A Photometric and Spectroscopic Survey of Solar Twin Stars Within 50 Parsecs of the Sun I
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Non-Collider Searches for Stable Massive Particles
Non-collider searches for stable massive particles S. Burdina, M. Fairbairnb, P. Mermodc,, D. Milsteadd, J. Pinfolde, T. Sloanf, W. Taylorg aDepartment of Physics, University of Liverpool, Liverpool L69 7ZE, UK bDepartment of Physics, King's College London, London WC2R 2LS, UK cParticle Physics department, University of Geneva, 1211 Geneva 4, Switzerland dDepartment of Physics, Stockholm University, 106 91 Stockholm, Sweden ePhysics Department, University of Alberta, Edmonton, Alberta, Canada T6G 0V1 fDepartment of Physics, Lancaster University, Lancaster LA1 4YB, UK gDepartment of Physics and Astronomy, York University, Toronto, ON, Canada M3J 1P3 Abstract The theoretical motivation for exotic stable massive particles (SMPs) and the results of SMP searches at non-collider facilities are reviewed. SMPs are defined such that they would be suffi- ciently long-lived so as to still exist in the cosmos either as Big Bang relics or secondary collision products, and sufficiently massive such that they are typically beyond the reach of any conceiv- able accelerator-based experiment. The discovery of SMPs would address a number of important questions in modern physics, such as the origin and composition of dark matter and the unifi- cation of the fundamental forces. This review outlines the scenarios predicting SMPs and the techniques used at non-collider experiments to look for SMPs in cosmic rays and bound in mat- ter. The limits so far obtained on the fluxes and matter densities of SMPs which possess various detection-relevant properties such as electric and magnetic charge are given. Contents 1 Introduction 4 2 Theory and cosmology of various kinds of SMPs 4 2.1 New particle states (elementary or composite) . -
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. -
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. -
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). -
[Astro-Ph.GA] 15 Oct 2015 Nt Eatooi,Gosc Inisamseia,Uni Atmosfericas, Ciencias E Geofisica Astronomia, De Inst
Submitted to Astrophysical Journal June 24, 2015 Charting the Interstellar Magnetic Field causing the Interstellar Boundary Explorer (IBEX) Ribbon of Energetic Neutral Atoms P. C. Frisch Dept. Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637 A. Berdyugin and V. Piirola Finnish Centre for Astronomy with ESO, University of Turku, Finland A. M. Magalhaes and D. B. Seriacopi Inst. de Astronomia, Geofisica e Ciencias Atmosfericas, Universidade de Sao Paulo, Brazil S. J. Wiktorowicz Dept. Astronomy, University of California at Santa Cruz, Santa Cruz, CA B-G Andersson SOFIA Science Center, USRA, Moffett Field, CA H. O. Funsten Los Alamos National Laboratory, Los Alamos, NM D. J. McComas1 Southwest Research Institute, San Antonio, TX arXiv:1510.04679v1 [astro-ph.GA] 15 Oct 2015 N. A. Schwadron Space Science Center, University of New Hampshire J. D. Slavin Harvard-Smithsonian Center for Astrophysics, Cambridge, MA A. J. Hanson 1Also University of Texas, San Antonio, TX –2– School of Informatics and Computing, Indiana University, Bloomington, IN C.-W. Fu School of Computer Engineering, Nanyang Technological University, Singapore ABSTRACT The interstellar magnetic field (ISMF) near the heliosphere is a fundamen- tal component of the solar galactic environment that can only be studied using polarized starlight. The results of an ongoing survey of the linear polarizations of local stars are analyzed with the goal of linking the interstellar magnetic field that shapes the heliosphere to the nearby field in interstellar space. We present new results on the direction of the magnetic field within 40 pc obtained from analyzing polarization data using a merit function that determines the field di- rection that provides the best fit to the polarization data. -
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. -
PDF, on the Incidence of Wise Infrared Excess Among Solar
The Astrophysical Journal, 837:15 (11pp), 2017 March 1 doi:10.3847/1538-4357/837/1/15 © 2017. The American Astronomical Society. All rights reserved. On the Incidence of Wise Infrared Excess Among Solar Analog, Twin, and Sibling Stars A. D. Da Costa1, B. L. Canto Martins1, I. C. Leão2, J. E. Lima Jr1, D. Freire da Silva1, D. B. de Freitas3, and J. R. De Medeiros1 1 Departamento de Física Teórica e Experimental, Universidade Federal do Rio Grande do Norte, Campus Universitário, Natal, RN, 59072-970, Brazil; dgerson@fisica.ufrn.br 2 European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany 3 Departamento de Física, Universidade Federal do Ceará, Caixa Postal 6030, Campus do Pici, 60455-900, Fortaleza, Ceará, Brazil Received 2016 April 25; revised 2016 November 3; accepted 2016 November 6; published 2017 February 27 Abstract This study presents a search for infrared (IR) excess in the 3.4, 4.6, 12, and 22 μm bands in a sample of 216 targets, composed of solar sibling, twin, and analog stars observed by the Wide-field Infrared Survey Explorer (WISE) mission. In general, an IR excess suggests the existence of warm dust around a star. We detected 12 μm and/or 22 μm excesses at the 3σ level of confidence in five solar analog stars, corresponding to a frequency of 4.1% of the entire sample of solar analogs analyzed, and in one out of 29 solar sibling candidates, confirming previous studies. The estimation of the dust properties shows that the sources with IR excesses possess circumstellar material with temperatures that, within the uncertainties, are similar to that of the material found in the asteroid belt in our solar system. -
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. -
Arxiv:Astro-Ph/0603770V1 28 Mar 2006
Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Southern Sample R.O. Gray Department of Physics and Astronomy, Appalachian State University, Boone, NC 28608 [email protected] C.J. Corbally Vatican Observatory Research Group, Steward Observatory, Tucson, AZ 85721-0065 [email protected] R.F. Garrison David Dunlap Observatory, P.O. Box 360, Station A, Richmond Hill, ON L4C 4Y6, Canada [email protected] M.T. McFadden, E.J. Bubar1 and C.E. McGahee Department of Physics and Astronomy, Appalachian State University, Boone, NC 28608 A.A. O’Donoghue and E.R. Knox Dept of Physics, St. Lawrence University, Canton, NY 13617 ABSTRACT We are obtaining spectra, spectral types and basic physical parameters for the nearly 3600 dwarf and giant stars earlier than M0 in the Hipparcos catalog within 40pc of the Sun. Here we report on results for 1676 stars in the southern hemisphere observed at Cerro Tololo Interamer- arXiv:astro-ph/0603770v1 28 Mar 2006 ican Observatory and Steward Observatory. These results include new, precise, homogeneous spectral types, basic physical parameters (including the effective temperature, surface gravity, and metallicity, [M/H]) and measures of the chromospheric activity of our program stars. We include notes on astrophysically interesting stars in this sample, the metallicity distribution of the solar neighborhood and a table of solar analogues. We also demonstrate that the bimodal ′ nature of the distribution of the chromospheric activity parameter log RHK depends strongly on the metallicity, and we explore the nature of the “low-metallicity” chromospherically active K-type dwarfs. -
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. -
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.