Is the Sun a Random Star?
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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, -
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. -
AGA5802 High Resolution Spectroscopy: Echelle • Echelle Spectrographs • Applications
AGA5802 High resolution spectroscopy: echelle • Echelle spectrographs • Applications Bibliography: To Measure the Sky, Kitchin, Lena and others ... Prof. Jorge Meléndez 1 How to achieve a high spectral resolution (high dispersion) using a grating 1. Use a grating of higher resolution (>> 1000 lines/mm) or increase fCOL 2. Work at high order m echelle s 2 High resolution 1: grating with many lines/mm + increase fCOL grating Slit Collimator Problem : small spectral coverage © Roy & Clarke 3 High resolution 1: grating with many lines/mm + increase fCOL Exemplo: espectrógrafo Coudé OPD (LNA) R (600nm) Å 12 000 1130 353 30 000 997 27 000 221 50 000 563 25 000 91 120 000 4 Comparison : Echelle HIRES coverage 4000Å ou 40 times High resolution 2: echelle spectrograph © Kitchin Echelle grating • Blazing angle is increased to optimize the observation of high orders (m ~ 30-150) better resolution • Typical grating 31 lines/mm • Problem: order overlapping? 5 Solution for mixing of the orders: cross disperser (prism or grating) cross disperser (grating or prism) CCD6 Example : HIRES spectrograph at KECK Cross disperser could be a grating or a prism; useful to split the orders 7 Echelle orders 8 Echelle orders : extracted 9 Echelle spectrographs Cross-disperser: can we use a prism instead of a grating? 10 2017-05-03 s 2017-05-03 11 Musicos: echelle grating + prism(s) 12 MUSICOS at Pic de Château-Renard http://www.astrosurf.com/thizy/musicos/musicos.htm 13 MUSICOS: blue setup MUSICOS: red setup 14 http://www.lna.br/opd/instrum/musicos.html Blue: 3800 -
A Photometric and Spectroscopic Survey of Solar Twin Stars Within 50
Astronomy & Astrophysics manuscript no. Porto-de-Mello-et-al-Solar-Twin-Survey˙PREPRINT c ESO 2018 July 7, 2018 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. da Silva1,⋆, L. da Silva2 and R. V. de Nader1,⋆⋆ 1 Universidade Federal do Rio de Janeiro, Observat´orio do Valongo, Ladeira do Pedro Antonio 43, CEP: 20080-090 Rio de Janeiro, RJ, Brazil e-mail: [email protected],[email protected],[email protected] 2 Observat´orio Nacional, Rua Gen. Jos´eCristino 77, CEP: 20921-400, Rio de Janeiro, Brazil e-mail: [email protected] Received; accepted 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. -
Systematic Investigation of Chemical Abundances Derived Using IR Spectra Obtained with GIANO E
Systematic investigation of chemical abundances derived using IR spectra obtained with GIANO E. Caffau, P. Bonifacio, E. Oliva, S. Korotin, L. Capitanio, S. Andrievsky, R. Collet, L. Sbordone, S. Duffau, N. Sanna, et al. To cite this version: E. Caffau, P. Bonifacio, E. Oliva, S. Korotin, L. Capitanio, et al.. Systematic investigation of chemical abundances derived using IR spectra obtained with GIANO. Astronomy and Astrophysics - A&A, EDP Sciences, 2019, 622, pp.A68. 10.1051/0004-6361/201834318. hal-02104740 HAL Id: hal-02104740 https://hal.archives-ouvertes.fr/hal-02104740 Submitted on 24 Nov 2020 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 622, A68 (2019) Astronomy https://doi.org/10.1051/0004-6361/201834318 & © ESO 2019 Astrophysics Systematic investigation of chemical abundances derived using IR spectra obtained with GIANO? E. Caffau1, P. Bonifacio1, E. Oliva2, S. Korotin3, L. Capitanio1, S. Andrievsky4,1, R. Collet5, L. Sbordone6, S. Duffau7, N. Sanna2, A. Tozzi2, L. Origlia8, N. Ryde9, and H.-G. Ludwig10,1 1 GEPI, Observatoire de Paris, Université PSL, CNRS, 5 Place Jules Janssen, 92190 Meudon, France e-mail: [email protected] 2 INAF, Osservatorio Astrofisico di Arcetri, Largo E. -
Arxiv:1207.6212V2 [Astro-Ph.GA] 1 Aug 2012
