kfghfhk Table des mati`eres I Objets par constellation 21 1 Androm`ede (And) Andromeda 23 1.1 Messier 31 (La grande Galaxie d'Androm`ede) . 25 1.2 Messier 32 . 27 1.3 Messier 110 . 29 1.4 NGC 404 . 31 1.5 NGC 752 . 33 1.6 NGC 891 . 35 1.7 NGC 7640 . 37 1.8 NGC 7662 (La boule de neige bleue) . 39 2 La Machine pneumatique (Ant) Antlia 41 2.1 NGC 2997 . 43 3 le Verseau (Aqr) Aquarius 45 3.1 Messier 2 . 47 3.2 Messier 72 . 49 3.3 Messier 73 . 51 3.4 NGC 7009 (La n¶ebuleuse Saturne) . 53 3.5 NGC 7293 (La n¶ebuleuse de l'h¶elice) . 56 3.6 NGC 7492 . 58 3.7 NGC 7606 . 60 3.8 Cederblad 211 (N¶ebuleuse de R Aquarii) . 62 4 l'Aigle (Aql) Aquila 63 4.1 NGC 6709 . 65 4.2 NGC 6741 . 67 4.3 NGC 6751 (La n¶ebuleuse de l’œil flou) . 69 4.4 NGC 6760 . 71 4.5 NGC 6781 (Le nid de l'Aigle ) . 73 TABLE DES MATIERES` 5 4.6 NGC 6790 . 75 4.7 NGC 6804 . 77 4.8 Barnard 142-143 (La tani`ere noire) . 79 5 le B¶elier (Ari) Aries 81 5.1 NGC 772 . 83 6 le Cocher (Aur) Auriga 85 6.1 Messier 36 . 87 6.2 Messier 37 . 89 6.3 Messier 38 . -
Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs
Draft version July 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The California Legacy Survey I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal,1 Benjamin J. Fulton,1, 2 Lea A. Hirsch,3 Howard T. Isaacson,4 Andrew W. Howard,1 Cayla M. Dedrick,5, 6 Ilya A. Sherstyuk,1 Sarah C. Blunt,1, 7 Erik A. Petigura,8 Heather A. Knutson,9 Aida Behmard,9, 7 Ashley Chontos,10, 7 Justin R. Crepp,11 Ian J. M. Crossfield,12 Paul A. Dalba,13, 14 Debra A. Fischer,15 Gregory W. Henry,16 Stephen R. Kane,13 Molly Kosiarek,17, 7 Geoffrey W. Marcy,1, 7 Ryan A. Rubenzahl,1, 7 Lauren M. Weiss,10 and Jason T. Wright18, 19, 20 1Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 6Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 7NSF Graduate Research Fellow 8Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 9Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 10Institute for Astronomy, University of Hawai`i, -
BAV Rundbrief Nr. 2 (2017)
BAV Rundbrief 2017 | Nr. 2 | 66. Jahrgang | ISSN 0405-5497 Bundesdeutsche Arbeitsgemeinschaft für Veränderliche Sterne e.V. (BAV) BAV Rundbrief 2017 | Nr. 2 | 66. Jahrgang | ISSN 0405-5497 Table of Contents G. Maintz Revised elements of RR Lyrae stars V574 Aur and FX CVn 45 G. Maintz Revised elements of RR Lyrae star V781 Cygni 49 G. Maintz Revised elements of RR Lyrae star V408 Tau 51 Inhaltsverzeichnis G. Maintz Überarbeitete Elemente der RR-Lyrae-Sterne V574 Aur und FX CVn 45 G. Maintz Überarbeitete Elemente des RR-Lyrae-Sterns V781 Cygni 49 G. Maintz Überarbeitete Elemente des RR-Lyrae-Sterns V408 Tau 51 Beobachtungsberichte W. Braune Meine letzte β-Lyrae-Lichtkurve aus 2016 53 M. Geffert et al. Drei neue variable Sterne im Sternbild Centaurus 56 D. Böhme V440 Gem ist ein halbregelmäßiger Veränderlicher (TYC 1329-64-1) 61 N. Buchholz Suche nach der unentdeckten Veränderlichkeit von Riesensternen in der ASAS-Datenbank 62 K. Bernhard / CL Puppis ist doch ein kataklysmischer Veränderlicher vom S. Hümmerich Typ UGSS 65 K. Wenzel Lichtkurve von S5 0716+71 August 2016 bis April 2017 70 K. Wenzel SN 2017eaw - helle Supernova in NGC 6946 71 Späni / Rusch / Veränderlicher Nebel in NGC 1333 im Perseus 72 Eisenring / Schräbler D. Bannuscher VV Cephei - den Start nicht verpassen 74 Aus der Literatur P. Lehmann AR Scorpii ist ein neuer Weißer Zwerg im Ejektor-Zustand 75 P. Lehmann Ein Brauner Zwerg im Detail 75 P. Lehmann Entdeckungen in symbiotischen Systemen und in der Nova- Forschung 76 P. Lehmann Neutrino-Emission von Supernovae 77 Aus der BAV G. -
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 -
2016 Publication Year 2021-04-23T14:32:39Z Acceptance in OA@INAF Age Consistency Between Exoplanet Hosts and Field Stars Title B
