Alberto Buzzoni Incarico Professionale Per Prestazione Di Collaborazione

Total Page:16

File Type:pdf, Size:1020Kb

Alberto Buzzoni Incarico Professionale Per Prestazione Di Collaborazione Curriculum Vitae Alberto Buzzoni PERSONAL INFORMATION Alberto Buzzoni Viale Cavour 142, 44121 Ferrara (Fe) +39 051 6357322 [email protected] http://www.bo.astro.it/~eps/home.html Skype: [email protected] Sex Male | Date of birth 04/11/1958 | Nationality Italian Incarico professionale per prestazione di collaborazione occasionale POSITION con l’Osservatorio Astronomico della Regione Autonoma della Valle d’Aosta WORK EXPERIENCE 2004 - present Senior Associate Astronomer INAF – Osservatorio Astronomico di Bologna - Via Gobetti 93/3 40129 Bologna ▪ INAF National Representative in the Steering Committee of OCIS, the national government entity for coordination of Space Surveillance & Defense activities (since 2017) ▪ INAF official Representative, on behalf of the President, at the “Space Weather Initiative” of the Italian Embassy of Washington (USA, 2017) ▪ Professor in charge (Professore incaricato) at UNIBO, teaching the course of “Spectral Evolution of Galaxies” (since 2006). Advisor of 19 MSc and PhD theses in Astrophysics and Cosmology. ▪ National PI of a PRIN/INAF (2005/07). ▪ Visiting professor at the Universidad Nacional de La Plata (Argentina), ESO HQ in Santiago de Chile (Chile) (2008) and MIAPP (Munich, Germany) (2018) ▪ Invited professor at the National PhD School of Astrophysics (2008), at the 3rd SAIt/MIUR Youth Summer School (2013) and at the Youth Olympics of Astronomy (since 2010) ▪ Scientific Advisor of Space TV Broadcasting on Space Science themes (since 2013) ▪ SOC member of three international conferences. ▪ Member of the Project Office of “PRISMA” (Prima Rete Italiana per la Sorveglianza sistematica di Meteore ed Alta Atmosfera) (since 2016) ▪ Member of the INAOE International Advisory Committee, Mexico (2004/11) ▪ Coordinator of the Selection Committee for the National Prize “Giampietro Puppi”, awarded to the best PhD thesis in Physics and Astrophysics in Italy (2010) ▪ Member of the Selection Committee for a position of Primo Ricercatore INAF, Bologna (2008), and for the international “Cassini” Fellowship in Astrophysics (2016) ▪ Scientific Evaluator for CONACyT (Mexico), CONICET (Argentina) and NCN (Poland) ▪ Horizon 2020 and EACEA/Erasmus Expert for the European Commission Framework Programme for Research and Innovation (Expert ID: EX2006C147586) Sector Public Research Institution 2000 - 2003 Resident Senior Associate Astronomer TNG – Telescopio Nazionale Galileo, La Palma (Canary Islands, Spain) ▪ Management of scientific and logistic activity at the TNG, with the function of Deputy Director. I dealt with the hosting Spanish Institutions at La Palma and took in charge the institutional duties as official representative of the Director, including the contacts with the media (press and TV) to promote the TNG activity. ▪ Scientific Evaluator of CNAA/INAF research programmes ▪ SOC and LOC member of two international conferences and scientific editor of the proceedings ▪ Advisor of 2 MSc and PhD theses in Astrophysics and Cosmology (Mexico and Milano) © European Union, 2002-2015 | europass.cedefop.europa.eu Page 1 / 8 Curriculum Vitae Alberto Buzzoni Sector Public Research Institution 1996 - 1999 Associate Astronomer INAF – Osservatorio Astronomico di Brera – Via Brera 28, 20121 Milano ▪ Research activity on Astrophysics at international level. Several academic/research visits at international institutes, mostly in Europe and Latin America ▪ IAU Membership joining Divisions G (Stars and Stellar Physics), H (Interstellar Matter and Local Universe), J (Galaxies and Cosmology), and Comm. 37 (Star Clusters and Associations) (since 1997) ▪ Responsible for the Milan-Mexico collaboration in