CHEMICAL ABUNDANCES OF WEAK T TAURI STARS
|
|
- Madison Robbins
- 5 years ago
- Views:
Transcription
1 CHEMICAL ABUNDANCES OF WEAK T TAURI STARS Gustavo de Araujo Rojas Universidade de São Paulo Instituto de Astronomia, Geofísica e Ciências Atmosféricas rojas@astro.iag.usp.br Jane Gregorio-Hetem Universidade de São Paulo Instituto de Astronomia, Geofísica e Ciências Atmosféricas jane@astro.iag.usp.br Abstract This work is a spectroscopic study aiming to derive chemical abundances of a sample of low mass pre-main sequence stars, previously identified as Weak T Tauri stars. High resolution optical spectra were obtained at the Observatório do Pico dos Dias and European Southern Observatory. A classification was developed based on the equivalent widths of the Li I 6708 Å and Hα lines and the spectral type of the studied stars. This classification allowed the identification of them into categories that correspond to different evolutive phases in the pre-main sequence. The position of these stars in the H-R Diagram was also inspected in order to estimate their ages and to confirm their classification in the assumed evolutive scenario. Among the 24 objects of the sample, it was verified that 6 are actually Weak T Tauri stars, 7 are Classical T Tauri, 1 is Post T Tauri, and 10 are Fe/Ge Pre-Main Sequence stars. The stellar fundamental parameters effective temperature and gravity were calculated by excitation and ionization equilibria of Iron absorption lines. Chemical abundances were obtained by spectral synthesis. The first results indicate that the studied sample shows solar abundances. 1
2 2 Introduction The identification of large samples of young stars and detailed analysis of the distribution of their chemical abundances, comparing pre-main sequence stars with young clusters, is of great interest to galactic chemical evolution models. Among pre-main sequence stars, the Weak T Tauri stars (WTTS) are specially suited for spectroscopic abundance analysis, as the veiling effect on absorption lines (which have made difficult the chemical analysis of classical T Tauri stars) is not enhanced. This can be interpreted as a less intense accretion activity. There are very few results in the literature concerning abundances in pre-main sequence stars, most of them focused on Lithium abundances. One of the few examples presenting metallicities of T Tauri stars was published by Padgett (1996), who calculated the Iron abundances of 30 stars of nearby star forming regions. 1. Target Selection and Observations 1.1 Target Selection Our sample consists of 22 candidates previously classified as WTTS, selected from the young stellar objects catalogues Pico dos Dias Survey (Gregorio-Hetem et al. 1992; Torres et al. 1995) and Herbig-Bell Catalogue (Herbig & Bell 1988). We selected all stars with Hα equivalent widths in emission inferior to 20 Å and a visual magnitude brighter than 12 mag. We also included 2 WTTS selected from the literature, HD 8558 (Torres et al. 2000) and SAO 76411A (Walter et al. 1988). 1.2 Observations The observations were performed at the Observatório do Pico dos Dias (OPD) in Brasópolis, Brazil, and at the European Southern Observatory (ESO) in La Silla, Chile, in six runs between October, 2000 and November, At the OPD we used the Coudé spectrograph and 1,60 m. telescope, obtaining spectra with resolution R=20000 in 4 spectral regions. At ESO we used the FEROS spectrograph and 1,52 m. telescope, obtaining high-resolution spectra (R=48000) covering the whole optical range (360 to 920 nm). Table 1 lists the stars of the sample and the observational data from the literature.
3 3 Table 1. Published data for the sample stars. The equivalent widths (W) of emission lines are represented by negative values. Object V Spectral Type W(Hα) (Å) HBC 400 a 12.1 K7V -3.2 HD 8558 b 8.5 G6V -3.3 PDS G9V PDS G5V PDS F6V -6.0 PDS M2V -2.1 PDS G0V PDS K5V 0.0 PDS M3V PDS K2V -5.0 PDS K7V -5.0 PDS F5V -3.0 PDS G0V PDS F7V 3.0 PDS F5V -6.0 PDS G3V -0.5 PDS G5V -9.0 PDS 117S 11.1 F6V -8.0 PDS F6V -7.0 PDS F5V -2.0 PDS F5+F8 IV -1.0 PDS 390S 8.7 F6V PDS F6IV -5.0 SAO 76411A c 8.9 G0V 0.1 References : a) Mundt et al. 1983; b) Torres et al. 2000; c) Walter et al The data for the remaining were obtained by Torres (1998) 2. Spectroscopic Classification Spectral types were determined by comparing the observed spectra with the digital libraries published by Danks & Dennefeld (1994) and Jacoby et al. (1984). We found no spectral type variations with the types published in previous works. 2.1 Emission Line Profiles By definition, the WTTS are distinguished from the Classical T Tauri stars (CTTS) by the equivalent width of the Hα emission, adopting W(Hα) < 10 Å for WTTS. However, the Hα emission is variable and should not be used as the only distinguishing criterion between these
4 4 two classes. Additional information about the circumstellar structure and activity can be obtained by the Hα emission profiles. In this work these line profiles were classified in three types : Type 1 for absorption lines, Type 2 for symmetric emission profiles and Type 3 for complex emission profiles. Figure 1 shows examples of each profile type. Figure 1. Examples of the three profile types of the Hα line. PDS 54 (upper left panel) shows a Type 1 profile, in absorption. HBC 400 (upper right panel) presents a Type 2 profile, with symmetric emission. PDS 111 (lower panel) shows a complex Hα emission, classified as Type 3.
