Relevant bibliographies by topics / Stellar parameters

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  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers

Academic literature on the topic 'Stellar parameters'

Author: Grafiati
Published: 4 June 2021
Last updated: 1 February 2022

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Journal articles on the topic "Stellar parameters"

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Bruntt, Hans. "Accurate Fundamental Stellar Parameters." Proceedings of the International Astronomical Union 5, S265 (August 2009): 215–16. http://dx.doi.org/10.1017/s1743921310000591.

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AbstractWe combine results from interferometry, asteroseismology and spectroscopic analyses to determine accurate fundamental parameters (mass, radius and effective temperature) of 10 bright solar-type stars covering the H-R diagram from spectral type F5 to K1. Using “direct” techniques that are only weakly model-dependent we determine the mass, radius and effective temperature. We demonstrate that model-dependent or “indirect” methods can be reliably used even for relatively faint single stars for which direct methods are not applicable. This is important for the characterization of the targets of the CoRoT and Kepler space missions.
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Grootel, Valérie Van, Catarina S. Fernandes, Michael Gillon, Emmanuel Jehin, Jean Manfroid, Richard Scuflaire, Adam J. Burgasser, et al. "Stellar Parameters for Trappist-1." Astrophysical Journal 853, no. 1 (January 19, 2018): 30. http://dx.doi.org/10.3847/1538-4357/aaa023.

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Decin, L., Z. Shkedy, G. Molenberghs, M. Aerts, and C. Aerts. "Estimating stellar parameters from spectra." Astronomy & Astrophysics 421, no. 1 (June 11, 2004): 281–94. http://dx.doi.org/10.1051/0004-6361:20040127.

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Ge, Junqiang, Shude Mao, Youjun Lu, Michele Cappellari, and Renbin Yan. "Recovering stellar population parameters via different population models and stellar libraries." Monthly Notices of the Royal Astronomical Society 485, no. 2 (February 11, 2019): 1675–93. http://dx.doi.org/10.1093/mnras/stz418.

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Martins, F., M. Bergemann, J. M. Bestenlehner, P. A. Crowther, W. R. Hamann, F. Najarro, M. F. Nieva, et al. "SpS5 - II. Stellar and wind parameters." Proceedings of the International Astronomical Union 10, H16 (August 2012): 420–28. http://dx.doi.org/10.1017/s1743921314011788.

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AbstractThe development of infrared observational facilities has revealed a number of massive stars in obscured environments throughout the Milky Way and beyond. The determination of their stellar and wind properties from infrared diagnostics is thus required to take full advantage of the wealth of observations available in the near and mid infrared. However, the task is challenging. This session addressed some of the problems encountered and showed the limitations and successes of infrared studies of massive stars.
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GAO, HUA, HUA-WEI ZHANG, MAO-SHENG XIANG, YANG HUANG, XIAO-WEI LIU, A.-LI LUO, HAO-TONG ZHANG, et al. "ACCURACY OF LAMOST DR1 STELLAR PARAMETERS." Publications of The Korean Astronomical Society 30, no. 2 (September 30, 2015): 279–81. http://dx.doi.org/10.5303/pkas.2015.30.2.279.

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Ryabchikova, T. A., L. I. Mashonkina, A. R. Titarenko, S. A. Alexeeva, Yu V. Pakhomov, N. E. Piskunov, T. M. Sitnova, and B. A. Nizamov. "Testing SME determination of stellar parameters." Proceedings of the International Astronomical Union 9, S298 (May 2013): 436. http://dx.doi.org/10.1017/s1743921313007023.

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Miglio, A., and J. Montalbán. "Constraining fundamental stellar parameters using seismology." Astronomy & Astrophysics 441, no. 2 (September 19, 2005): 615–29. http://dx.doi.org/10.1051/0004-6361:20052988.

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Jordi, C., C. Fabricius, J. M. Carrasco, F. Figueras, E. Masana, H. Voss, and X. Luri. "Stellar parameters through high precision parallaxes." Proceedings of the International Astronomical Union 3, S248 (October 2007): 500–501. http://dx.doi.org/10.1017/s1743921308019947.