the framework of the Scientific and Technical Agreement signed between the Brera Observatory and the UNAM Mexico. ▪ SOC Co-chairman of two international conferences and scientific editor of the proceedings ▪ Scientific Evaluator of CNAA/INAF research programmes ▪ Invited professor at two National PhD Schools of Astrophysics in Italy ▪ Advisor of 3 MSc and PhD theses in Astrophysics, Cosmology and Philosophy of Science (Bologna, Napoli, Mexico) ▪ Responsible for the Workplace Safety Service of the Brera Astronomical Observatory Sector Public Research Institution 1986 - 1995 Research Astronomer INAF – Osservatorio Astronomico di Brera – Via Brera 28, 20121 Milano ▪ Research activity on Astrophysics at international level. ▪ Visiting scientist at the Instituto Nacional de Astrofisica, Optica y Electronica (INAOE) of Puebla (Mexico) (1993/95) ▪ Member of the CONACyT Evaluation Committee for the Large National Project of Science and Technology “TIM: the New 6.5m Infrared Mexican Telescope” (Mexico) (1994) ▪ Principal investigator of two CONACyT Research Programmes (Mexico) ▪ ASTRONET National Computer Network for Astronomy: member of the Italian User Committee ▪ Adjunct Professor at Università Statale di Milano (Laurea career in Physics) (1986/92) ▪ Advisor of 5 MSc and PhD theses in Astrophysics, Cosmology (Milano) ▪ Member of the Italian Astronomical Society (since 1985) Sector Public Research Institution EDUCATION AND TRAINING 1978 - 1982 Doctoral Laurea in Astronomy (Laurea quadriennale) 8 Università di Bologna, Facoltà di Scienze MM FF NN – Grade: Summa cum Laude ▪ Thesis Defense on “Calculation procedures for stellar population synthesis” 1972 - 1977 High-school degree in Science 4 Liceo Scientifico “A. Roiti”, Ferrara PERSONAL SKILLS Mother tongue(s) Italian Other language(s) UNDERSTANDING SPEAKING WRITING Listening Reading Spoken interaction Spoken production English C1 C2 C1 C2 C2 Spanish C2 C2 C2 C2 C2 © European Union, 2002-2015 | europass.cedefop.europa.eu Page 2 / 8 Curriculum Vitae Alberto Buzzoni French C2 C2 B2 B2 B2 German A2 A2 A2 A2 A2 Levels: A1/A2: Basic user - B1/B2: Independent user - C1/C2 Proficient user Common European Framework of Reference for Languages © European Union, 2002-2015 | europass.cedefop.europa.eu Page 3 / 8 Curriculum Vitae Alberto Buzzoni Scientific Achievements My research fields mainly deal with the study of spectrophotometric evolution of galaxies and other stellar systems in the local and deep Universe, aiming at probing the distinctive evolutionary properties of stellar populations along the different cosmic epochs and aggregation scales in the Universe. This work is carried out both from the theoretical and experimental point of view, relying on spectrophotometric modelling of stellar populations and on observing programs at the major available telescopes, from ground and space. Theoretical research: I'm the author of an original code for stellar population synthesis (1989; ~230 citations), whose results have been extensively used by the international astronomical community. In collaboration with A. Renzini, I also discovered the so-called "Fuel Consumption Theorem" (1986; ~380 citations), internationally recognized as a seminal contribution in the theory of stellar populations, leading to important applications to the observation of local and extragalactic stellar aggregates. Synthesis models have been continually updated along the years, to better assess elliptical galaxy evolution (1995; ~110 citations), and chemo-photometric evolution (2002, 2005 and 2011) of galaxies along the whole Hubble morphological sequence (over 350 downloads/year of the data sets over the Web). On this line, in collaboration with Mexican colleagues of the INAOE (namely M. Chavez, E. Bertone and L.H. Rodriguez-Merino) I’ve also being working on stellar model atmospheres