Relevant bibliographies by topics / Solar-type star

Contents

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

Academic literature on the topic 'Solar-type star'

Author: Grafiati
Published: 4 June 2021
Last updated: 19 February 2022

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Journal articles on the topic "Solar-type star"

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Smith, Keith T. "Is the Sun a solar-type star?" Science 357, no. 6347 (2017): 159.1–159. http://dx.doi.org/10.1126/science.357.6347.159-a.

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Mirzoyan, L. V. "Flare stars in star clusters, associations and solar vicinity." Symposium - International Astronomical Union 137 (1990): 1–13. http://dx.doi.org/10.1017/s0074180900187303.

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The observational data on flare stars observed in star clusters and associations as well as in the solar vicinity (the UV Ceti type stars) are discussed. The analysis of these data show that they constitute one common class of objects possessing flare activity and the differences between them are conditioned by the age differences. The stage of flare activity is an evolutionary stage, one of the earliest stages of evolution passed by all red dwarf stars. It comes before the end of their T Tau stage of evolution. The UV Ceti type flare stars in the solar vicinity seem to be the population of the general galactic field, which were formed in the systems, already desintegrated. Most probably the stellar flares are the result of the release of the the surplus energy having intra-stellar origin.
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He, Han, Huaning Wang, Yan Yan, and Duo Yun. "Magnetic Activity Discrepancies of Solar-Type Stars Revealed by Kepler Light Curves." Proceedings of the International Astronomical Union 13, S335 (2017): 7–10. http://dx.doi.org/10.1017/s1743921317007670.

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AbstractMagnetic activity information is concealed in the shape of stellar light curves owing to the process of rotational modulation. We developed approaches to extract magnetic activity characteristics from stellar light curves, and applied the method to a solar-type star observed with Kepler space telescope and also to the Sun for comparison. The result reveals distinct magnetic activity discrepancies between the solar-type star and the Sun. (1) The light-curve periodicity of the solar-type star is generally stronger than that of the Sun. (2) For the solar-type star, when the range of light-curve fluctuation is larger, the periodicity is also higher; while for the Sun, only during the solar minima with minimal range of fluctuation, the light curves show some periodicity. We propose that on the solar-type star, it is the large-scale magnetic field that leads to the light curves with both high periodicity and large range of fluctuation.
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Roberts, Lewis C., Andrei Tokovinin, Brian D. Mason, William I. Hartkopf, and Reed L. Riddle. "OBSERVATIONS OF HIERARCHICAL SOLAR-TYPE MULTIPLE STAR SYSTEMS." Astronomical Journal 150, no. 4 (2015): 130. http://dx.doi.org/10.1088/0004-6256/150/4/130.

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Porto de Mello, G. F., and L. da Silva. "HR 6094: A Young Solar-Type, Solar-Metallicity Barium Dwarf Star." Astrophysical Journal 476, no. 2 (1997): L89—L92. http://dx.doi.org/10.1086/310504.

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da Silva, L., and G. F. Porto de Mello. "Lithium Abundances in Solar-Type Stars." Symposium - International Astronomical Union 198 (2000): 495–97. http://dx.doi.org/10.1017/s0074180900167142.

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We report Li abundances from the λ6707 line for 19 nearby dwarf and subgiant solar-type stars. The unevolved stars in this sample present high (> 2.00) Li abundances. We found a few cases of subgiant stars which present high Li content. The Sun seems to be part of a population of nearly unevolved stars which have depleted their Li to a high degree: all other metal-normal, near ZAMS stars in our sample show higher than solar Li content. There seems to be no correlation of the degree of Li depletion with mass, atmospheric parameters or state of evolution: as an example we found a star (HR1532) almost identical to the Sun in its state of evolution and atmospheric parameters, but with over ten times the solar Li abundance. We propose that different histories of angular momentum distribution at star birth, and/or post-birth angular momentum evolution, may account for these differences.
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Mayor, Michel, and Didier Queloz. "A Jupiter-mass companion to a solar-type star." Nature 378, no. 6555 (1995): 355–59. http://dx.doi.org/10.1038/378355a0.

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Soderblom, David R. "Determining the temperatures of solar-type stars - Do star spots produce color anomalies?" Astrophysical Journal 342 (July 1989): 823. http://dx.doi.org/10.1086/167639.

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Brown, Carolyn, Brad Carter, Stephen Marsden, and Ian Waite. "Starspots on Young Solar-Type Stars." Proceedings of the International Astronomical Union 9, S302 (2013): 148–49. http://dx.doi.org/10.1017/s1743921314001938.

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AbstractDoppler Imaging of starspots on young solar analogues is a way to investigate the early history of solar magnetic activity by proxy. Doppler images of young G-dwarfs have yielded the presence of large polar spots, extending to moderate latitudes, along with measurements of the surface differential rotation. The differential rotation measurement for one star (RX J0850.1-7554) suggests it is possibly the first example of a young G-type dwarf whose surface rotates as almost a solid body, in marked contrast to the differential rotation of other rapidly rotating young G-dwarfs and the present-day Sun. Overall, our Doppler imaging results show that the young Sun possessed a fundamentally different dynamo to today.
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Barker, Adrian J., and Gordon I. Ogilvie. "Internal wave breaking and the fate of planets around solar-type stars." Proceedings of the International Astronomical Union 6, S271 (2010): 363–64. http://dx.doi.org/10.1017/s1743921311017807.