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AbstractBefore Hipparcos, the determination of absolute luminosity was usually done through calibrations based on a few stellar parallaxes measured at the highest precision. The Hipparcos mission meant a giant step on the knowledge of luminosities and fine structure of the HR diagram. The Gaia mission will go an enormous step further. Besides luminosities, Gaia will allow us to derive other stellar parameters like temperature and extinction, gravity, chemical composition, age and mass by the combination of astrometric and spectrometric data. Through simulations during the mission preparation, it has been shown that the astrometric parallax information is essential to deal with the degeneracy between gravity and chemical composition ([Fe/H] and [α/Fe]), that cannot be treated using only spectrophotometry. We show the expected HR diagram for the Gaia domain and the accuracies of stellar parameters.
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Gould, Andrew. "Stellar Halo Parameters from 4588 Subdwarfs." Astrophysical Journal 583, no. 2 (February 2003): 765–75. http://dx.doi.org/10.1086/345446.

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Dissertations / Theses on the topic "Stellar parameters"

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van, Saders Jennifer Lynn. "Using Modern Stellar Observables to Constrain Stellar Parameters and the Physics of the Stellar Interior." The Ohio State University, 2014. http://rave.ohiolink.edu/etdc/view?acc_num=osu1404130939.

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Badenes, Carles, Christine Mazzola, Todd A. Thompson, Kevin Covey, Peter E. Freeman, Matthew G. Walker, Maxwell Moe, et al. "Stellar Multiplicity Meets Stellar Evolution and Metallicity: The APOGEE View." IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/627094.

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We use the multi-epoch radial velocities acquired by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey to perform a large-scale statistical study of stellar multiplicity for field stars in the Milky Way, spanning the evolutionary phases between the main sequence (MS) and the red clump. We show that the distribution of maximum radial velocity shifts (Delta RVmax) for APOGEE targets is a strong function of log g, with MS stars showing Delta RVmax as high as similar to 300 km s(-1), and steadily dropping down to similar to 30 km s(-1) for log g similar to 0, as stars climb up the red giant branch (RGB). Red clump stars show a distribution of Delta RVmax values comparable to that of stars at the tip of the RGB, implying they have similar multiplicity characteristics. The observed attrition of high Delta RVmax systems in the RGB is consistent with a lognormal period distribution in the MS and a multiplicity fraction of 0.35, which is truncated at an increasing period as stars become physically larger and undergo mass transfer after Roche Lobe overflow during H-shell burning. The Delta RVmax distributions also show that the multiplicity characteristics of field stars are metallicity-dependent, with metal-poor ([Fe/H] less than or similar to -0.5) stars having a multiplicity fraction a factor of 2-3 higher than metal-rich ([Fe/H] less than or similar to 0.0) stars. This has profound implications for the formation rates of interacting binaries observed by astronomical transient surveys and gravitational wave detectors, as well as the habitability of circumbinary planets.
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Burke, Christopher J. "Survey for transiting extrasolar planets in stellar systems stellar and planetary content of the Open Cluster NGC 1245 /." Columbus, Ohio : Ohio State University, 2005. http://rave.ohiolink.edu/etdc/view?acc%5Fnum=osu1132168623.

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Ireland, Lewis George. "Stellar models with magnetism and rotation : mixing length theories and convection simulations." Thesis, University of Exeter, 2018. http://hdl.handle.net/10871/34350.

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Some low-mass stars appear to have larger radii than predicted by standard 1D structure models; prior work has suggested that inefficient convective heat transport, due to rotation and/or magnetism, may ultimately be responsible. In this thesis, we explore this possibility using a combination of 1D stellar models, 2D and 3D simulations, and analytical theory. First, we examine this issue using 1D stellar models constructed using the Modules for Experiments in Stellar Astrophysics (MESA) code. We begin by considering standard models that do not explicitly include rotational/magnetic effects, with convective inhibition modelled by decreasing a depth-independent mixing length theory (MLT) parameter αMLT. We provide formulae linking changes in αMLT to changes in the interior specific entropy, and hence to the stellar radius. Next, we modify the MLT formulation in MESA to mimic explicitly the influence of rotation and magnetism, using formulations suggested by Stevenson (1979) and MacDonald and Mullan (2014) respectively. We find rapid rotation in these models has a negligible impact on stellar structure, primarily because a star’s adiabat, and hence its radius, is predominantly affected by layers near the surface; convection is rapid and largely uninfluenced by rotation there. Magnetic fields, if they influenced convective transport in the manner described by MacDonald and Mullan (2014), could lead to more noticeable radius inflation. Finally, we show that these non-standard effects on stellar structure can be fabricated using a depth-dependent αMLT: a non-magnetic, non-rotating model can be produced that is virtually indistinguishable from one that explicitly parameterises rotation and/or magnetism using the two formulations above. We provide formulae linking the radially-variable αMLT to these putative MLT reformulations. We make further comparisons between MLT and simulations of convection, to establish how heat transport and stellar structure are influenced by rotation and magnetism, by looking at the entropy content of 2D local and 3D global convective calculations. Using 2D “box in a star” simulations, created using the convection code Dedalus, we investigate changes in bulk properties of the specific entropy for increasingly stratified domains. We observe regions stable against convection near the bottom boundary, resulting in the specific entropy in the bulk of the domain exceeding the bottom boundary value: this could be a result of physical effects, such as increased amounts of viscous dissipation for more supercritical, highly stratified cases, but may also be influenced by the artificial boundary conditions imposed by these local simulations. We then turn to 3D global simulations, created using the convection code Rayleigh, and investigate these same properties as a function of rotation rate. We find the average of the shell-averaged specific entropy gradient in the middle third of the domain to scale with rotation rate in a similar fashion to the scaling law derived via MLT arguments in Barker et al. (2014), i.e., |⟨ds/dr⟩| ∝ Ω^4/5.
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Gazzano, Jean-christophe. "Populations stellaires et systèmes planétaires observés par CoRoT." Thesis, Aix-Marseille 1, 2011. http://www.theses.fr/2011AIX10031/document.