Draft: Submitted to ApJ Supp. A Preprint typeset using LTEX style emulateapj v. 5/2/11 PRECISE RADIAL VELOCITIES OF 2046 NEARBY FGKM STARS AND 131 STANDARDS1 Carly Chubak2, Geoffrey W. Marcy2, Debra A. Fischer5, Andrew W. Howard2,3, Howard Isaacson2, John Asher Johnson4, Jason T. Wright6,7 (Received; Accepted) Draft: Submitted to ApJ Supp. ABSTRACT We present radial velocities with an accuracy of 0.1 km s−1 for 2046 stars of spectral type F,G,K, and M, based on ∼29000 spectra taken with the Keck I telescope. We also present 131 FGKM standard stars, all of which exhibit constant radial velocity for at least 10 years, with an RMS less than 0.03 km s−1. All velocities are measured relative to the solar system barycenter. Spectra of the Sun and of asteroids pin the zero-point of our velocities, yielding a velocity accuracy of 0.01 km s−1for G2V stars. This velocity zero-point agrees within 0.01 km s−1 with the zero-points carefully determined by Nidever et al. (2002) and Latham et al. (2002). For reference we compute the differences in velocity zero-points between our velocities and standard stars of the IAU, the Harvard-Smithsonian Center for Astrophysics, and l’Observatoire de Geneve, finding agreement with all of them at the level of 0.1 km s−1. But our radial velocities (and those of all other groups) contain no corrections for convective blueshift or gravitational redshifts (except for G2V stars), leaving them vulnerable to systematic errors of ∼0.2 km s−1 for K dwarfs and ∼0.3 km s−1 for M dwarfs due to subphotospheric convection, for which we offer velocity corrections. -
Cal. Legacy Survey I
The Astrophysical Journal Supplement Series, 255:8 (67pp), 2021 July https://doi.org/10.3847/1538-4365/abe23c © 2021. The American Astronomical Society. All rights reserved. The California Legacy Survey. I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal1 , Benjamin J. Fulton1,2 , Lea A. Hirsch3 , Howard T. Isaacson4 , Andrew W. Howard1 , Cayla M. Dedrick1,5 , Ilya A. Sherstyuk1, Sarah C. Blunt1,18 , Erik A. Petigura6 , Heather A. Knutson7 , Aida Behmard7,18 , Ashley Chontos8,18 , Justin R. Crepp9 , Ian J. M. Crossfield10, Paul A. Dalba11,19 , Debra A. Fischer12 , Gregory W. Henry13 , Stephen R. Kane11 , Molly Kosiarek14,18 , Geoffrey W. Marcy4 , Ryan A. Rubenzahl1,18 , Lauren M. Weiss8 , and Jason T. Wright15,16,17 1 Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2 IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3 Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4 Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5 Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 6 Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 7 Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 8 Institute for Astronomy, University of Hawaii, Honolulu, HI 96822, -
Astrophysics in 2006
Space Sci Rev (2007) 132: 1–182 DOI 10.1007/s11214-007-9224-0 Astrophysics in 2006 Virginia Trimble · Markus J. Aschwanden · Carl J. Hansen Received: 11 May 2007 / Accepted: 24 May 2007 / Published online: 23 October 2007 © Springer Science+Business Media B.V. 2007 Abstract The fastest pulsar and the slowest nova; the oldest galaxies and the youngest stars; the weirdest life forms and the commonest dwarfs; the highest energy particles and the lowest energy photons. These were some of the extremes of Astrophysics 2006. We attempt also to bring you updates on things of which there is currently only one (habitable planets, the Sun, and the Universe) and others of which there are always many, like meteors and molecules, black holes and binaries. Keywords Cosmology: general · Galaxies: general · ISM: general · Stars: general · Sun: general · Planets and satellites: general · Astrobiology · Star clusters · Binary stars · Clusters of galaxies · Gamma-ray bursts · Milky Way · Earth · Active galaxies · Supernovae 