producing two extended libraries of high-resolution (up to R=500,000) synthetic spectra of stars, named UVBLUE (2005) and BLUERED (2004), both based on the Kurucz ATLAS code. These libraries stand out in the current literature as widely recognized references for spectral synthesis of distant galaxies and for abundance studies of single stars (about 100 downloads/year of the data sets over the Web). Experimental research: My work of 1983 on the so-called R-method (in collaboration with R. Buonanno, C. Corsi and F. Fusi Pecci), provided a yet fully original estimate of the primordial Helium abundance in the Universe, a result still so widely accounted in the current literature (~270 citations) on cosmic nucleosynthesis and stellar evolution theory. In a series of papers of 2006-08, the collaboration with M. Arnaboldi, R. Corradi and R.A. Gonzalez-Lopezlira led me to tackle the role of planetary nebulae in the more general framework of galaxy evolution. From one hand, these results proved to be of special relevance to properly assess the so-called “UV upturn” phenomenon of elliptical galaxies; on the other hand, a cutting-edge application to the study of galaxy clusters was also envisaged using extragalactic planetary nebulae as effective tracers to probe the diffuse intra-cluster luminosity. In the extragalactic field, between years 1989-96 I’ve been actively involved in the study of high- redshift galaxy clusters, in collaboration with G. Chincarini, E. Molinari, and other colleagues at the Brera Observatory. To some extent, this work in the early 90’s pioneered the current popular “photometric redshift” techniques, to constrain redshift of distant galaxies from the match of multicolour photometry with population synthesis models. On a more local extragalactic context, first in collaboration with L. Carrasco and other colleagues at the INAOE (Mexico), and then with J.C. Forte, S. Cellone and their group at the La Plata University (Argentina), I've also been working on spectrophotometric classification of galaxies
Recommended publications
  • 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.
    [Show full text]
  • SILICON and OXYGEN ABUNDANCES in PLANET-HOST STARS Erik Brugamyer, Sarah E
    The Astrophysical Journal, 738:97 (11pp), 2011 September 1 doi:10.1088/0004-637X/738/1/97 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. SILICON AND OXYGEN ABUNDANCES IN PLANET-HOST STARS Erik Brugamyer, Sarah E. Dodson-Robinson, William D. Cochran, and Christopher Sneden Department of Astronomy and McDonald Observatory, University of Texas at Austin, 1 University Station C1400, Austin, TX 78712, USA; [email protected] Received 2011 February 4; accepted 2011 June 22; published 2011 August 16 ABSTRACT The positive correlation between planet detection rate and host star iron abundance lends strong support to the core accretion theory of planet formation. However, iron is not the most significant mass contributor to the cores of giant planets. Since giant planet cores are thought to grow from silicate grains with icy mantles, the likelihood of gas giant formation should depend heavily on the oxygen and silicon abundance of the planet formation environment. Here we compare the silicon and oxygen abundances of a set of 76 planet hosts and a control sample of 80 metal-rich stars without any known giant planets. Our new, independent analysis was conducted using high resolution, high signal-to-noise data obtained at McDonald Observatory. Because we do not wish to simply reproduce the known planet–metallicity correlation, we have devised a statistical method for matching the underlying [Fe/H] distributions of our two sets of stars. We find a 99% probability that planet detection rate depends on the silicon abundance of the host star, over and above the observed planet–metallicity correlation.
