MOOO MO 00 Hoob MQOO MOOO MO&O MOOO MOOO MOOO
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Exploring the Realm of Scaled Solar System Analogues with HARPS?,?? D
A&A 615, A175 (2018) Astronomy https://doi.org/10.1051/0004-6361/201832711 & c ESO 2018 Astrophysics Exploring the realm of scaled solar system analogues with HARPS?;?? D. Barbato1,2, A. Sozzetti2, S. Desidera3, M. Damasso2, A. S. Bonomo2, P. Giacobbe2, L. S. Colombo4, C. Lazzoni4,3 , R. Claudi3, R. Gratton3, G. LoCurto5, F. Marzari4, and C. Mordasini6 1 Dipartimento di Fisica, Università degli Studi di Torino, via Pietro Giuria 1, 10125, Torino, Italy e-mail: [email protected] 2 INAF – Osservatorio Astrofisico di Torino, Via Osservatorio 20, 10025, Pino Torinese, Italy 3 INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122, Padova, Italy 4 Dipartimento di Fisica e Astronomia “G. Galilei”, Università di Padova, Vicolo dell’Osservatorio 3, 35122, Padova, Italy 5 European Southern Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile 6 Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012, Bern, Switzerland Received 8 February 2018 / Accepted 21 April 2018 ABSTRACT Context. The assessment of the frequency of planetary systems reproducing the solar system’s architecture is still an open problem in exoplanetary science. Detailed study of multiplicity and architecture is generally hampered by limitations in quality, temporal extension and observing strategy, causing difficulties in detecting low-mass inner planets in the presence of outer giant planets. Aims. We present the results of high-cadence and high-precision HARPS observations on 20 solar-type stars known to host a single long-period giant planet in order to search for additional inner companions and estimate the occurence rate fp of scaled solar system analogues – in other words, systems featuring lower-mass inner planets in the presence of long-period giant planets. -
• August the 26Th 2004 Detection of the Radial-Velocity Signal Induced by OGLE-TR-111 B Using UVES/FLAMES on the VLT (See Pont Et Al
2004 • August the 26th 2004 Detection of the radial-velocity signal induced by OGLE-TR-111 b using UVES/FLAMES on the VLT (see Pont et al. 2004, A&A in press, astro-ph/0408499). • August the 25th 2004 TrES-1b: A new transiting exoplanet detected by the Trans-Atlantic Exoplanet Survey (TreS) team . (see Boulder Press release or Alonso et al.) • August the 25th 2004 HD 160691 c : A 14 Earth-mass planet detected with HARPS (see ESO Press Release or Santos et al.) • July the 8th 2004 HD 37605 b: The first extra-solar planet detected with HRS on the Hobby- Eberly Telescope (Cochran et al.) • May the 3rd 2004 HD 219452 Bb withdrawn by Desidera et al. • April the 28th 2004 Orbital solution for OGLE-TR-113 confirmed by Konacki et al • April the 15th 2004 OGLE 2003-BLG-235/MOA 2003-BLG-53: a planetary microlensing event (Bond et al.) • April the 14th 2004 FLAMES-UVES spectroscopic orbits for two OGLE III transiting candidates: OGLE-TR-113 and OGLE-TR-132 (Bouchy et al.) • February 2004 Detection of Carbon and Oxygen in the evaporating atmosphere of HD 209458 b by A. Vidal-Madjar et al. (from HST observations). • January the 5th 2004 Two planets orbiting giant stars announced by Mitchell et al. during the AAS meeting: HD 59686 b and 91 Aqr b (HD 219499 b). Two other more massive companions, Tau Gem b (HD 54719 b) and nu Oph b (HD 163917 b), have also been announced by the same authors. 2003 • December 2003 First planet detected with HARPS: HD 330075 b (see Mayor et al., in the ESO Messenger No 114) • July the 3rd 2003 A long-period planet on a circular orbit around HD 70642 announced by the AAT team (Carter et al. -
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. -
THE LARGE-SCALE MAGNETIC FIELDS of PLANET-HOSTING SOLAR-TYPE STARS a Thesis Submitted by Matthew W. Mengel, M.Phil., G.D.Inf.Tec
THE LARGE-SCALE MAGNETIC FIELDS OF PLANET-HOSTING SOLAR-TYPE STARS A Thesis Submitted by Matthew W. Mengel, M.Phil., G.D.Inf.Tech, B.Inf.Tech. For the Award of Doctor of Philosophy 2017 Abstract Stellar magnetic fields and their associated phenomena influence stellar be- haviour and evolution, and potentially have significant impacts on any surrounding planetary system. However, the nature of star-planet interactions is unclear, especially the potential impact on a star of a closely orbiting massive planet with a powerful mag- netic field. This thesis presents a spectropolarimetric survey of the large-scale magnetic fields of planet-hosting solar-type stars. While little evidence is found for a systematic dif- ference in the magnetic field characteristics of planet-hosting stars compared with the population