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Dans le cadre de ma thèse, j'ai effectué l'analyse spectrale d'un échantillon massif de spectres stellaires dans le contexte du programme exoplanète de la mission CoRoT. J'ai tiré avantage des instruments Flames/GIRAFFE pour observer près de 2000 étoiles dans le but de comprendre les populations stellaires dans les champs CoRoT. Dans ce but, j'ai implémenté, calibré, testé, et appliqué une chaîne de traitement et de réduction fiable et efficace afin de réduire et d'analyser automatiquement (en utilisant l'algorithme de paramétrisation MATISSE, Gazzano et al. 2010) un large échantillon de spectres stellaires. J'ai déterminé la vitesse barycentrique radiale, une estimation de la vitesse de rotation projetée sur la ligne de visée, la température effective, la gravité de surface, de la métallicité global et l'enrichissement des éléments par rapport au fer pour 1 227 étoiles dans trois des champs CoRoT. Ainsi, j'ai construit un des premiers échantillons affranchis de biais de sélection pour toute étude concernant la relation planète métallicité dans les champs CoRoT et démontré que le nombre des étoiles naines a été généralement sous-estimé par la classification photométrique (Exo-Dat, Deleuil et al. 2009). J'ai appliqué la relation reliant le nombre de planètes détectées à la métallicité de l'étoile hôte (Udry & Santos 2007), parfaitement en accord avec le nombre actuel de détection planétaire dans les champs CoRoT correspondant (Gazzano et al. 2010). En utilisant les paramètres atmosphériques MATISSE, nous avons déterminé les distances et nous les avons combinées avec des informations cinématiques (les mouvements propres du catalogue PPMXL - Roeser et al. (2010), et l'astrométrie). Nous avons dérivé les composantes de cinématique Galactique : position et vitesse. Cela m'a permis d'étudier les populations stellaires dans les champs CoRoT /exoplanète et de quantifier le gradient de métallicité dans la Galaxie (Gazzano et al. En préparation). J'ai par ailleurs montré que les étoiles à planètes détectées dans les champs considérés pour ma thèse sont exclusivement des étoiles de disque mince. J'ai également participé au suivi des candidats planète CoRoT à l'aide de spectroscopie à haute résolution. J'ai effectué l'analyse spectrale, avec le logiciel VWA (Bruntt et al. 2010b,a), des étoiles hôtes pour la mission spatiale CoRoT. Ces études ont conduit à la détermination des paramètres fondamentaux de l'étoile, qui est une étape indispensable pour la caractérisation complète de la planète
During my Ph.D., I performed the spectral analysis of a massive sample of stellar spectra in the context of the CoRoT /Exoplanet mission. We took advantage of the Flames/GIRAFFE multi-fibre instrument to observe almost 2 000 stars with the aim of understanding the stellar populations in the CoRoT fields. To these purposes, I implemented, calibrated, tested and applied an automatic pipeline to reduce and analyse automatically (using the parameterization algorithm MATISSE, Gazzano et al. 2010) a large sample of stellar spectra. I derived the barycentric radial velocity, an estimate of the rotational velocity projected on the line of sight, the effective temperature, the surface gravity, the overall metallicity and the -enhancement for 1227 stars in three of the CoRoT fields. Hence, I built one of the first unbiased samples for any study regarding planet metallicity relationship in the CoRoT fields and demonstrated that the amount of dwarf stars was generally underestimated by the photometric classification (in Exo-Dat, Deleuil et al. 2009). I applied the relationship linking the number of planets as a function of the metallicity of the host star (Udry & Santos 2007), totally in agreement with the current number of planetary detection in the corresponding CoRoT fields (Gazzano et al. 2010). Using MATISSE atmospheric parameters, we determined distances and combining them with kinematics information (proper motions from PPMXL catalogue - Roeser et al. (2010) and astrometry), we derived Galactic kinematics components : position, velocities and orbits. This allowed me to study the stellar populations in the CoRoT /Exoplanet fields and quantify the metallicity gradient in the Galaxy (Gazzano et al. in preparation). I also participated to the spectroscopic follow-up observations of CoRoT planetary candidates with high resolution spectroscopy, to the spectroscopic analysis, with the VWA software (Bruntt et al. 2010b,a), of planet hosting stars for the CoRoT space mission and to their characterisation and publication. Indeed, the determination of the fundamental parameters of the star is a mandatory step for the complete characterisation of the planet
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Martinez, Arturo O., Ian J. M. Crossfield, Joshua E. Schlieder, Courtney D. Dressing, Christian Obermeier, John Livingston, Simona Ciceri, et al. "Stellar and Planetary Parameters for K2's Late-type Dwarf Systems from C1 to C5." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623204.