    [Show full text]
  • Chemical Abundance Study of Planetary Hosting Stars P
    CHEMICAL ABUNDANCE STUDY OF PLANETARY HOSTING STARS P. Rittipruk and Y. W. Kang Department of Astronomy and Space Science Sejong University, Korea Planetary Hosting Stars Metallicity ∝ Probability of Hosting Planets Planetary Hosting Stars Planetary Hosting Stars 0.8 0.6 with planet 0.4 without planet 0.2 0.0 -0.2 -0.4 -0.6 Corr-Coef of [X/H] vs EP -0.8 -1.0 -1.5 -1.0 -0.5 0.0 0.5 1.0 [M/H] Chemical abundances of 1111 FGK stars (Adibekyan et al, 2012) 1.2 c 0.8 0.4 0.0 -0.4 -0.8 Corr-Coef of [X/H] vs T with planet without planet -1.2 -1.5 -1.0 -0.5 0.0 0.5 1.0 [M/H] Chemical abundances of 1111 FGK stars (Adibekyan et al, 2012) HD 20794 ‘s Planets Earth to Sun = 1 AU Mass = 0.70 Msun Radius = 0.92 Rsun Distance = 6.06 pc Age = 14±6 Gyr (Bernkopf+2012) = 5.76±0.66 (Gyr)(Pepe+ 2011) bcde M sin i 0.0085 0.0076 0.0105 0.0150 (MJ) (2.7) (2.4) (4.8) (4.7) a(AU) 0.1207 0.2036 0.3499 0.509 P(days) 18.315 40.114 90.309 147.2 HD 47536 ‘s Planets ■ Mass = 0.94 Msun Earth to Sun = 1AU ■ Radius = 23.47 Rsun ■ Distance = 121.36 pc ■ Age = 9.33 Gyr (Silva+2006) HD 47536b HD 47536c** M sin i (MJ) 4.96 6.98 a(AU) 1.61 3.72 P(days) 430 2500 Observation CHIRON Echelle Spectrometer Wavelength cover : 4200 – 8800 A Narrow Slit (R = 120,000) SMART-1.5m at CTIO, La Serena, Chile Observed Spectrum Echelle Spectrum of HD20794 obtained using CHIRON Spectrometers Reduced Spectrum Spectrum of HD20794 after reduction plotted with synthesis spectrum Algorithms Rotational Velocity (v sin i) Determination Reiners & Schmitt (2003) ⁄ sin 0.610 0.062 0.027 0.012 0.004
    [Show full text]
  • Doctor of Philosophy
    Study of Sun-like G Stars and Their Exoplanets Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy by Mr. SHASHANKA R. GURUMATH May, 2019 ABSTRACT By employing exoplanetary physical and orbital characteristics, aim of this study is to understand the genesis, dynamics, chemical abundance and magnetic field structure of Sun-like G stars and relationship with their planets. With reasonable constraints on selection of exoplanetary physical characteristics, and by making corrections for stellar rate of mass loss, a power law relationship between initial stellar mass and their exo- planetary mass is obtained that suggests massive stars harbor massive planets. Such a power law relationship is exploited to estimate the initial mass (1.060±0.006) M of the Sun for possible solution of “Faint young Sun paradox” which indeed indicates slightly higher mass compared to present mass. Another unsolved puzzle of solar system is angular momentum problem, viz., compare to Sun most of the angular momentum is concentrated in the solar system planets. By analyzing the exoplanetary data, this study shows that orbital angular momentum of Solar system planets is higher compared to orbital angular momentum of exoplanets. This study also supports the results of Nice and Grand Tack models that propose the idea of outward migration of Jovian planets during early history of Solar system formation. Furthermore, we have examined the influence of stellar metallicity on the host stars mass and exoplanetary physical and orbital characteristics that shows a non-linear relationship. Another important result is most of the planets in single planetary stellar systems are captured from the space and/or inward migration of planets might have played a dominant role in the final architecture of single planetary stellar systems.
    [Show full text]
  • 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.
    [Show full text]
  • Hungarian Academy of Sciences CENTRAL RESEARCH INSTITUTE for PHYSICS
    KFKI 1990 50/C В. LUKÁCS SZ. BÉRCZI I. MOLNÁR G. PAÁL EVOLUTION: FROM COSMOGENESIS TO BIOGENESIS Hungarian Academy of Sciences CENTRAL RESEARCH INSTITUTE FOR PHYSICS BUDAPEST KFKI-1990-50/C PREPRINT EVOLUTION: FROM COSMOGENESIS TO BIOGENESIS B. LUKÁCS. SZ. BÉRCZI, I. MOLNÁR, G. PAÁL (eds.) Central Research institute for Physics H-1526 Budapest 114. P.O.B. 49, Hungary T.F. Farkas: Structures under Crystallization. (1980) The material of the t8 Evolution Symposium of the Evolution of Matter Subcommittee of the Qeonomy Scientific CommiUee of the Hungarian Academy of Science. 28 31 May, 1990. HU ICSN 0368 5330 В. Lukács, Sz. Bérezi. I. Molnár, Q. Paál (eds.): Evolution: from cosmogenesis to biogenesis KFKI 1990 50/C ABSTRACT The Volume contains the material of an interdisciplinary evolution symposium The purpose was to shed some light on possible connections between steps of evolution of matter on different levels of organisation. The topics involved are as follow: cosmogenesis; galactic and stellar evolution, formation and evolution of the solar system; global atmospheric and tectonic changes of Earth; viral evolution; phytogeny and evolution of terrestrial lile; evolution of neural system; hominization The material also includes some discussions of the underlying phenomena and laws of Nature. Б. Лукач, С, Берци, И. Молнар, Г. Паал (ред.): Эволюция от космогенезиса до биогенезиса. KFKI-1990-50/C АННОТАЦИЯ Сборник содержит материалы интердисциплинарного симпозиума по эволюции. Целью симпозиума являлось выяснение связи между шагами эволюции материи на раз­ ных уровнях организации. Были затронуты следующие темы: коемогенеэис, эволюция звезд и Солнечной системы, глобальная тектоника Земли, эволюция атмосферы Земли, эволюция вирусов, филогенезис, эволюция жизни, эволюция нервной системы, гомини- эация, термодинамические аспекты эволюции.