5 2.2 Ages Ages were estimated by comparing the positions of the stars in the HR Diagram. The pre-main sequence evolutionary tracks published by D Antonna & Mazzitelli (1994) were adopted. The luminosities were derived using distances estimated from the Hipparcos parallaxes when avaiable, or the distance of the parent molecular cloud. Figure 2 shows the observed HR diagram and the evolutionary tracks. 5 Figure 2. Position in the HR diagram of the stars of the sample. The pre-main sequence evolutionary tracks are from D Antonna & Mazitelli (1994).
6 6 2.3 Spectroscopic Classification According to emission features, spectral type, and derived age, the stars of the sample were classified in four categories : Classical T Tauri (CTTS) : spectral type K or M, stronger emission lines with complex profiles, ages < 10 Myr Weak T Tauri (WTTS): spectral type K or M, weak emission lines with symmetric profiles, ages < 20 Myr Post T Tauri (PTTS) : spectral type K or M, Hα in absorption, ages > 20 Myr Fe/Ge Pre-Main Sequence (Fe/Ge): spectral type F or G, stronger emission lines with complex profiles, ages < 10 Myr Table 2 presents the final obtained stellar parameters and classification. Table 2. Spectroscopic classification of the sample Object T eff (K) W LiI (Å) W(Hα) (Å) Hα Profile Class HBC WTT HD PTT PDS CTT PDS CTT PDS Fe/Ge PDS WTT PDS CTT PDS WTT PDS WTT PDS WTT PDS CTT PDS Fe/Ge PDS CTT PDS Fe/Ge PDS Fe/Ge PDS CTT PDS CTT PDS 117S Fe/Ge PDS Fe/Ge PDS Fe/Ge PDS Fe/Ge PDS 390S Fe/Ge PDS Fe/Ge SAO 76411A WTT
7 3. Results and Discussion 3.1 Effective Temperatures The effective temperature (T eff ) was derived from three independent criteria: calibration with spectral type, excitation equilibrium of Fe I and equivalent width ratio of metallic absorption lines. A first estimative of the T eff was obtained using the empirical spectral type calibration published by de Jager & Nieuwenhuijzen (1987). This method was employed to all the stars of the sample. Excellent quality spectra were obtained for seven stars, which have small rotational velocities and low veiling. In this case, hundreds of Iron absorption lines were accuratelly measured and used in the code Renoir (kindly provided by M. Spite) to determine effective temperatures based on the excitation equilibrium (more details are presented in section 3.2). An even more precise method uses the equivalent width ratio of selected absorption lines showing different excitation potentials, which are very sensitive to temperature changes. The adopted calibration was published by Padgett (1996), who lists six pairs of absorption lines of Fe I and V I. This method was only applied to the seven stars mentioned above. Table 3 lists the obtained results, showing a good agreement among the three different methods. 7 Table 3. Comparision of the effective temperatures obtained from three independent criteria: spectral type calibration (T ST ), excitation equilibrium (T EE ), and equivalent width ratio (T EW ). Object T ST (K) T EE(K) T EW (K) HBC HD PDS PDS PDS PDS SAO 76411A
8 8 3.2 Surface Gravities Surface gravities (log g) were calculated based on the ionization equilibrium of Iron lines, using the code Renoir mentioned in section 3.1. This code calculate Iron abundances from measured equivalent widths of Fe I and Fe II lines, where the gravity is a free parameter. The adopted value of log g is the one which provides the same abundance for both Fe I and Fe II lines. For the calculations solar metallicities and a microturbulent velocity of 2 km/s were assumed. The atmospheric models are from Kurucz (1993) and the atomic line data are from the Vienna Atomic Line Database (Kupka et al. 1999). Table 4 lists the results, showing typical subgiant gravities (as expected), with values of log g ranging from 4.0 to 4.8 dex. Table 4. Surface gravities (log g) calculated from the ionization equilibrium of Fe I and Fe II lines. Object log g (dex) HBC HD PDS PDS PDS PDS SAO 76411A Abundances Elemental abundances were calculated for 22 chemical elements by spectral synthesis of selected absorption lines of 22 elements. The code Spectroscopy Made Easy (Valenti & Piskunov 1996) was adopted, which calculates abundances in the local thermodynamical equilibrium. As in the case of excitation and ionization equilibrium, we were only able to perform the spectral synthesis for the seven stars of excellent spectra quality. Examples of synthetic spectra are presented in Figure 3, and the calculated abundances are listed in Table 5.
9 Figure 3. Examples of the fitted synthetic spectra for the star HD Blue : synthetic spectrum. Red : observed spectrum. 9
10 10 Table 5. Chemical abundances [X/Fe] relative to the Sun calculated for the stars of the sample for which the spectral synthesis were performed. Element Li C O Na Mg Al Si S Ca Sc Ti HBC HD PDS PDS PDS PDS SAO76411A Element V Cr Mn Fe Co Ni Sr Y Ba La Eu HBC HD PDS PDS PDS PDS SAO76411A Conclusions Spectroscopic criteria were applied for 24 objects previously identified as Weak T Tauri stars in order to separate them into different pre-main sequence categories. Our re-classification showed that only six of the stars are actually WTTS, the remaining being CTTS, PTTS or Fe/Ge Pre-Main Sequence stars. Stellar parameters and chemical abundances of 22 elements were obtained for seven stars of the sample. For all of them the abundances, with the exception of Lithium, are similar to the solar values. Acknowledgments GAR acknowledges the grant provided by the Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) for the MSc research. Both authors thank the Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) for partial finnancial support (Proc. No. 2001/ ).