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The NASA K2 mission uses photometry to find planets transiting stars of various types. M dwarfs are of high interest since they host more short-period planets than any other type of main-sequence star and transiting planets around M dwarfs have deeper transits compared to other main-sequence stars. In this paper, we present stellar parameters from K and M dwarfs hosting transiting planet candidates discovered by our team. Using the SOFI spectrograph on the European Southern Observatory's New Technology Telescope, we obtained R approximate to 1000 J-, H-, and K-band (0.95-2.52 mu m) spectra of 34 late-type K2 planet and candidate planet host systems and 12 bright K4-M5 dwarfs with interferometrically measured radii and effective temperatures. Out of our 34 late-type K2 targets, we identify 27 of these stars as M dwarfs. We measure equivalent widths of spectral features, derive calibration relations using stars with interferometric measurements, and estimate stellar radii, effective temperatures, masses, and luminosities for the K2 planet hosts. Our calibrations provide radii and temperatures with median uncertainties of 0.059 R-circle dot (16.09%) and 160 K (4.33%), respectively. We then reassess the radii and equilibrium temperatures of known and candidate planets based on our spectroscopically derived stellar parameters. Since a planet's radius and equilibrium temperature depend on the parameters of its host star, our study provides more precise planetary parameters for planets and candidates orbiting late-type stars observed with K2. We find a median planet radius and an equilibrium temperature of approximately 3 R-circle plus and 500 K, respectively, with several systems (K2-18b and K2-72e) receiving near-Earth-like levels of incident irradiation.
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Neilson, Hilding R., and Richard Ignace. "Period Change and Stellar Evolution of β Cephei Stars." Digital Commons @ East Tennessee State University, 2015. https://dc.etsu.edu/etsu-works/2689.

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The β Cephei stars represent an important class of massive star pulsators that probe the evolution of B-type stars and the transition from main sequence to hydrogen-shell burning evolution. By understanding β Cep stars, we gain insights into the detailed physics of massive star evolution, including rotational mixing, convective core overshooting, magnetic fields, and stellar winds, all of which play important roles. Similarly, modeling their pulsation provides additional information into their interior structures. Furthermore, measurements of the rate of change of pulsation period offer a direct measure of β Cephei stellar evolution. In this work, we compute state-of-the-art stellar evolution models assuming different amounts of initial rotation and convective core overshoot and measure the theoretical rates of period change, that we compare to rates previously measured for a sample of β Cephei stars. The results of this comparison are mixed. For three stars, the rates are too low to infer any information from stellar evolution models, whereas for three other stars the rates are too high. We infer stellar parameters, such as mass and age, for two β Cephei stars: ξ1 CMa and δ Cet, which agree well with independent measurements. We explore ideas for why models may not predict the higher rates of period change. In particular, period drifts in β Cep stars can artificially lead to overestimated rates of secular period change.
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Posbic, Hélène. "Automatic stellar parameters determination : chemical characterization of the Galactic thick disk and preparation to the Gaia mission." Observatoire de Paris, 2012. https://hal.science/tel-02095129.