    [Show full text]
  • Determining the True Mass of Radial-Velocity Exoplanets with Gaia 9 Planet Candidates in the Brown-Dwarf/Stellar Regime and 27 Confirmed Planets
    Astronomy & Astrophysics manuscript no. exoplanet_mass_gaia c ESO 2020 September 30, 2020 Determining the true mass of radial-velocity exoplanets with Gaia 9 planet candidates in the brown-dwarf/stellar regime and 27 confirmed planets F. Kiefer1; 2, G. Hébrard1; 3, A. Lecavelier des Etangs1, E. Martioli1; 4, S. Dalal1, and A. Vidal-Madjar1 1 Institut d’Astrophysique de Paris, Sorbonne Université, CNRS, UMR 7095, 98 bis bd Arago, 75014 Paris, France 2 LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 5 place Jules Janssen, 92195 Meudon, France? 3 Observatoire de Haute-Provence, CNRS, Universiteé d’Aix-Marseille, 04870 Saint-Michel-l’Observatoire, France 4 Laboratório Nacional de Astrofísica, Rua Estados Unidos 154, 37504-364, Itajubá - MG, Brazil Submitted on 2020/08/20 ; Accepted for publication on 2020/09/24 ABSTRACT Mass is one of the most important parameters for determining the true nature of an astronomical object. Yet, many published exoplan- ets lack a measurement of their true mass, in particular those detected thanks to radial velocity (RV) variations of their host star. For those, only the minimum mass, or m sin i, is known, owing to the insensitivity of RVs to the inclination of the detected orbit compared to the plane-of-the-sky. The mass that is given in database is generally that of an assumed edge-on system (∼90◦), but many other inclinations are possible, even extreme values closer to 0◦ (face-on). In such case, the mass of the published object could be strongly underestimated by up to two orders of magnitude.
    [Show full text]
  • Solar System Analogues Among Exoplanetary Systems
    Solar System analogues among exoplanetary systems Maria Lomaeva Lund Observatory Lund University ´´ 2016-EXA105 Degree project of 15 higher education credits June 2016 Supervisor: Piero Ranalli Lund Observatory Box 43 SE-221 00 Lund Sweden Populärvetenskaplig sammanfattning Människans intresse för rymden har alltid varit stort. Man har antagit att andra plan- etsystem, om de existerar, ser ut som vårt: med mindre stenplaneter i banor närmast stjärnan och gas- samt isjättar i de yttre banorna. Idag känner man till drygt 2 000 exoplaneter, d.v.s., planeter som kretsar kring andra stjärnor än solen. Man vet även att vissa av dem saknar motsvarighet i solsystemet, t. ex., heta jupitrar (gasjättar som har migrerat inåt och kretsar väldigt nära stjärnan) och superjordar (stenplaneter större än jorden). Därför blir frågan om hur unikt solsystemet är ännu mer intressant, vilket vi försöker ta reda på i det här projektet. Det finns olika sätt att detektera exoplaneter på men två av dem har gett flest resultat: transitmetoden och dopplerspektroskopin. Med transitmetoden mäter man minsknin- gen av en stjärnas ljus när en planet passerar framför den. Den metoden passar bäst för stora planeter med små omloppsbanor. Dopplerspektroskopin använder sig av Doppler effekten som innebär att ljuset utsänt från en stjärna verkar blåare respektive rödare när en stjärna förflyttar sig fram och tillbaka från observatören. Denna rörelse avslöjar att det finns en planet som kretsar kring stjärnan och påverkar den med sin gravita- tion. Dopplerspektroskopin är lämpligast för massiva planeter med små omloppsbanor. Under projektets gång har vi inte bara letat efter solsystemets motsvarigheter utan även studerat planetsystem som är annorlunda.