11 References Danks, A. C., Dennefeld, M. 1994, PASP 106, 382 D Antona, F., Mazzitelli, I. 1994, ApJS 90, 467 de Jager, C., Nieuwenhuijzen, H. 1987, A&A 177, 217 Gregorio-Hetem, J., Lépine, J., Quast, G., Torres, C.A., de la Reza, R. 1992, AJ 103, 549 Herbig, G. H., Bell, K. R Lick Obs. Bull Jacoby, G. H., Hunter, D. A., Christian, C. A. 1984, ApJS 56, 257 Kupka, F., Ryabchikova, T. A., Stemples, H. C., Weiss, W. W. 1999, A&AS 138, 119 Kurucz, R. L CD-ROM No. 18 Mundt, R., Walter, F. M., Feigelson, E. D., Finkenzeller, U., Herbig, G. H., Odell, A. P ApJ 269, 229 Padgett, D. L. 1996, ApJ 471, 847 Torres, C. A. O PhD. Thesis, CNPq/Observatório Nacional, Brasil Torres, C.A., Quast, G., de la Reza, R., Lépine, J., Gregorio-Hetem, J. 1995, AJ 109, 2146 Torres, C. A. O., Da Silva, l., Quast, G. R., De La Reza, R., Jilinski, E AJ 120, 1410 Valenti, J. A., Piskunov, N A&ASS 118, 595 Walter, F. M., Brown, A., Mathieu, R. D., Myers, P. C., Vrba, F. J AJ 96,
The Great Austral Nearby Young Association 1
Young Stars Near Earth: Progress and Prospects ASP Conference Series, Vol.???, 2001 Ray Jayawardhana and Thomas Greene, eds. The Great Austral Nearby Young Association 1 C. A. O. Torres, G.R. Quast Laboratório
More informationarxiv:astro-ph/ v1 16 Dec 2004
The Metallicity of Post-T Tauri Stars: A preliminary approach to the understanding of the metal enrichment of stars harboring planets arxiv:astro-ph/0412398v1 16 Dec 2004 Ramiro de la Reza, Licio da Silva
More informationDifferential abundances in the HAT-P-4 binary system
Differential abundances in the HAT-P-4 binary system Carlos Saffe 1,4, Emiliano Jofré 2,4, Eder Martioli 3 Matías Flores 1,4, Romina Petrucci 2,4 & Marcelo Jaque 1,4 (1) Instituto de Ciencias Astronómicas,
More informationHigh resolution spectroscopy of two metal-poor red giants: HD and HD
High resolution spectroscopy of two metal-poor red giants: HD 3078 and HD 1873 Faculty of Physics and Mathematics, University of Latvia, Raiņa bulv. 19, Riga, LV-1586, Latvia E-mail: arturs_ lv@inbox.lv
More informationChemical tagging of FGK stars: testing membership to stellar kinematic groups
Chemical tagging of FGK stars: testing membership to stellar kinematic groups David Montes, Hugo M. Tabernero, Jonay I. González Hernández Dpto. Astrofísica, F. Físicas Universidad Complutense de Madrid,
More informationHigh-dispersion Spectroscopic Observations of the T Tauri-type Stars with Weak Emission Lines
ELSEVIER Chinese Astronomy and Astrophysics 37 (2013) 418 427 CHINESE ASTRONOMY AND ASTROPHYSICS High-dispersion Spectroscopic Observations of the T Tauri-type Stars with Weak Emission Lines XING Li-feng
More informationarxiv:astro-ph/ v1 2 Jul 2002
**TITLE** ASP Conference Series, Vol. **VOLUME***, **YEAR OF PUBLICATION** **NAMES OF EDITORS** SACY - Present Status 1 C. A. O. Torres, G.R. Quast Laboratório Nacional de Astrofísica/MCT, 37504-364 Itajubá,
More informationCHEMICAL ABUNDANCE ANALYSIS OF RC CANDIDATE STAR HD (46 LMi) : PRELIMINARY RESULTS
Dig Sites of Stellar Archeology: Giant Stars in the Milky Way Ege Uni. J. of Faculty of Sci., Special Issue, 2014, 145-150 CHEMICAL ABUNDANCE ANALYSIS OF RC CANDIDATE STAR HD 94264 (46 LMi) : PRELIMINARY
More informationEclipsing Binaries in Open Clusters
Eclipsing Binaries in Open Clusters John Southworth (jkt@astro.keele.ac.uk) and Jens Viggo Clausen (jvc@astro.ku.dk) Niels Bohr Institute, Copenhagen University, Denmark. Abstract. The study of detached
More informationSpectroWeb: An Interactive Graphical Database of Digital Stellar Spectral Atlases
: An Interactive Graphical Database of Digital Stellar Spectral Atlases arxiv:0707.3722v1 [astro-ph] 25 Jul 2007. A. LOBEL 1 1 Royal Observatory of Belgium, Ringlaan 3, Brussels, B-1180, Belgium ABSTRACT
More informationHigh resolution spectroscopic characterization of the FGK stars in the solar neighbourhood
High resolution spectroscopic characterization of the FGK stars in the solar neighbourhood R. Martínez-Arnáiz 1, J. Maldonado 2, D. Montes 1, C. Eiroa 2, B. Montesinos 3, I. Ribas 4, E. Solano 3 Abstract
More informationBRASS. The Belgian Repository of fundamental Atomic data and Stellar Spectra. Contact day meeting 19th September 2017
Contact day meeting 19th September 2017 mike.laverick@kuleuven.be BRASS The Belgian Repository of fundamental Atomic data and Stellar Spectra Mike Laverick Thibault Merle Alex Lobel Pierre Royer Christophe
More informationarxiv: v1 [astro-ph] 5 Dec 2007
Contrib. Astron. Obs. Skalnaté Pleso 1, 1 6, (2007) Magnetic, Chemical and Rotational Properties of the Herbig Ae/Be Binary System HD 72106 arxiv:0712.0771v1 [astro-ph] 5 Dec 2007 C.P. Folsom 1,2,3, G.A.Wade
More informationHigh-resolution Spectroscopy of CARMENCITA objects. Patrick Schöfer
High-resolution Spectroscopy of CARMENCITA objects Patrick Schöfer 2015-10-22 Overview Motivation Aims of the analysis and data sample Prelude I: Data reduction Prelude II: Target identification Analysis
More informationFrom the first stars to planets
High precision stellar spectroscopy: From the first stars to planets Jorge Meléndez Departamento de Astronomia, IAG, Universidade de São Paulo My group: SAMPA Stellar Atmospheres, Planets & Abundances
More informationSISD Training Lectures in Spectroscopy
SISD Training Lectures in Spectroscopy Anatomy of a Spectrum Visual Spectrum of the Sun Blue Spectrum of the Sun Morphological Features in Spectra λ 2 Line Flux = Fλ dλ λ1 (Units: erg s -1 cm -2 ) Continuum
More informationOxygen in red giants from near-infrared OH lines: 3D effects and first results from. Puerto de la Cruz, May 14, 2012! Carlos Allende Prieto!