1 Introduction Astrophysics in 2006 modifies a long tradition by moving to a new journal, which you hold in your (real or virtual) hands. The fifteen previous articles in the series are referenced oc- casionally as Ap91 to Ap05 below and appeared in volumes 104–118 of Publications of V. Trimble Department of Physics and Astronomy, University of California, Irvine, CA 92697-4575, USA e-mail: [email protected] V. Trimble Las Cumbres Observatory, Santa Barbara, CA, USA M.J. Aschwanden () Lockheed Martin Advanced Technology Center, Solar and Astrophysics Laboratory, Organization ADBS, Building 252, 3251 Hanover Street, Palo Alto, CA 94304, USA e-mail: [email protected] C.J. -
Análise Da Composiç˜Ao Qu´Imica Das Gêmeas Solares HIP 100963, HD
Universidade de S~aoPaulo Instituto de Astronomia, Geof´ısicae Ci^enciasAtmosf´ericas Departamento de Astronomia Jhon Yana Galarza An´alise da composi¸c~aoqu´ımicadas g^emeas solares HIP 100963, HD 45184 e a descoberta da g^emeasolar Inti 1 S~aoPaulo 2016 Jhon Yana Galarza An´alise da composi¸c~aoqu´ımicadas g^emeas solares HIP 100963, HD 45184 e a descoberta da g^emeasolar Inti 1 Disserta¸c~aoapresentada ao Departamento de Astronomia do Instituto de Astronomia, Geof´ısica e Ci^enciasAtmosf´ericasda Universidade de S~aoPaulo como requisito parcial para a ob- ten¸c~aodo t´ıtulode Mestre em Ci^encias. Vers~aoCorrigida. O original encontra- se dispon´ıvel na Unidade Area´ de Concentra¸c~ao:Astronomia Orientador: Prof. Dr. Jorge Mel´endez S~aoPaulo 2016 Dedico este trabalho `aminha professora, orientadora e amiga Mar´ıaLuisa Aguilar Hurtado, quem foi a primeira astro^noma do Peru. Agradecimentos A` minha querida fam´ılia: Aurelio Yana, Ines Galarza e Luis Yana Galarza, pelo seu apoio, assist^enciae carinho ao longo dos anos sem os quais a realiza¸c~aodesta disserta¸c~ao teria sido imposs´ıvel. A` minha noiva Cecilia Toledo, pela companhia de todos os dias, pelo apoio nos momen- tos mais dif´ıceise tamb´empelos bons momentos que ajudaram ao sucesso deste trabalho. Ao meu orientador Dr. Jorge Mel´endez,pela orienta¸c~ao,paci^encia,prestatividade e as in´umerasoportunidades que me deu, permitindo a minha forma¸c~aocient´ıfica. Aos meus colegas do grupo SAMPA: Leonardo dos Santos, Mar´ıliaCarlos, Henrique Reggiani, Lorenzo Spina e Marcelo Tucci, pelas importantes discuss~oesastrof´ısicasque contribu´ıramao desenvolvimento desta disserta¸c~ao. -
Planet Signatures and Effect of the Chemical Evolution of the Galactic Thin-Disk Stars
A&A 585, A152 (2016) Astronomy DOI: 10.1051/0004-6361/201527429 & c ESO 2016 Astrophysics Planet signatures and effect of the chemical evolution of the Galactic thin-disk stars Lorenzo Spina1, Jorge Meléndez1, and Ivan Ramírez2 1 Universidade de São Paulo, IAG, Departamento de Astronomia, Rua do Mãtao 1226, São Paulo, 05509-900 SP, Brasil e-mail: [email protected] 2 Department of Astronomy, University of Texas at Austin; 2515 Speedway, Stop C1400, Austin, TX 78712-1205, USA Received 23 September 2015 / Accepted 19 October 2015 ABSTRACT Context. Studies based on high-precision abundance determinations revealed that chemical patterns of solar twins are characterised by the correlation between the differential abundances relative to the Sun and the condensation temperatures (Tc) of the elements. It has been suggested that the origin of this relation is related to the chemical evolution of the Galactic disk, but other processes, associated with the presence of planets around stars, might also be involved. Aims. We analyse HIRES spectra of 14 solar twins and the Sun to provide new insights on the mechanisms that can determine the relation between [X/H] and Tc. Methods. Our spectroscopic analysis produced stellar parameters (Teff,log g,[Fe/H], and ξ), ages, masses, and abundances of 22 ele- ments (C, O, Na, Mg, Al, Si, S, K, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Sr, Y, and Ba). We used these determinations to place new constraints on the chemical evolution of the Galactic disk and to verify whether this process alone can explain the different [X/H]-Tc slopes observed so far. -