    [Show full text]
  • Survival of Exomoons Around Exoplanets 2
    Survival of exomoons around exoplanets V. Dobos1,2,3, S. Charnoz4,A.Pal´ 2, A. Roque-Bernard4 and Gy. M. Szabo´ 3,5 1 Kapteyn Astronomical Institute, University of Groningen, 9747 AD, Landleven 12, Groningen, The Netherlands 2 Konkoly Thege Mikl´os Astronomical Institute, Research Centre for Astronomy and Earth Sciences, E¨otv¨os Lor´and Research Network (ELKH), 1121, Konkoly Thege Mikl´os ´ut 15-17, Budapest, Hungary 3 MTA-ELTE Exoplanet Research Group, 9700, Szent Imre h. u. 112, Szombathely, Hungary 4 Universit´ede Paris, Institut de Physique du Globe de Paris, CNRS, F-75005 Paris, France 5 ELTE E¨otv¨os Lor´and University, Gothard Astrophysical Observatory, Szombathely, Szent Imre h. u. 112, Hungary E-mail: [email protected] January 2020 Abstract. Despite numerous attempts, no exomoon has firmly been confirmed to date. New missions like CHEOPS aim to characterize previously detected exoplanets, and potentially to discover exomoons. In order to optimize search strategies, we need to determine those planets which are the most likely to host moons. We investigate the tidal evolution of hypothetical moon orbits in systems consisting of a star, one planet and one test moon. We study a few specific cases with ten billion years integration time where the evolution of moon orbits follows one of these three scenarios: (1) “locking”, in which the moon has a stable orbit on a long time scale (& 109 years); (2) “escape scenario” where the moon leaves the planet’s gravitational domain; and (3) “disruption scenario”, in which the moon migrates inwards until it reaches the Roche lobe and becomes disrupted by strong tidal forces.
    [Show full text]
  • 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.
    [Show full text]
  • Revising the Ages of Planet-Hosting Stars⋆
    A&A 575, A18 (2015) Astronomy DOI: 10.1051/0004-6361/201424951 & c ESO 2015 Astrophysics Revising the ages of planet-hosting stars? A. Bonfanti1;2, S. Ortolani1;2, G. Piotto1;2, and V. Nascimbeni1;2 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 10 September 2014 / Accepted 14 November 2014 ABSTRACT Aims. This article aims to measure the age of stars with planets (SWP) through stellar tracks and isochrones computed with the PAdova and TRieste Stellar Evolutionary Code (PARSEC). Methods. We developed algorithms based on two different techniques for determining the ages of field stars: isochrone placement and Bayesian estimation. Their application to a synthetic sample of coeval stars shows the intrinsic limits of each method. For instance, the Bayesian computation of the modal age tends to select the extreme age values in the isochrones grid. Therefore, we used the isochrone placement technique to measure the ages of 317 SWP. Results. We found that ∼6% of SWP have ages lower than 0.5 Gyr. The age distribution peaks in the interval [1.5, 2) Gyr, then it decreases. However, ∼7% of the stars are older than 11 Gyr. The Sun turns out to be a common star that hosts planets, when considering its evolutionary stage. Our SWP age distribution is less peaked and slightly shifted towards lower ages if compared with ages in the literature and based on the isochrone fit.
    [Show full text]
  • Age Consistency Between Exoplanet Hosts and Field Stars
    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. Working with TPH, the observational stellar mean density ρ? allows us to compute stellar luminosity even if the distance is not available, by combining ρ? with the spectroscopic log g.
    [Show full text]