Pedro Figueira – Curriculum Vitae
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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. -
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 -
A Search for Variability and Transit Signatures In
A SEARCH FOR VARIABILITY AND TRANSIT SIGNATURES IN HIPPARCOS PHOTOMETRIC DATA A thesis presented to the faculty of 3 ^ San Francisco State University Zo\% In partial fulfilment of W* The Requirements for The Degree Master of Science In Physics: Astronomy by Badrinath Thirumalachari San JVancisco, California December 2018 Copyright by Badrinath Thirumalachari 2018 CERTIFICATION OF APPROVAL I certify that I have read A SEARCH FOR VARIABILITY AND TRANSIT SIGNATURES IN HIPPARCOS PHOTOMETRIC DATA by Badrinath Thirumalachari and that in my opinion this work meets the criteria for approving a thesis submitted in partial fulfillment of the requirements for the degree: Master of Science in Physics: Astronomy at San Francisco State University. fov- Dr. Stephen Kane, Ph.D. Astrophysics Associate Professor of Planetary Astrophysics Dr. Uo&eph Barranco, Ph.D. .%trtJphysics Chairfe Associate Professor of Physics K + A Q , L a . Dr. Ron Marzke, Ph.D. Astronomy Assoc. Dean of College of Science & Engineering A SEARCH FOR VARIABILITY AND TRANSIT SIGNATURES IN HIPPARCOS PHOTOMETRIC DATA Badrinath Thirumalachari San Francisco State University 2018 The study and characterization of exoplanets has picked up pace rapidly over the past few decades with the invention of newer techniques and instruments. Detecting transits in stellar photometric data around stars already known to harbor exoplanets is crucial for exoplanet characterization. Due to these advancements we now have oceans of data and coming up with an automated way of performing exoplanet characterization is a challenge. In this thesis I describe one such method to search for transits in Hipparcos dataset containing photometric data for over 118000 stars. The radial velocity method has discovered a lot of planets around bright host stars and a follow up transit detection will give us the density of the exoplanet. -
Mètodes De Detecció I Anàlisi D'exoplanetes
MÈTODES DE DETECCIÓ I ANÀLISI D’EXOPLANETES Rubén Soussé Villa 2n de Batxillerat Tutora: Dolors Romero IES XXV Olimpíada 13/1/2011 Mètodes de detecció i anàlisi d’exoplanetes . Índex - Introducció ............................................................................................. 5 [ Marc Teòric ] 1. L’Univers ............................................................................................... 6 1.1 Les estrelles .................................................................................. 6 1.1.1 Vida de les estrelles .............................................................. 7 1.1.2 Classes espectrals .................................................................9 1.1.3 Magnitud ........................................................................... 9 1.2 Sistemes planetaris: El Sistema Solar .............................................. 10 1.2.1 Formació ......................................................................... 11 1.2.2 Planetes .......................................................................... 13 2. Planetes extrasolars ............................................................................ 19 2.1 Denominació .............................................................................. 19 2.2 Història dels exoplanetes .............................................................. 20 2.3 Mètodes per detectar-los i saber-ne les característiques ..................... 26 2.3.1 Oscil·lació Doppler ........................................................... 27 2.3.2 Trànsits -
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. -
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 -
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. -
Alves Do Nascimento, S. Dissertaã§Ã£O De Mestrado UFRN/DFTE
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 PROPRIEDADES FÍSICAS DE PLANETAS EXTRASOLARES Sânzia Alves do Nascimento Orientador: Prof. Dr. José Renan De Medeiros Dissertação apresentada ao Departamento de Físi- ca Teórica e Experimental da Universidade Fede- ral do Rio Grande do Norte como requisito parcial à obtenção do grau de MESTRE em FÍSICA. Natal, abril de 2008 Aos meus pais, por terem sido os responsáveis pelo evento mais importante da minha vida: meu nascimento. Na mesma pedra se encontram, Conforme o povo traduz, Quando se nasce - uma estrela, Quando se morre - uma cruz. Mas quantos que aqui repousam Hão de emendar-nos assim: “Ponham-me a cruz no princípio... E a luz da estrela no fim!” Mário Quintana (Inscrição para um portão de cemitério) Ser como o rio que deflui Silencioso dentro da noite. Não temer as trevas da noite. Se há estrelas no céu, refleti-las. E se os céus se pejam de nuvens, como o rio as nuvens são água, refleti-las também sem mágoa, nas profundidades tranqüilas. Manuel Bandeira (Estrela da vida inteira) Agradecimentos gradeço a mim mesma por ter tido coragem de levar adiante os sonhos de A Deus edoprofessor Renan em minha vida, e, por sonharem comigo, agradeço a ambos; a Deus, por tudo, inclusive pela fé que me faz agradecer a Ele antes de a qualquer um outro. Ao prof. Renan, pela paternidade científica e pelos bons vinhos. Aos professores Marizaldo Ludovico e João Manoel sou imensamente grata. -