Oxygen in red giants from near-infrared OH lines: 3D effects and first results from Puerto de la Cruz, May 14, 2012! Carlos Allende Prieto! Overview! 1. APOGEE: status and prospects! 2. A first look at
More informationCO Emission in the Inner Disk Around Young Intermediate-Mass Stars
Clemson University TigerPrints Publications Physics and Astronomy 7-1-2012 CO Emission in the Inner Disk Around Young Intermediate-Mass Stars Matt L. Stevans University of Colorado Sean D. Brittain Clemson
More informationA study of accretion disk wind emission
Mem. S.A.It. Vol. 83, 525 c SAIt 2012 Memorie della A study of accretion disk wind emission R. E. Puebla 1, M. P. Diaz 1, and D. J. Hillier 2 1 Departamento de Astronomia, Instituto de Astronomia, Geofísica
More informationOverview of Gaia-ESO Survey results based on high-resolution spectra of FGK-type stars Rodolfo Smiljanic! (Gaia-ESO WG11 co-coordinator)
Overview of Gaia-ESO Survey results based on high-resolution spectra of FGK-type stars Rodolfo Smiljanic! (Gaia-ESO WG11 co-coordinator) The Gaia-ESO Survey http://www.gaia-eso.eu Public spectroscopic
More informationA Spectral Atlas of F and G Stars
Chin. J. Astron. Astrophys. Vol. 4 (2004), No. 3, 279 283 ( http: /www.chjaa.org or http: /chjaa.bao.ac.cn ) Chinese Journal of Astronomy and Astrophysics A Spectral Atlas of F and G Stars V. G. Klochkova
More informationarxiv: v1 [astro-ph] 22 Oct 2007
arxiv:0710.4134v1 [astro-ph] 22 Oct 2007 Radial velocities of giant stars: an investigation of line profile variations. S Hekker 1, I A G Snellen 1, C Aerts 2,3, A Quirrenbach 4, S Reffert 4 and D S Mitchell
More informationSURVEYING THE SUBSTELLAR COMPONENT OF THE ORION DISPERSED POPULATIONS
SURVEYING THE SUBSTELLAR COMPONENT OF THE ORION DISPERSED POPULATIONS Juan José Downes (1,2), César Briceño (1), Jesús Hernández (1), Nuria Calvet (3) & Lee Hartmann (3) WITH THE COLLABORATION OF: Cecilia
More informationNew Results of Spectral Observations of CP Stars in the Li I 6708 Å Spectral Region with the 6 m BTA Telescope
Magnetic Stars, 2011, pp. 374 381 New Results of Spectral Observations of CP Stars in the Li I 6708 Å Spectral Region with the 6 m BTA Telescope Polosukhina N. 1, Shavrina A. 2, Drake N. 3, Kudryavtsev
More information6. Stellar spectra. excitation and ionization, Saha s equation stellar spectral classification Balmer jump, H -
6. Stellar spectra excitation and ionization, Saha s equation stellar spectral classification Balmer jump, H - 1 Occupation numbers: LTE case Absorption coefficient: κ ν = n i σ ν$ à calculation of occupation
More informationThe Composition of the Old, Metal-Rich Open Cluster, NGC 6791
The Composition of the Old, Metal-Rich Open Cluster, NGC 6791 Liz Jensen --- Smith College, REU at IFA, University of Hawaii 2006 Mentor: Ann M. Boesgaard --- Institute for Astronomy, University of Hawaii
More informationProtoplanetary discs of isolated VLMOs discovered in the IPHAS survey
Protoplanetary discs of isolated VLMOs discovered in the IPHAS survey Luisa Valdivielso Casas Collaborators: E. Martín, H. Bouy, E. Solano,J. Drew,R. Greimel 1 IAC - ULL 14 de septiembre 2010 Outline Introduction
More informationChapter 10: Unresolved Stellar Populations
Chapter 10: Unresolved Stellar Populations We now consider the case when individual stars are not resolved. So we need to use photometric and spectroscopic observations of integrated magnitudes, colors
More informationStar formation in the region of young open cluster - NGC 225
Bull. Astr. Soc. India (2006) 34, 315 325 Star formation in the region of young open cluster - NGC 225 Annapurni Subramaniam 1, Blesson Mathew 1 and Sreeja S. Kartha 1,2 1 Indian Institute of Astrophysics,
More informationClassical Methods for Determining Stellar Masses, Temperatures, and Radii
Classical Methods for Determining Stellar Masses, Temperatures, and Radii Willie Torres Harvard-Smithsonian Center for Astrophysics 2010 Sagan Exoplanet Summer Workshop 1 Outline Basic properties of stars
More informationSara Lucatello Osservatorio Astronomico di Padova, Vicolo dell Osservatorio 5, 35122, Padova, Italy
The Frequency of Carbon-Enhanced Stars in HERES and SDSS Dept. of Physics & Astronomy and JINA: Joint Institute for Nuclear Astrophysics, Michigan State University, E. Lansing, MI 48824 USA E-mail: beers@pa.msu.edu
More informationSUPPLEMENTARY INFORMATION
doi:10.1038/nature10389 Observations The Kepler satellite gathered 30 days of uninterrupted data for HD 187547 (KIC 7548479) between October 19 and November 18, 2009, corresponding to Kepler s observing