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La formation de la Voie Lactée est toujours une question ouverte. Plusieurs scénarios sont proposés. Les différents scénarios prédisent différentes caractéristiques chimiques du disque. Cette thèse a pour but de caractériser chimiquement le disque de la Voie Lactée, dans et en dehors du voisinage solaire, pour contraindre les scénarios de formation de disque. Ceci sera possible grâce à des spectres stellaires de haute résolution de 200 étoiles qui ont été observées avec le spectographe Giraffe sur le Very Large Telescope (VLT). Ces étoiles ont été sélectionnées de sorte à avoir des altitudes galactiques ǀZǀ qui couvrent en espace le disque mince et le disque épais (ǀZǀ jusqu'à 2 kpc). Un nouveau logiciel d'analyse automatique de spectres a été dévoloppé pour déterminer les paramètres stellaires de ces étoiles, plus particulièrement leurs abondances individuelles. SPADES (Stellar PArameters DEtermination Software) est basé sur une analyse raie par raie qui utilise une grille de spectres de référence synthétiques. Une des particularités de SPADES est sa capacité à calculer des spectres synthétiques à la volée. Une fois testé pour déterminer les erreurs internes et externes de la méthode, SPADES a été utilisé pour déterminer les vitesses radiales, températures effectives, gravités de surface, métallicités et abondances individuelles de l'chantillon d'étoiles. Les distances de ces étoiles ont également été déterminées. La fonction de distribution de métallicité du disque a été calculée en utilisant cet échantillon d'étoiles. Elle montre une majorité d'étoiles du disque épais, avec une transition lisse de la métallicité au niveau de l'interface disque épais/halo. Le comportement vertical de la fonction de distribution de métallicité a aussi été étudié. Un grandient vertical de metallicité dans le disque de valeur 0. 19 +/- 0. 14 dex/kpc a été marginalement détecté avec un niveau sigma de 1. 4. Les tendance de [Ti/Fe] et [Ca/Fe] par à [Fe /H] pour les étoiles à moinns de 1 kpc au dessus du plan sont en bon accord avec celles d'études précédentes. Ceci fut la conclusion de la comparaison entre ce travail et celui des auteurs : Bensby et al. (2005), Takeda (2007), et Neves et al. (2009). Le résultat principal de l'analyse est que les tendances de [Ca/Fe] vs [Fe/H] et [Ti/Fe] vs [Fe/H] sont similaires aux basses altitudes (i. E. ǀZǀ < 1 kpc) et aux altitudes plus hautes (1 < ǀZǀ < 2. 5 kpc). Ceci laisse suggérer que les gaz et les étoiles du disque épais ont été enrichis par la même proportion de super novae de type II et type I proche du plan Galactique et jusqu'à des altitudes de 2. 5 kpc et plus. Ces résultats appuient les scénarios de formation du disque épais du genre "collapse" ou accrétion de gaz défavorisant l'idée d'un disque épais formé par capture pendant la fusion
The formation of the Milky Way disk is still an open question. Many scenarios are proposed. Different formation scenarios predict different disk chemical trends. This thesis aims to chemically characterize the Milky Way disk inside and outside the solar neighbourhood, to better constrain its formation scenario. This is possible thanks to high resolution spectra of 200 disk stars observed using the Giraffe spectograph on the Very Large Telescope (VLT). They were selected to have galactic altitudes ǀZǀ that cover both the thin and tick disk (ǀZǀ up to 2 kpc). A new automatic spectra analysis software was developed to determine the stellar parameters, and most importantly, the elemental abundances of these stars. SPADES (Stellar PArameters DEtermination Software) is based on a line-by-line analysis using a reference grid of synthetic stellar spectra. One of its particularities is its ability to calculate synthetic spectra on-the-y. Once tested for internal and external errors, it was used to determine the radial velocity, effective temperature, surface gravity, metallicity and elemental abundances of the smple stars. The distances of these stars were also determined. The metallicity distribution function of the disk using this sample was calculated. It showed a large contribution of the disk stars and a smooth transition at the metallicity of the thick disk/halo interface. The vertivcal behaviour of the metallicity distribution function was also studied. A vertical metallicity grandient in the disk of 0. 19 +/- 0. 14 dex/kpc was marginally detected at the 1. 4 sigma level. The [Ti/Fe] and [Ca/Fe] vs [Fe/H] trends for stars located at less than 1 kpc above the plane were found to be in good agreement with previous studies. This is conclusion from the comparison of this work with author's like Bensky et al. (2005), Takeda (2007), and Neves et al. (2009). The main result of the analysis is that the trends of [Ca/Fe] vs [Fe/H] and [Ti/He] vs [Fe/H] show no significant difference close (i. E. ǀZǀ < 1 kpc) and farther away (1 < ǀZǀ < 2. 5 kpc) from the Galactic plane. This suggests that the thick disk gas and stars have been enriched by the same proportion of type II and type I super-novae from the galactic plane up to at least 2. 5 kpc. These results support thick disk formation scenarios like collapse or gas-rich accretion and disfavour a thick disc formed of stars captured during merger event
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Ekanayake, Gemunu. "Determination of Stellar Parameters through the Use of All Available Flux Data and Model Spectral Energy Distributions." UKnowledge, 2017. http://uknowledge.uky.edu/physastron_etds/44.