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AbstractInternal gravity waves are excited at the interface of convection and radiation zones of a solar-type star, by the tidal forcing of a short-period planet. The fate of these waves as they approach the centre of the star depends on their amplitude. We discuss the results of numerical simulations of these waves approaching the centre of a star, and the resulting evolution of the spin of the central regions of the star and the orbit of the planet. If the waves break, we find efficient tidal dissipation, which is not present if the waves perfectly reflect from the centre. This highlights an important amplitude dependence of the (stellar) tidal quality factor Q′, which has implications for the survival of planets on short-period orbits around solar-type stars, with radiative cores.
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Dissertations / Theses on the topic "Solar-type star"

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Al-Edhari, Ali Jaber. "Complex organic molecules in solar-type star forming regions." Thesis, Université Grenoble Alpes (ComUE), 2016. http://www.theses.fr/2016GREAY048/document.

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Le but de la présente thèse est l'étude de la compléxité moléculaire dans les régions de formation stellaires. Cette thèse s'axe sur deux classes de molécule aux caractéristiques prébiotiques : les molécules organiques complexes et les cyanopolyynes.Dans ce contexte, j'ai analysé des données d'un seul échantillon de relevés spec- traux en exploitant des codes de transfert radiatif à l'équilibre thermodynamique local (LTE) et/ou non-LTE pour deux sources : une proto-étoile de type solaire dans un environnement calme (IRAS 16293-2422) et un proto-ama constitué de proto-étoile de type solaire (OMC2-FIR4).L'objectif est de trouver des similar- ités et des différences entre ces deux cas.J'ai utilisé des données issu de deux relevés spectraux : TIMASSS (The IRAS16293-2422 Millimeter And Submilimeter Spectral Survey) réalisés en 2011 (Caux et al. 2011), et ASAI(Astrochemical Surveys At IRAM) réalisés pen- dant la période 2013-2015 (eg Lopez-Sepulcre et al.2015). J'ai extrais les lignes (identification et intensité intégrée) en utilisant le paquet disponible publique- ment : CASSIS (Centre d'Analyse Scientifique de Spectres Infrarouges et Sub- millimetrique). Pour finir, j'ai utilisé le paquet GRAPES (GRenoble Analysis of Protostellar Envelope Spectral) afin de modéliser la distribution spectrale énergétique de ligne (SLED) des molécules détectées, mais aussi afin d'estimer leurs abondances à travers l'envelope de IRAS16293 et du coeur chaud OMC2- FIR4.Les principaux résultats de la thèse sont :1. Le premier recensement complet des molecules organiques complexes (COMs) dans IRAS162932. La première détéction de COMs dans l'enveloppe froide d'une proto-étoile de type solaire (IRAS16293-2422) supportant l'idée qu'un méchanisme de formation, relativement efficace pour les COMs détectées, doit exister en phase gazeuse froide.3. La découverte d'une fine corrélation entre le diméthyle-éther (DME) et le méthyle-formate (MF) suggère une relation mère fille entre ces deux espèces.4. La detection de formamide, espèce avec un très fort potentiel prébiotique, dans plusieurs protoétoiles incluant IRAS16293-2422 et OMC2-FIR4.5. Le recensement complet des cyanopolyynes dans IRAS16293 et OMC2- FIR4 avec la détection de HC3N, HC5N, DC3N et pour OMC2-FIR4: le C13 isotopologue du HC3N cyanopolyynes.Ces résultats sont le sujet principal de deux publications (Jaber et al.2014, ApJ; Lopez-Sepulcre, Jaber et al.2015,MNRAS), un article accepté (Jaber et al., A &amp; A) et un article à soumettre (Jaber et al. A &amp; A)<br>The present PhD thesis goal is the study of the molecular complexity in solar type star forming regions. It specifically focuses on two classes of molecules with a pre-biotic value, the complex organic molecules and the cyanopolyynes.At this scope, I analyzed data from single-dish spectral surveys by means of non-LTE or/and non-LTE radiative transfer codes in two sources, a solar type protostar in an isolated and quiet environment (IRAS16293-2422) and a proto-cluster of solar type protostars (OMC2-FIR4). The goal is to find similarities and differences between these two cases.I used data from two spectra surveys: TIMASSS (The IRAS16293-2422 Millimeter And Submillimeter Spectral Survey), which has been carried out in 2011 (Caux et al. 2011), and ASAI (Astrochemical Surveys At IRAM), which has been carried out in 2013-2015 (e.g. Lopez-Sepulcre et al. 2015).I extracted the lines (identification and integrated intensity) by means of the publicly available package CASSIS (Centre dAnalyse Scientifique de Spectres Infrarouges et Submillimtriques).Finally, I used the package GRAPES (GRenoble Analysis of Protostellar Envelope Spectra) to model the Spectral Line Energy Distribution (SLED) of the detected molecules, and to estimate their abundance across the envelope and hot corino of IRAS16293-2422 and OMC2-FIR4, respectively.The major results of the thesis are:1) The first full census of complex organic molecules (COMs) in IRAS16293-2422;2) The first detection of COMs in the cold envelope of a solar type protostar (IRAS16293-2422), supporting the idea that a relatively efficient formation mechanism for the detected COMs must exist in the cold gas phase;3) The discovery of a tight correlation between the dimethyl ether (DME) and methyl format (MF), suggesting a mother-daughter relationship;4) The detection of formamide, a species with a very high pre-biotic value, in several protostars, included IRAS16293-2422 and OMC2-FIR4;5) The full census of the cyanopolyynes in IRAS16293-2422 and OMC2-FIR4, with the detection of HC3N and HC5N, DC3N and, for OMC2-FIR4, the 13C isotopologue of HC3N cyanopolyynes.These results are the focus of two published articles (Jaber et al. 2014, ApJ; Lopez-Sepulcre, Jaber et al. 2015, MNRAS), one accepted article (Jaber et al., A&amp;A) and a final article to be submitted (Jaber et al., A&amp;A)
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Mengel, Matthew Wayne. "The active young solar-type star HR 1817 (=HD 35850)." University of Southern Queensland, Faculty of Sciences, 2005. http://eprints.usq.edu.au/archive/00001474/.