More informationThe age of the Galactic thin disk from Th/Eu nucleocosmochronology. III. Extended sample,
A&A 440, 1153 1159 (2005) DOI: 101051/0004-6361:20053307 c ESO 2005 Astronomy & Astrophysics The age of the Galactic thin disk from Th/Eu nucleocosmochronology III Extended sample, E F del Peloso 1,2,LdaSilva
More informationCCD astrometry and UBV photometry of visual binaries
ASTRONOMY & ASTROPHYSICS JUNE I 1998, PAGE 299 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 130, 299 304 (1998) CCD astrometry and UBV photometry of visual binaries II. Visual double stars with mainly
More informationLithium abundances and metallicities: trends from metal-poor and AGB/RGB stars
Mem. S.A.It. Suppl. Vol. 22, 103 c SAIt 2012 Memorie della Supplementi Lithium abundances and metallicities: trends from metal-poor and AGB/RGB stars W. J. Maciel and R. D. D. Costa Astronomy Department
More informationRX J a surprising pre-main sequence spectroscopic binary
A&A 366, 965 971 (2001) DOI: 10.1051/0004-6361:20000355 c ESO 2001 Astronomy & Astrophysics RX J1603.8-3938 a surprising pre-main sequence spectroscopic binary E. W. Guenther 1, G. Torres 2, N. Batalha
More informationChemical abundances in solar analogs Ricardo López Valdivia
Chemical abundances in solar analogs Ricardo López Valdivia Dr. Miguel Chávez Dr. Emanuele Bertone Objetive Make a detailed analysis of chemical abundances in G0-G3 main sequence stars (solar analogs)
More informationX-ray emission from PTT stars
X-ray emission from PTT stars G. Del Zanna a,c H.L. Worters b G.E. Bromage b C.A. Foley c H.E. Mason a M. Landini d A. Whiting e a DAMTP, University of Cambridge, Cambridge UK b University of Central Lancashire,
More informationA new code for automatic determination of equivalent widths: Automatic Routine for line Equivalent widths in stellar Spectra (ARES), ABSTRACT
A&A 469, 783 791 (2007) DOI: 10.1051/0004-6361:20077288 c ESO 2007 Astronomy & Astrophysics A new code for automatic determination of equivalent widths: Automatic Routine for line Equivalent widths in
More informationTwo new T Tauri stars and a candidate FU Orionis star associated with Bok globules
Astron. Astrophys. 320, 167 171 (1997) ASTRONOMY AND ASTROPHYSICS Two new T Tauri stars and a candidate FU Orionis star associated with Bok globules J.L. Yun 1, M.C. Moreira 1, J.F. Alves 1, and J. Storm
More informationMassive Stars as Tracers for. Stellar & Galactochemical Evolution
as Tracers for Stellar & Galactochemical Evolution Norbert Przybilla Dr. Remeis-Observatory Bamberg M. Firnstein, F. Schiller M.F. Nieva, K. Butler, R.P. Kudritzki, G. Meynet, A. Maeder Outline Intro Diagnostics
More informationCharacterization of the exoplanet host stars. Exoplanets Properties of the host stars. Characterization of the exoplanet host stars
Characterization of the exoplanet host stars Exoplanets Properties of the host stars Properties of the host stars of exoplanets are derived from a combination of astrometric, photometric, and spectroscopic
More informationGalac%c Unprecedented Precision (0.01 dex)
Li Be B Si O Fe Dy Ce Ru Y Pb C a Ti L V b Y Eu Al N Pr d Sr Mo Ba P Ca K Cr S N Sm Gd U Ag Pd Mg Ni Galac%c Archaeology @ Unprecedented Precision (0.01 dex) @DrJorgeMelendez Dep. Astronomia, Univ. São
More informationThe Gaia-ESO Spectroscopic Survey. Survey Co-PIs. Gerry Gilmore (IoA, Cambridge) & Sofia Randich (INAF/Arcetri) >300 CoIs
The Gaia-ESO Spectroscopic Survey Survey Co-PIs Gerry Gilmore (IoA, Cambridge) & Sofia Randich (INAF/Arcetri) >300 CoIs Gaia-ESO survey context and motivations (conclusions and key words of several talks)
More informationAstronomical Spectroscopy Introduction PMO David Haworth Copyright 2014
Astronomical Spectroscopy Introduction PMO 2014 David Haworth www.stargazing.net/david Copyright 2014 Astronomical Spectroscopy Astrophysics Quantum Mechanics Electromagnetic spectrum provides insight
More informationA spectroscopic study of RGB stars in the globular cluster NGC 2808 with FLAMES
Mem. S.A.It. Suppl. Vol. 5, 59 c SAIt 2004 Memorie della Supplementi A spectroscopic study of RGB stars in the globular cluster NGC 2808 with FLAMES C. Cacciari, A. Bragaglia and E. Carretta INAF Osservatorio
More informationPossible detection of a magnetic field in T Tauri
A&A 401, 1057 1061 (2003) DOI: 10.1051/0004-6361:20030156 c ESO 2003 Astronomy & Astrophysics Possible detection of a magnetic field in T Tauri D. A. Smirnov 1,3,S.N.Fabrika 2,S.A.Lamzin 1,3, and G. G.