of solar-type stars, a small positive correlation is indicated between the magnitude of the tidal effects of the planet on the star and the magnetic field strength. Nevertheless, further spectropolarimetric observations of hot Jupiter hosting systems are required to confirm this tentative relationship. For the particular case of a moderately active star with a thin convective zone and a closely orbiting hot Jupiter (τ Boötis) presented here, a remarkably rapid magnetic cycle with a period of ∼ 240 d is discovered. For stars with shallow convective en- velopes, this is an unusual occurrence and suggests a possible role for planetary tidal or magnetic interaction with the star’s convective zone and magnetic dynamo. More observations are required to verify this possible star-planet interaction and to extend the work to other similar systems as they come to light from exoplanet surveys. -
Carbon and Oxygen Abundances in Stellar Populations
Astronomy & Astrophysics manuscript no. nissen.C-O c ESO 2014 June 23, 2014 Carbon and oxygen abundances in stellar populations ⋆,⋆⋆ P. E. Nissen1,2, Y. Q. Chen1, L. Carigi3, W. J. Schuster4, and G. Zhao1 1 Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China. 2 Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK–8000 Aarhus C, Denmark. e-mail: [email protected] 3 Instituto de Astronom´ıa, Universidad Nacional Aut´onoma de M´exico, AP 70-264, 04510 M´exico DF, Mexico 4 Observatorio Astron´omico Nacional, Universidad Nacional Aut´onoma de M´exico, Apartado Postal 877, C.P. 22800 Ensenada, B.C., Mexico. Received 12 May 2014 / Accepted 17 June 2014 ABSTRACT Context. Carbon and oxygen abundances in stars are important in many fields of astrophysics including nucleosynthesis, stellar structure, evolution of galaxies, and formation of planetary systems. Still, our knowledge of the abundances of these elements in different stellar populations is uncertain because of difficulties in observing and analyzing atomic and molecular lines of C and O. Aims. Abundances of C, O, and Fe are determined for F and G main-sequence stars in the solar neighborhood with metallicities in the range −1.6 < [Fe/H] < +0.4 in order to study trends and possible systematic differences in the C/Fe, O/Fe, and C/O ratios for thin- and thick-disk stars as well as high- and low-alpha halo stars. In addition, we investigate if there is any connection between C and O abundances in stellar atmospheres and the occurrence of planets. -
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. -
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. -
Astronomie Pentru Şcolari
NICU GOGA CARTE DE ASTRONOMIE Editura REVERS CRAIOVA, 2010 Referent ştiinţific: Prof. univ.dr. Radu Constantinescu Editura Revers ISBN: 978-606-92381-6-5 2 În contextul actual al restructurării învăţământului obligatoriu, precum şi al unei manifeste lipse de interes din partea tinerei generaţii pentru studiul disciplinelor din aria curiculară Ştiinţe, se impune o intensificare a activităţilor de promovare a diferitelor discipline ştiinţifice. Dintre aceste discipline Astronomia ocupă un rol prioritar, având în vedere că ea intermediază tinerilor posibilitatea de a învăţa despre lumea în care trăiesc, de a afla tainele şi legile care guvernează Universul. În plus, anul 2009 a căpătat o co-notaţie specială prin declararea lui de către UNESCO drept „Anul Internaţional al Astronomiei”. În acest context, domnul profesor Nicu Goga ne propune acum o a doua carte cu tematică de Astronomie. După apariţia lucrării Geneza, evoluţia şi sfârşitul Universului, un volum care s+a bucurat de un real succes, apariţia lucrării „Carte de Astronomie” reprezintă un adevărat eveniment editorial, cu atât mai mult cu cât ea constitue în acelaşi timp un material monografic şi un material cu caracter didactic. Cartea este structurată în 13 capitole, trecând în revistă problematica generală a Astronomiei cu puţine elemente de Cosmologie. Cartea îşi propune şi reuşeşte pe deplin să ofere răspunsuri la câteva întrebări fundamentale şi tulburătoare legate de existenţa fiinţei umane şi a dimensiunii cosmice a acestei existenţe, incită la dialog şi la dorinţa de cunoaştere. Consider că, în ansamblul său, cartea poate contribui la îmbunătăţirea educaţiei ştiinţifice a tinerilor elevi şi este deosebit de utilă pentru toţi „actorii” implicaţi în procesul de predare-învăţare: elevi, părinţi, profesori. -
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. -
Summer 2021 Schedule of Classes