Improved Orbital Parameters and Photometry
The Astrophysical Journal, 743:162 (8pp), 2011 December 20 doi:10.1088/0004-637X/743/2/162 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. A SEARCH FOR THE TRANSIT OF HD 168443b: IMPROVED ORBITAL PARAMETERS AND PHOTOMETRY Genady Pilyavsky1, Suvrath Mahadevan1,2, Stephen R. Kane3, Andrew W. Howard4,5, David R. Ciardi3, Chris de Pree6, Diana Dragomir3,7, Debra Fischer8, Gregory W. Henry9,EricL.N.Jensen10, Gregory Laughlin11, Hannah Marlowe6, Markus Rabus12, Kaspar von Braun3, Jason T. Wright1,2, and Xuesong X. Wang1 1 Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA; [email protected] 2 Center for Exoplanets & Habitable Worlds, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA; [email protected] 3 NASA Exoplanet Science Institute, Caltech, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USA 4 Department of Astronomy, University of California, Berkeley, CA 94720, USA 5 Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA 6 Department of Physics and Astronomy, Agnes Scott College, 141 East College Avenue, Decatur, GA 30030, USA 7 Department of Physics & Astronomy, University of British Columbia, Vancouver, BC V6T1Z1, Canada 8 Department of Astronomy, Yale University, New Haven, CT 06511, USA 9 Center of Excellence in Information Systems, Tennessee State University, 3500 John A. Merritt Blvd., Box 9501, Nashville, TN 37209, USA 10 Department of Physics & Astronomy, Swarthmore College, Swarthmore, PA 19081, USA 11 UCO/Lick Observatory, University of California, Santa Cruz, CA 95064, USA 12 Departamento de Astonom´ıa y Astrof´ısica, Pontificia Universidad Catolica´ de Chile, Casilla 306, Santiago 22, Chile Received 2011 July 14; accepted 2011 September 21; published 2011 December 2 ABSTRACT The discovery of transiting planets around bright stars holds the potential to greatly enhance our understanding of planetary atmospheres. -
Quantization of Planetary Systems and Its Dependency on Stellar Rotation Jean-Paul A
Quantization of Planetary Systems and its Dependency on Stellar Rotation Jean-Paul A. Zoghbi∗ ABSTRACT With the discovery of now more than 500 exoplanets, we present a statistical analysis of the planetary orbital periods and their relationship to the rotation periods of their parent stars. We test whether the structure of planetary orbits, i.e. planetary angular momentum and orbital periods are ‘quantized’ in integer or half-integer multiples with respect to the parent stars’ rotation period. The Solar System is first shown to exhibit quantized planetary orbits that correlate with the Sun’s rotation period. The analysis is then expanded over 443 exoplanets to statistically validate this quantization and its association with stellar rotation. The results imply that the exoplanetary orbital periods are highly correlated with the parent star’s rotation periods and follow a discrete half-integer relationship with orbital ranks n=0.5, 1.0, 1.5, 2.0, 2.5, etc. The probability of obtaining these results by pure chance is p<0.024. We discuss various mechanisms that could justify this planetary quantization, such as the hybrid gravitational instability models of planet formation, along with possible physical mechanisms such as inner discs magnetospheric truncation, tidal dissipation, and resonance trapping. In conclusion, we statistically demonstrate that a quantized orbital structure should emerge naturally from the formation processes of planetary systems and that this orbital quantization is highly dependent on the parent stars rotation periods. Key words: planetary systems: formation – star: rotation – solar system: formation 1. INTRODUCTION The discovery of now more than 500 exoplanets has provided the opportunity to study the various properties of planetary systems and has considerably advanced our understanding of planetary formation processes. -
Recherche De Compagnons De Faible Masse Par Optique Adaptative Guillaume Montagnier
Recherche de compagnons de faible masse par Optique Adaptative Guillaume Montagnier To cite this version: Guillaume Montagnier. Recherche de compagnons de faible masse par Optique Adaptative. Astro- physique stellaire et solaire [astro-ph.SR]. Université Joseph-Fourier - Grenoble I, 2008. Français. tel-00714874 HAL Id: tel-00714874 https://tel.archives-ouvertes.fr/tel-00714874 Submitted on 5 Jul 2012 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. LABORATOIRE D’ASTROPHYSIQUE DEPARTEMENT´ D’ASTRONOMIE OBSERVATOIRE DE GRENOBLE FACULTE´ DES SCIENCES UJF/CNRS en cotutelle avec UNIVERSITE´ DE GENEVE` Dr. Jean-Luc Beuzit Pr. Stephane´ Udry Dr. Damien Segransan´ Recherche de compagnons de faible masse Par Optique Adaptative THESE` present´ ee´ par Guillaume MONTAGNIER (Grenoble, France) le 18 decembre´ 2008 pour obtenir le titre de : DOCTEUR DE L’UNIVERSITE´ JOSEPH FOURIER Discipline : ASTROPHYSIQUE ET MILIEUX DILUES´ DOCTEUR ES` SCIENCES, UNIVERSITE´ DE GENEVE` Mention : ASTRONOMIE ET ASTROPHYSIQUE COMPOSITION DU JURY : Dr. Jerome´ BOUVIER President´ Pr. Rene´ DOYON Rapporteur Pr. Eduardo MART´IN Rapporteur Dr. Jean-Luc BEUZIT Directeur de these` Pr. Stephane´ UDRY Directeur de these` Dr. Damien SEGRANSAN´ Co-directeur de these` 2008 Table des matieres` 1 Recherche de compagnons de faible masse 5 1.1 Questions astrophysiques .