More informationX-ray emission and variability of young, nearby stars
Young Stars Near Earth: Progress and Prospects ASP Conference Series, Vol.???, 2001 Ray Jayawardhana and Thomas Greene, eds. X-ray emission and variability of young, nearby stars B. Stelzer, R. Neuhäuser
More information6. Stellar spectra. excitation and ionization, Saha s equation stellar spectral classification Balmer jump, H -
6. Stellar spectra excitation and ionization, Saha s equation stellar spectral classification Balmer jump, H - 1 Occupation numbers: LTE case Absorption coefficient: = n i calculation of occupation numbers
More informationSpectroscopy of giants and supergiants! Maria Bergemann MPIA Heidelberg"
Spectroscopy of giants and supergiants! Maria Bergemann MPIA Heidelberg" Spectroscopy of (cool) giants and supergiants! Maria Bergemann MPIA Heidelberg" Outline! Motivation why do spectroscopy of giant
More informationSignatures of Peculiar Supernova Nucleosynthesis in Extremely α-enhanced Metal-poor Stars
Signatures of Peculiar Supernova Nucleosynthesis in Extremely α-enhanced Metal-poor Stars Hye-Eun Jang 1, Sung-Chul Yoon 1, Young Sun Lee 2, Ho-Gyu Lee 3, Wonseok Kang 4 and Sang-Gak Lee 1 1 Seoul National
More informationTHE OBSERVATION AND ANALYSIS OF STELLAR PHOTOSPHERES
THE OBSERVATION AND ANALYSIS OF STELLAR PHOTOSPHERES DAVID F. GRAY University of Western Ontario, London, Ontario, Canada CAMBRIDGE UNIVERSITY PRESS Contents Preface to the first edition Preface to the
More informationStar formation : circumstellar environment around Young Stellar Objects
Bull. Astr. Soc. India (2005) 33, 327 331 Star formation : circumstellar environment around Young Stellar Objects Manoj Puravankara Inter-University Centre for Astronomy and Astrophysics, Pune - 411007,
More informationAstr 5465 Feb. 6, 2018 Today s Topics
Astr 5465 Feb. 6, 2018 Today s Topics Stars: Binary Stars Determination of Stellar Properties via Binary Stars Classification of Binary Stars Visual Binaries Both stars visible Only one star visible Spectroscopic
More information6. Stellar spectra. excitation and ionization, Saha s equation stellar spectral classification Balmer jump, H -
6. Stellar spectra excitation and ionization, Saha s equation stellar spectral classification Balmer jump, H - 1 Occupation numbers: LTE case Absorption coefficient: = n i calculation of occupation numbers
More informationPhysical parameter determinations of young Ms
Mem. S.A.It. Vol. 85, 773 c SAIt 2014 Memorie della Physical parameter determinations of young Ms Taking advantage of the Virtual Observatory to compare methodologies A. Bayo 1,2, C. Rodrigo 3,4, D. Barrado
More informationChapter 7: From theory to observations
Chapter 7: From theory to observations Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle, predict the evolution of the stellar bolometric luminosity, effective
More informationarxiv: v1 [astro-ph] 2 Aug 2007
Mon. Not. R. Astron. Soc., accepted (2018) Printed 22 May 2018 (MN LATEX style file v1.4) Polaris B, an optical companion of Polaris (α UMi) system: atmospheric parameters, chemical composition, distance
More informationThe enigma of lithium: from CP stars to K giants. First results of CP star observations obtained at Mount Stromlo Observatory
Modelling of Stellar Atmospheres IAU Symposium, Vol. xxx, xxxx N. E. Piskunov, W. W. Weiss, D. F. Gray, eds. The enigma of lithium: from CP stars to K giants. First results of CP star observations obtained
More informationCHEMICAL ABUNDANCES FOR A SAMPLE OF SOUTHERN OB STARS. 1 II. THE OUTER DISK
The Astrophysical Journal, 606:514 519, 2004 May 1 # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. CHEMICAL ABUNDANCES FOR A SAMPLE OF SOUTHERN OB STARS. 1 II. THE OUTER
More informationTHE SPECTRUM OF A STAR
THE SPECTRUM OF A STAR Overview: Stars can be classified by using the general shape and specific lines of their spectra. Objectives: The student will: perform a simple analysis of spectral lines to classify
More informationDetailed chemical abundances of M-dwarf planet hosts from APOGEE observations
Detailed chemical abundances of M-dwarf planet hosts from APOGEE observations Diogo Souto Observatório Nacional - ON/MCTI + Katia Cunha Anibal Verne Smith C. Allende Prieto Garcia Hernandez Olga Zamora
More informationarxiv:astro-ph/ v1 20 Mar 2006
A search for ultra-compact dwarf galaxies in the NGC 1023 group of galaxies Steffen Mieske 1, Michael J. West 2, and Claudia Mendes de Oliveira 3 arxiv:astro-ph/0603524v1 20 Mar 2006 1 ESO, Karl-Schwarzschild-Str.