Proje Sonuç Raporu
T.C. ERCİYES ÜNİVERSİTESİ BİLİMSEL ARAŞTIRMA PROJELERİ KOORDİNASYON BİRİMİ OB BİLEŞENLİ ERKEN TÜR ÇİFT YILDIZLARIN IŞIK EĞRİSİ ANALİZİ VE FİZİKSEL PARAMETRELERİNİN BELİRLENMESİ Proje No: FBA-09-788 Normal Araştırma Projesi (NAP) SONUÇ RAPORU Proje Yürütücüsü: Doç.Dr. Mehmet TANRIVER Fen Fakültesi / Astronomi ve Uzay Bilimleri Bölümü Yrd.Doç.Dr. Hasan AK Fen Fakültesi / Astronomi ve Uzay Bilimleri Bölümü Yrd.Doç.Dr. Nurten FİLİZ AK Fen Fakültesi / Astronomi ve Uzay Bilimleri Bölümü Yrd.Doç.Dr. İnci AKKAYA ORALHAN Fen Fakültesi / Astronomi ve Uzay Bilimleri Bölümü Yrd.Doç.Dr. Mikail SARIKAYA Kurum Dışı Ocak 2017 KAYSERİ TEŞEKKÜR “OB BİLEŞENLİ ERKEN TÜR ÇİFT YILDIZLARIN IŞIK EĞRİSİ ANALİZİ VE FİZİKSEL PARAMETRELERİNİN BELİRLENMESİ” başlıklı FBA-09-788 numaralı Normal Araştırma Projesi (NAP) Erciyes Üniversitesi Bilimsel Araştırma Projeleri Birimi tarafından desteklenmiştir. İÇİNDEKİLER Sayfa No ÖZET 5 ABSTRACT 6 1. GİRİŞ / GENEL BİLGİLER 7 2. GEREÇ VE YÖNTEM 11 3. BULGULAR 15 4. TARTIŞMA VE SONUÇ 16 5. KAYNAKLAR 17 6. EKLER 23 EK.1. 23 EK.2. 39 EK.3. 40 EK.4. 41 EK.5. 42 EK.6. 43 EK.7. 44 OB BİLEŞENLİ ERKEN TÜR ÇİFT YILDIZLARIN IŞIK EĞRİSİ ANALİZİ VE FİZİKSEL PARAMETRELERİNİN BELİRLENMESİ ÖZET OB yıldızları yaydıkları güçlü ışınım enerjisi ve rüzgarla galaksinin kimyasal evrimini ve dinamiğini etkiler. Kataloglarda 300 kadar büyük kütleli OB yıldızı, etkileşen çift yıldız bileşeni durumundadır. OB bileşenli çift yıldız sistemlerinde ışık eğrisini bozan çevresel etkiler vardır. Bu çevresel etkiler ışık eğrisinde kendini minimumlarda asimetri ve minimum genişliklerinin eşit olmaması şeklinde gösterir. Bu tür sistemlerde (değen ve yarı-değen türlerde) aşırı kütle kaybı ve izotropik olmayan yıldız rüzgarı ile sistemi terkeden madde, sistem etrafında homojen olmayan birikim bölgeleri, sistemi saran bir zarf oluşturur. -
Proceedings of the 6Th Australian Space Science Conference Canberra 19-21 July, 2006
Proceedings of the 6th Australian Space Science Conference Canberra 19-21 July, 2006 Australian Space Science Conference Series 1st Edition Published in Australia in 2007 by National Space Society of Australia Ltd GPO Box 7048 Sydney NSW 2001 Fax: 61 (02) 9988-0262 email: [email protected] website: http://www.nssa.com.au Copyright © 2007 National Space Society of Australia Ltd All rights reserved. No part of this publication may be reproduced, stored in a retrieval system or transmitted in any form or by any means, electronic, mechanical, photocopying, recording or otherwise, without prior permission from the publisher. ISBN 13: 978-0-9775740-0-1 Editor: Wayne Short Distributed on CD-Rom Proceedings of the 6th Australian Space Science Conference, 2006 Page i Page ii Proceedings of the 6th Australian Space Science Conference, 2006 Preface A large number of the presenters at the conference later submitted completed academic papers which form the basis of the conference proceedings. All papers published in these proceedings, have been subject to a peer review process whereby a scholarly judgement by suitable individuals determined if the paper was suitable to be published. In some cases, paper not initially accepted were revised until deemed suitable. The editor would like to give special thanks to those scholars who participated in the peer review process. Finally I would like to thank our sponsors for their support and the Organising Committee for giving generously of their time and efforts. We trust that you will find the 2006 Conference Proceedings enjoyable and informative. Responsibility for the content of each paper lies with its author(s).