Publication Year 2016 Acceptance in OA@INAF 2021-04-23T14:32:39Z Title Age consistency between exoplanet hosts and field stars Authors Bonfanti, A.; Ortolani, S.; NASCIMBENI, VALERIO DOI 10.1051/0004-6361/201527297 Handle http://hdl.handle.net/20.500.12386/30887 Journal ASTRONOMY & ASTROPHYSICS Number 585 A&A 585, A5 (2016) Astronomy DOI: 10.1051/0004-6361/201527297 & c ESO 2015 Astrophysics Age consistency between exoplanet hosts and field stars A. Bonfanti1;2, S. Ortolani1;2, and V. Nascimbeni2 1 Dipartimento di Fisica e Astronomia, Università degli Studi di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, Italy e-mail: [email protected] 2 Osservatorio Astronomico di Padova, INAF, Vicolo dell’Osservatorio 5, 35122 Padova, Italy Received 2 September 2015 / Accepted 3 November 2015 ABSTRACT Context. Transiting planets around stars are discovered mostly through photometric surveys. Unlike radial velocity surveys, photo- metric surveys do not tend to target slow rotators, inactive or metal-rich stars. Nevertheless, we suspect that observational biases could also impact transiting-planet hosts. Aims. This paper aims to evaluate how selection effects reflect on the evolutionary stage of both a limited sample of transiting-planet host stars (TPH) and a wider sample of planet-hosting stars detected through radial velocity analysis. Then, thanks to uniform deriva- tion of stellar ages, a homogeneous comparison between exoplanet hosts and field star age distributions is developed. Methods. Stellar parameters have been computed through our custom-developed isochrone placement algorithm, according to Padova evolutionary models. The notable aspects of our algorithm include the treatment of element diffusion, activity checks in terms of 0 log RHK and v sin i, and the evaluation of the stellar evolutionary speed in the Hertzsprung-Russel diagram in order to better constrain age. -
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). -
ON the INCLINATION DEPENDENCE of EXOPLANET PHASE SIGNATURES Stephen R
The Astrophysical Journal, 729:74 (6pp), 2011 March 1 doi:10.1088/0004-637X/729/1/74 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. ON THE INCLINATION DEPENDENCE OF EXOPLANET PHASE SIGNATURES Stephen R. Kane and Dawn M. Gelino NASA Exoplanet Science Institute, Caltech, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USA; [email protected] Received 2011 December 2; accepted 2011 January 5; published 2011 February 10 ABSTRACT Improved photometric sensitivity from space-based telescopes has enabled the detection of phase variations for a small sample of hot Jupiters. However, exoplanets in highly eccentric orbits present unique opportunities to study the effects of drastically changing incident flux on the upper atmospheres of giant planets. Here we expand upon previous studies of phase functions for these planets at optical wavelengths by investigating the effects of orbital inclination on the flux ratio as it interacts with the other effects induced by orbital eccentricity. We determine optimal orbital inclinations for maximum flux ratios and combine these calculations with those of projected separation for application to coronagraphic observations. These are applied to several of the known exoplanets which may serve as potential targets in current and future coronagraph experiments. Key words: planetary systems – techniques: photometric 1. INTRODUCTION and inclination for a given eccentricity. We further calculate projected separations at apastron as a function of inclination The changing phases of an exoplanet as it orbits the host star and determine their correspondence with maximum flux ratio have long been considered as a means for their detection and locations.