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Basic stellar atmospheric parameters, such as effective temperature, surface gravity, and metallicity plays a vital role in the characterization of various stellar populations in the Milky Way. The Stellar parameters can be measured by adopting one or more observational techniques, such as spectroscopy, photometry, interferometry, etc. Finding new and innovative ways to combine these observational data to derive reliable stellar parameters and to use them to characterize some of the stellar populations in our galaxy is the main goal of this thesis. Our initial work, based on the spectroscopic and photometric data available in literature, had the objective of calibrating the stellar parameters from a range of available flux observations from far-UV to far-IR. Much effort has been made to estimate probability distributions of the stellar parameters using Bayesian inference, rather than point estimates. We applied these techniques to blue straggler stars (BSSs) in the galactic field, which are thought to be a product of mass transfer mechanism associated with binary stars. Using photometry available in SDSS and GALEX surveys we identified 85 stars with UV excess in their spectral energy distribution (SED) : indication of a hot white dwarf companion to BSS. To determine the parameter distributions (mass, temperature and age) of the WD companions, we developed algorithms that could fit binary model atmospheres to the observed SED. The WD mass distribution peaks at 0.4M , suggests the primary formation channel of field BSSs is Case-B mass transfer, i.e. when the donor star is in red giant phase of its evolution. Based on stellar evolutionary models, we estimate the lower limit of binary mass transfer efficiency β ~ 0.5. Next, we have focused on the Canis Major overdensity (CMO), a substructure located at low galactic latitude in the Milky Way, where the interstellar reddening (E(B-V )) due to dust is significantly high. In this study we estimated the reddening, metallicity distribution and kinematics of the CMO using a sample of red clump (RC) stars. The averageE(B-V)(~0.19)is consistent with that measured from Schlegel maps (Schlegal et.al. 1998). The overall metallicity and kinematic distribution is in agreement with the previous estimates of the disk stars. But the measured mean alpha element abundance is relatively larger with respect to the expected value for disk stars.
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Bruno, Giovanni. "Characterization of transiting exoplanets : analyzing the impact of the host star on the planet parameters." Thesis, Aix-Marseille, 2015. http://www.theses.fr/2015AIXM4746/document.