More informationarxiv:astro-ph/ v1 14 Dec 1998
Spectroscopy of red giants of the Sagittarius dwarf galaxy arxiv:astro-ph/9812267v1 14 Dec 1998 G. Marconi Osservatorio Astronomico di Roma P. Bonifacio Osservatorio Astronomico di Trieste L. Pasquini
More informationFrom theory to observations
Stellar Objects: From theory to observations 1 From theory to observations Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle, give the prediction of the
More informationASTR-1020: Astronomy II Course Lecture Notes Section III
ASTR-1020: Astronomy II Course Lecture Notes Section III Dr. Donald G. Luttermoser East Tennessee State University Edition 4.0 Abstract These class notes are designed for use of the instructor and students
More informationarxiv: v1 [astro-ph.co] 2 Dec 2011
The Spectral Energy Distribution of Galaxies Proceedings IAU Symposium No. 284, 2011 R.J. Tuffs & C.C.Popescu, eds. c 2011 International Astronomical Union DOI: 00.0000/X000000000000000X Spectral models
More informationThe Classification of Stellar Spectra Chapter 8
The Classification of Stellar Spectra Chapter 8 Star Clusters in the Large Magellanic Cloud http://www.seds.org/hst/ NGC850.html The Classification of Stellar Spectra Classification scheme developed before
More information12. Physical Parameters from Stellar Spectra. Fundamental effective temperature calibrations Surface gravity indicators Chemical abundances
12. Physical Parameters from Stellar Spectra Fundamental effective temperature calibrations Surface gravity indicators Chemical abundances 1 Fundamental Properties of Stars Temperature (T) Radius (R) Chemical
More informationarxiv:astro-ph/ v1 12 Jun 2003
arxiv:astro-ph/0306265v1 12 Jun 2003 SACY - A SEARCH FOR ASSOCIATIONS CONTAINING YOUNG STARS * Carlos A. O. Torres, Germano R. Quast Laboratório Nacional de Astrofísica/MCT, 37504-364 Itajubá, Brazil beto@lna.br,
More informationHigh-mass stars in the Galactic center Quintuplet cluster
High-mass stars in the Galactic center Quintuplet cluster Adriane Liermann 1,2, Wolf-Rainer Hamann 2, Lidia M. Oskinova 2 and Helge Todt 2 1 Max-Planck-Institut für Radioastronomie, Bonn, Germany 2 Universität
More informationTESS Proposal on behalf of TASC WG 4 Cadence: 2-min sampling
TESS Proposal on behalf of TASC WG 4 Cadence: 2-min sampling Title: A survey of rapidly oscillating Ap stars Abstract: The magnetic, and chemically peculiar nature of the rapidly oscillating Ap (roap)
More informationV. Stars.
V. Stars http://sgoodwin.staff.shef.ac.uk/phy111.html 0. The local HR diagram We saw that locally we can make an HR diagram of absolute luminosity against temperature. We find a main sequence, giants and
More informationFIA0221: Taller de Astronomía II. Lecture 14 Spectral Classification of Stars
FIA0221: Taller de Astronomía II Lecture 14 Spectral Classification of Stars Spectral types along the stellar CMD. Oh, Be A Fine Girl Kiss Me! Classification of Stellar spectra: The MK system: strong He+
More informationStellar Spectra ASTR 2110 Sarazin. Solar Spectrum
Stellar Spectra ASTR 2110 Sarazin Solar Spectrum Test #1 Monday, October 9, 11-11:50 am Ruffner G006 (classroom) You may not consult the text, your notes, or any other materials or any person Bring pencils,
More informationarxiv: v2 [astro-ph] 4 Nov 2008
Comm. in Asteroseismology Vol. number, publication date (will be inserted in the production process) On the nature of HD 207331: a new δ Scuti variable arxiv:0810.0476v2 [astro-ph] 4 Nov 2008 L.Fox Machado
More informationarxiv:astro-ph/ v2 14 Oct 2002
Star Formation through Time ASP Conference Series, Vol. **VOLUME**, 2003 Pérez, González Delgado, Tenorio-Tagle The Environmental Dependence of Star Formation in the Nearby Universe arxiv:astro-ph/0210242v2
More informationINFRARED SURVEY FOR THE CHARACTERIZATION OF STELLAR POPULATION OF: SPIRAL ARMS AND OF A BAR AT THE GALACTIC CENTER
INFRARED SURVEY FOR THE CHARACTERIZATION OF STELLAR POPULATION OF: SPIRAL ARMS AND OF A BAR AT THE GALACTIC CENTER Eduardo B. de Amôres 1 and Jacques R. D. Lépine 1 1 Instituto de Astronomia Geofísica
More informationSpectral analysis of very hot H-deficient [WCE]-type central stars of planetary nebulae
Spectral analysis of very hot H-deficient [WCE]-type central stars of planetary nebulae Graziela R. Keller 1 Colaborators: Luciana Bianchi 2 and Walter J. Maciel 1 1 IAG/Universidade de São Paulo 2 The
More informationMethods of Determining Relative Age of Young Stellar Objects Zak Schroeder, Nathan Stano, Graham Kozak Teacher: Ardis Herrold
Methods of Determining Relative Age of Young Stellar Objects Zak Schroeder, Nathan Stano, Graham Kozak Teacher: Ardis Herrold ABSTRACT The main goal of the project was to study various types of Young Stellar
More informationLecture Three: Stellar Populations. Stellar Properties: Stellar Populations = Stars in Galaxies. What defines luminous properties of galaxies
Lecture Three: ~2% of galaxy mass in stellar light Stellar Populations What defines luminous properties of galaxies face-on edge-on https://www.astro.rug.nl/~etolstoy/pog16/ 18 th April 2016 Sparke & Gallagher,
More informationEmission Lines in the Spectrum of the 3 He Star 3 Cen A