SUMMER 2021 Class Schedule Classes Begin June 7 (714) 484-7000 @CypressCollege CypressCollege.edu Cypress College — Summer 2021 1 Welcome to Cypress College! COVID 19 Due to the COVID-19 health emergency and possible continued social distancing restrictions, the delivery for most courses will be through remote instruction, which will require a computer and Internet access. Classes partially taught on campus will be noted in the schedule. In some cases, students will also be required to download our secure testing software, if required by their instructor. If this happens, students will be notified prior to the start of instruction. All student services remain available online. Important Dates . 2 Six Easy Steps to the Registration Process . .3 Continuing Student Registration Schedule . 6 Registration Information . 7 myGateway Registration Worksheet . .9 Frequently Asked Questions . 11 How to Add/Drop a Class . 12 Fee Calculation Worksheet. 13 Fees and Refunds . 14 Definitions . 16 How to Read the Class Schedule .. 17 Courses . 18 3 Steps to Distance Education Success . 51 Online Courses . 52 Hybrid Courses . .53 Academic/College Policies Affecting Students . .54 Student Services . .58 General Education Requirements . 62 Quick Guide to Help You . 68 California Nonresident Tuition Exemption Request . 69 Cypress College has made every reasonable effort to determine that everything stated in this Class Schedule is accurate. This publication is prepared in advance of the time period it covers; therefore, changes in courses and programs offered, together with other matters contained herein, are subject to change without notice by the administration of Cypress College. The College reserves the right to cancel any class for which the enrollment is not sufficient to warrant continuation, and to change the class hours and/or days as necessity demands. -
Predictions of Planets for 586 Exosystems and a Method for Predicting Planets in Multi-Planetary Exosystems Valeri Beck
Predictions of planets for 586 exosystems and a method for predicting planets in multi-planetary exosystems Valeri Beck To cite this version: Valeri Beck. Predictions of planets for 586 exosystems and a method for predicting planets in multi- planetary exosystems. 2019. hal-02050412v4 HAL Id: hal-02050412 https://hal.archives-ouvertes.fr/hal-02050412v4 Preprint submitted on 7 Aug 2019 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. Predictions of planets for 586 exosystems and a method for predicting planets in multi-planetary exosystems Valeri Beck*1 *Alfa Carbon® Beck, Berlin, Germany ABSTRACT We have applied a model of planetary system formation in the field of a standing sound wave (the ‘SSW-Model’) to the prediction of planets in 586 multi-planetary exosystems (384 bi- planetary, 127 tri-planetary and 75 exosystems with four or more confirmed planets). We have verified our predictions using transit-like events from the NASA Threshold-Crossing Event (TCE) catalogue, finding that more than 80% of these events are included in our list of exoplanet predictions. We describe a method for predicting the periods and semi-major axes of additional planets for exosystems with two or more confirmed planets. -
Arxiv:1804.08329V1
Astronomy & Astrophysics manuscript no. harps-kp c ESO 2018 April 24, 2018 Exploring the realm of scaled Solar System analogs with HARPS ⋆ D. Barbato1, 2, A. Sozzetti2, S. Desidera3, M. Damasso2, A.S. Bonomo2, P. Giacobbe2, L.S. Colombo4, C. Lazzoni4, 3, R. Claudi3, R. Gratton3, G. LoCurto5, F. Marzari4, and C. Mordasini6 1 Dipartimento di Fisica, Università degli Studi di Torino, via Pietro Giuria 1, I-10125 Torino, Italy 2 INAF – Osservatorio Astrofisico di Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy 3 INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122, Padova, Italy 4 Dipartimento di Fisica e Astronomia "G. Galilei", Università di Padova, Vicolo dell’Osservatorio 3, I-35122 Padova, Italy 5 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile 6 Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland Received <date> / Accepted <date> ABSTRACT Context. The assessment of the frequency of planetary systems reproducing the Solar System’s architecture is still an open problem in exoplanetary science. Detailed study of multiplicity and architecture is generally hampered by limitations in quality, temporal extension and observing strategy, causing difficulties in detecting low-mass inner planets in the presence of outer giant planetary bodies. Aims. We present the results of high-cadence and high-precision HARPS observations on 20 solar-type stars known to host a single long-period giant planet in order to search for additional inner companions and estimate the occurence rate fp of scaled Solar System analogs, i.e. systems featuring lower-mass inner planets in the presence of long-period giant planets.