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Dans le cadre de ma thèse, j’ai analysé les spectres de neuf étoiles Kepler obtenus avec les relevés de vitesse radiale (VR). Cela a permis la caractérisation de leur compagnons planétaires. J’ai analysé les spectres de 21 autres étoiles CoRoT et Kepler, probablement hôtes de naines M à faible masse. Cela a permis d’'élargir l'échantillon des étoiles à faible masse avec masse et rayon mesurés. J’ai calculé l’indice d’activité chromosphérique de 31 étoiles observées avec SOPHIE/OHP, en aidant l’étude des interactions étoile-planète. J’ai étudié le comportement de SOPHIE à bas signal à bruit (S/B). J’ai déterminé l’intervalle de S/B dans lequel un spectre stellaire est fiable pour la mesure des paramètres stellaires.Dans le cadre du consortium SOPHIE, j’ai suivi l’analyse complète du système Kepler-117. Ce système multi-planétaire montre variations des périodes orbitaux dues aux échanges dynamiques entre les planètes (TTV). Pour déterminer les paramètres du système, un approche spécifique a été développé pour l’ajustement simultané de transits, VR et TTV (Bruno et al. 2015).Finalement, je me suis intéressé à l’activité stellaire dans la photométrie de transit. J’ai impl ́ementé deux logiciels de modélisation de tâches stellaires dans un code MCMC, en ajoutant l’évolution des tâches dans l’un d’eux. J’ai appliqué les logiciels au Soleil, à CoRoT-7 et à CoRoT-2. J’ai amené un étude détaillé de la courbe de lumière de CoRoT-2, et exploré les effets des tâches dans les paramètres du transit (Bruno et al., en prep.). Avec la méthode FF’ (Aigrain et al. 2012), j’ai contribué à l’exploration du lien entre la signature des tâches de CoRoT-7 et dans la photométrie et dans les VR
During my PhD, I analyzed the spectra of nine Kepler stars obtained by radial velocity (RV) observations. This allowed the characterization of their planetary companions. I analyzed the spectra of twenty-one other CoRoT and Kepler stars, likely orbited by low-mass M dwarfs. This helped widening the sample of low-mass stars with measured mass and radius. I calculated the chromospheric activity indfex of thirty-one stars observed with SOPHIE/OHP, helping the study of star-planet interactions. I studied the behavior of SOPHIE in low signal-to-noise ratio (SNR) regime. I determinhed the SNR range in which a stellar spectrum is reliable for the measure of the stellar parameters.Within the SOPHIE consortium, I followed the complete analysis of the Kepler-117 system. This multi-planetary system presents variations in the planetary orbital periods due to their mutual dynamical interacion (TTVs). To fit the system parameters, a specific fitting approach including TTV modeling was developed. We derived the system parameters by the simultaneous fit of transits, RVs, and TTVs (Bruno et al. 2015).Finally, I addressed the problem of stellar activity in transit photometry. I implemented two starspot modeling codes into an MCMC algorithm, adding spot evolution to oneof them. I applied the codes to the Sun, CoRoT-7, and CoRoT-2. I carried an extensive study on the light curve of CoRoT-2, and explored the effects of the spots on the transit parameters (Bruno et al., in prep.). With the FF’ method (Aigrain et al. 2012), I contributed to explore the connection between the photometric and RV signature of starspots in CoRoT-7
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Books on the topic "Stellar parameters"

1

Stern, Robert A. Investigation of physical parameters in stellar flares observed by Ginga. [Washington, DC: National Aeronautics and Space Administration, 1994.

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D, Garmany C., Shull J. Michael, and United States. National Aeronautics and Space Administration., eds. The Lyman-continuum fluxes and stellar parameters of O and early B-type stars. [Washington, DC: National Aeronautics and Space Administration, 1996.

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D, Garmany C., Shull J. Michael, and United States. National Aeronautics and Space Administration., eds. The Lyman-continuum fluxes and stellar parameters of O and early B-type stars. [Washington, DC: National Aeronautics and Space Administration, 1996.

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D, Garmany C., Shull J. Michael, and United States. National Aeronautics and Space Administration., eds. The Lyman-continuum fluxes and stellar parameters of O and early B-type stars. [Washington, DC: National Aeronautics and Space Administration, 1996.

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United States. National Aeronautics and Space Administration., ed. Investigation of physical parameters in stellar flares observed by Ginga. [Washington, DC: National Aeronautics and Space Administration, 1994.

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United States. National Aeronautics and Space Administration., ed. Investigation of physical parameters in stellar flares observed by Ginga: Final report submitted to ... Marshall Space Flight Center ... [Washington, DC: National Aeronautics and Space Administration, 1994.

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United States. National Aeronautics and Space Administration., ed. Investigation of physical parameters in stellar flares observed by Ginga: Final report submitted to ... Marshall Space Flight Center ... [Washington, DC: National Aeronautics and Space Administration, 1994.

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Book chapters on the topic "Stellar parameters"

1

Van De Kamp, Peter. "Stellar Parameters." In Dark Companions of Stars, 244–50. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4692-7_5.

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Smalley, Barry. "Stellar Parameters from Photometry." In Determination of Atmospheric Parameters of B-, A-, F- and G-Type Stars, 111–20. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-06956-2_10.

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Jordi, C., J. M. Carrasco, F. Figueras, J. Torra, X. Luri, and E. Masana. "GAIA: Derivation of Stellar Parameters." In Highlights of Spanish Astrophysics III, 481. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-1778-6_124.

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Salukvadze, G. N., and G. SH Javakhishvili. "Some Physical Parameters and UV BY β Photometry of Trapezium Type Multiple Systems." In Stellar Populations, 378. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-011-0125-7_53.

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Bailer-Jones, C. A. L. "Determination of Stellar Parameters with GAIA." In Census of the Galaxy: Challenges for Photometry and Spectrometry with GAIA, 21–29. Dordrecht: Springer Netherlands, 2002. http://dx.doi.org/10.1007/978-94-010-0361-2_3.