Emission Lines in the Spectrum of the 3 He Star 3 Cen A T. A. A. Sigut, J. D. Landstreet and S. L. S. Shorlin Department of Physics and Astronomy, The University of Western Ontario Received ; accepted
More informationAtlas of CMFGEN Models for OB Massive Stars
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC, 127:428 436, 2015 May 2015. The Astronomical Society of the Pacific. All rights reserved. Printed in U.S.A. Atlas of CMFGEN Models for OB Massive
More informationChemical abundances of planet-host stars. Results for alpha and Fe-group elements. 1 With probably the only exception being the studies of beryllium
A&A 404, 715 727 (2003) DOI: 10.1051/0004-6361:20030543 c ESO 2003 Astronomy & Astrophysics Chemical abundances of planet-host stars Results for alpha and Fe-group elements A. Bodaghee 1,N.C.Santos 1,2,
More informationAbundance structure of the atmospheres of magnetic CP stars
Abundance structure of the atmospheres of magnetic CP stars T.A. Ryabchikova Institute of Astronomy, Russian Academy of Sciences Moscow, Russia Institute for Astronomy, Vienna University Vienna, Austria
More informationNeutron-capture element abundances in the globular clusters: 47 Tuc, NGC 6388, NGC 362 & ω Cen
Neutron-capture element abundances in the globular clusters: 47 Tuc, NGC 6388, NGC 362 & ω Cen C. C. Worley Université de Nice Sophia Antipolis, CNRS (UMR 6202), Observatoire de la Côte d Azur, Cassiopée,
More informationarxiv: v1 [astro-ph.sr] 28 Jan 2011
The proceedings of the Physics of Accreting Compact Binaries 1 Cyclotron Modeling of the Polar CP Tuc Claudia V. Rodrigues, 1 Joaquim E. R. Costa, 1 Karleyne M. G. Silva, 1 Cleber A. de Souza, 1 Deonisio
More informationMeasurement of the stellar irradiance
Measurement of the stellar irradiance Definitions Specific Intensity : (monochromatic) per unit area normal to the direction of radiation per unit solid angle per unit wavelength unit (or frequency) per
More informationOn the Red Edge of the δ Scuti Instability Strip
Chin. J. Astron. Astrophys. Vol. 2 (2002), No. 5, 441 448 ( http: /www.chjaa.org or http: /chjaa.bao.ac.cn ) Chinese Journal of Astronomy and Astrophysics On the Red Edge of the δ Scuti Instability Strip
More informationGeometry of giant star model atmospheres: a consistency test. U. Heiter and K. Eriksson
A&A 452, 1039 1048 (2006) DOI: 10.1051/0004-6361:20064925 c ESO 2006 Astronomy & Astrophysics Geometry of giant star model atmospheres: a consistency test U. Heiter and K. Eriksson Department of Astronomy
More informationScience Olympiad Astronomy C Division Event National Exam
Science Olympiad Astronomy C Division Event National Exam University of Nebraska-Lincoln May 15-16, 2015 Team Number: Team Name: Instructions: 1) Please turn in all materials at the end of the event. 2)
More informationarxiv:astro-ph/ v1 6 Nov 2002
ACCEPTED IN APJL. TO BE APPEAR IN DEC. 10TH ISSUE Preprint typeset using L A TEX style emulateapj v. 14/09/00 LITHIUM DEPLETION BOUNDARY IN A PRE-MAIN SEQUENCE BINARY SYSTEM INSEOK SONG 1,2, M. S. BESSELL
More informationA new spectroscopic calibration to determine T eff and [Fe/H] of FGK dwarfs and giants
A new spectroscopic calibration to determine T eff and [Fe/H] of FGK dwarfs and giants G.D.C.Teixeira 1,2,, S. G. Sousa 1, M. Tsantaki 1,3, M.J.P.F.G.Monteiro 1,2, N. C. Santos 1,2, and G. Israelian 4,5
More informationCNO abundances in the Sun and Solar Twins
CNO abundances in the Sun and Solar Twins Jorge Meléndez Departamento de Astronomia, IAG, Universidade de São Paulo Sunset in Paracas, Peru (c) www.flickr.com/photos/rodrigocampos/ Why are C, N, O (and
More informationParallax: Space Observatories. Stars, Galaxies & the Universe Announcements. Stars, Galaxies & Universe Lecture #7 Outline
Stars, Galaxies & the Universe Announcements HW#4: posted Thursday; due Monday (9/20) Reading Quiz on Ch. 16.5 Monday (9/20) Exam #1 (Next Wednesday 9/22) In class (50 minutes) first 20 minutes: review
More informationTests of MATISSE on large spectral datasets from the ESO Archive
Tests of MATISSE on large spectral datasets from the ESO Archive Preparing MATISSE for the ESA Gaia Mission C.C. Worley, P. de Laverny, A. Recio-Blanco, V. Hill, Y. Vernisse, C. Ordenovic and A. Bijaoui
More information386 Brazilian Journal of Physics, vol. 30, no. 2, June, 2000 Atomic Transitions for the Doubly Ionized Argon Spectrum, Ar III 1 F. R. T. Luna, 2 F. Br
386 Brazilian Journal of Physics, vol. 30, no. 2, June, 2000 Atomic Transitions for the Doubly Ionized Argon Spectrum, Ar III 1 F. R. T. Luna, 2 F. Bredice, 3 G. H. Cavalcanti, and 1;4 A. G. Trigueiros,
More informationSearch for associations containing young stars (SACY) II. Chemical abundances of stars in 11 young associations in the solar neighborhood,
A&A 501, 965 971 (2009) DOI: 10.1051/0004-6361/200811194 c ESO 2009 Astronomy & Astrophysics Search for associations containing young stars (SACY) II. Chemical abundances of stars in 11 young associations
More informationSupergiant Studies out to Virgo & Fornax
Supergiant Studies out to Virgo & Fornax Norbert Przybilla R.P. Kudritzki, M.A. Urbaneja (IfA Hawaii), A. Seifahrt (Univ. Chicago), K. Butler (LMU Munich), M.F. Nieva (Bamberg), H.-U. Käufl, A. Kaufer
More information