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Massaglia, Silvano. "Constraining the Parameters of Agn Jets." In Jets in Young Stellar Objects, 223–33. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-007-0999-7_37.

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Hauck, B. "Calibration in Temperature of Photometric Parameters." In Calibration of Fundamental Stellar Quantities, 271–84. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5456-4_16.

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Gustafsson, Bengt, and Uffe Graae-Jørgensen. "Fundamental Parameters and Models of Stellar Atmospheres." In Calibration of Fundamental Stellar Quantities, 303–29. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5456-4_18.

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Petersen, J. O. "On the Application of Fourier Decomposition Parameters." In Nonlinear Phenomena in Stellar Variability, 157–58. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-1062-4_20.

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Santos, Nuno C., and Lars A. Buchhave. "Accurate Stellar Parameters for Radial Velocity Surveys." In Handbook of Exoplanets, 1–18. Cham: Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-30648-3_181-1.

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Conference papers on the topic "Stellar parameters"

1

Korn, Andreas. "Stellar parameters and abundances." In 11th Symposium on Nuclei in the Cosmos. Trieste, Italy: Sissa Medialab, 2011. http://dx.doi.org/10.22323/1.100.0301.

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Blay, Georgina, and Catherine Lovekin. "Determination of stellar parameters using binary system models." In INTERNATIONAL CONFERENCE OF COMPUTATIONAL METHODS IN SCIENCES AND ENGINEERING 2015 (ICCMSE 2015). AIP Publishing LLC, 2015. http://dx.doi.org/10.1063/1.4937704.

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Korn, Andreas J., Lyudmila Mashonkina, Olivier Richard, Anna Frebel, Wako Aoki, and Norbert Christlieb. "HE 1327—2326: Stellar Parameters, Atomic Diffusion and Lithium abundance." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905530.

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Zhang, Hongying, Liangping Tu, and Ke Lu. "Automatic Estimation of Stellar Atmospheric Parameters Based on Extremely Randomized Trees." In 2019 12th International Congress on Image and Signal Processing, BioMedical Engineering and Informatics (CISP-BMEI). IEEE, 2019. http://dx.doi.org/10.1109/cisp-bmei48845.2019.8965811.

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Evans, Nancy Remage, Joyce Ann Guzik, and Paul A. Bradley. "Fundamental Parameters of Cepheids: Masses and Multiplicity." In STELLAR PULSATION: CHALLENGES FOR THEORY AND OBSERVATION: Proceedings of the International Conference. AIP, 2009. http://dx.doi.org/10.1063/1.3246577.

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Jin, Xu, Liangping Tu, and Ke Lu. "Kpca-Ent:A New Method for Automatic Measurement of Stellar Atmospheric Physical Parameters." In 2019 12th International Congress on Image and Signal Processing, BioMedical Engineering and Informatics (CISP-BMEI). IEEE, 2019. http://dx.doi.org/10.1109/cisp-bmei48845.2019.8966061.

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Prieto, Carlos Allende, and Coryn A. L. Bailer-Jones. "Stellar Atmospheric Parameters: The Four-Step Program and Gaia’s Radial Velocity Spectrometer." In CLASSIFICATION AND DISCOVERY IN LARGE ASTRONOMICAL SURVEYS: Proceedings of the International Conference: “Classification and Discovery in Large Astronomical Surveys”. AIP, 2008. http://dx.doi.org/10.1063/1.3059081.

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Barcza, S., J. M. Benkő, Joyce Ann Guzik, and Paul A. Bradley. "Physical Parameters of RR Lyrae Stars from Multicolor Photometry and Kurucz Atmospheric Models." In STELLAR PULSATION: CHALLENGES FOR THEORY AND OBSERVATION: Proceedings of the International Conference. AIP, 2009. http://dx.doi.org/10.1063/1.3246455.

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Sousa, S. G., N. C. Santos, M. Mayor, S. Udry, L. Casagrande, G. Israelian, F. Pepe, D. Queloz, M. J. P. F. G. Monteiro, and Eric Stempels. "Spectroscopic parameters for 451 stars in the HARPS GTO planet search program: Stellar [Fe∕H] and the frequency of exo-Neptunes." In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099152.

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Du, Bing, Ali Luo, JianNan Zhang, Yue Wu, and FengFei Wang. "Comparison of different interpolation algorithm in feature-based template matching for stellar parameters analysis." In SPIE Astronomical Telescopes + Instrumentation, edited by Nicole M. Radziwill and Gianluca Chiozzi. SPIE, 2012. http://dx.doi.org/10.1117/12.925970.

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