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The active F dwarf HR 1817 represents the upper temperature extreme of what are broadly termed solar-type stars - stars which have the same internal structure as the Sun, albeit in this case with a much smaller convective zone. To date, studies of the active surface features and magnetic fields of solar-type stars have been restricted to G and K dwarfs. This thesis investigates the surface and magnetic features of HR 1817 using the techniques of Doppler and Zeeman Doppler Imaging, resulting in tomographic maps of the stellar surface and magnetic field. Cooler stars than HR 1817 exhibit large polar spots, and while HR 1817 also exhibits a polar spot, it is not nearly as large as those usually seen. The lower-latitude surface features of HR 1817 are weak but well defined and cover a relatively small area of the stellar surface. Total spot coverage is relatively small (~ 1.7 - 2 per cent). Zeeman Doppler Imaging reveals that HR 1817 exhibits a richly-detailed, though weak magnetic topography. A ring of azimuthal field appears around the pole, while the radial field exhibits many well-defined and distinct bipolar mid-latitude magnetic features, perhaps indicating a more dominant interface dynamo as opposed to the posited distributed dynamo of cooler active dwarfs. Finally, a differential rotation measurement of the star indicates an extremely large rotational shear. Values for the equatorial rotation and rotational shear of 6.494 +/- 0.010 rad/d and 0.256 +/- 0.017 rad/d respectively are found. This equatorial rotation is equivalent to a rotational period for HR 1817 of ~ 0.98 days. The very high rotational shear of 0.256 rad/d is fast enough for the equator to lap the pole in approximately 23 days.
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Namekata, Kousuke. "Observational Studies of Extreme Stellar Magnetic Activities: Spots, Flares, and Mass Ejections." Doctoral thesis, Kyoto University, 2021. http://hdl.handle.net/2433/263473.

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Fuentes, Pineda Rosinda. "Triphenylamine-based hole transport materials for perovskite solar cells." Thesis, University of Edinburgh, 2018. http://hdl.handle.net/1842/31410.

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The rapid development in perovskite solar cells (PSC) has generated a tremendous interest in the photovoltaic community. The power conversion efficiency (PCE) of these devices has increased from 3.8% in 2009 to a recent certified efficiency of over 20% which is mainly the product of the remarkable properties of the perovskite absorber material. One of the most important advances occurred with the replacement of the liquid electrolyte with a solid state hole conductor which enhanced PCE values and improved the device stability. Spiro-OMeTAD (2,2',7,7'-tetrakis(N,N'-di-p-methoxyphenylamine)- 9,9'-spirobifluorene) is the most common hole transport material in perovskite solar cells. Nevertheless, the poor conductivity, low charge transport and expensive synthetic procedure and purification have limited its commercialisation. Triphenylamines (TPA) like Spiro-OMeTAD are commonly employed due to the easy oxidation of the nitrogen centre and good charge transport. Other triarylamines have similar properties to Spiro-OMeTAD but are easier to synthesise. The aim of this doctoral thesis is to investigate different types of hole transport materials in perovskite solar cells. Three different series of triphenylamine-based HTM were designed, synthesised, characterised and studied their function in perovskite solar cells. A series of five diacetylide-triphenylamine (DATPA) derivatives (Chapter 3) with different alkyl chain length in the para position was successfully synthesised through a five step synthesis procedure. A range of characterisation techniques was carried out on the molecules including; optical, electrochemical, thermal and computational methods. The results show that the new HTMs have desirable optical and electrochemical properties, with absorption in the UV, a reversible redox property and a suitable highest occupied molecular orbital (HOMO) energy level for hole transport. Perovskite solar cell device performances were studied and discussed in detail. This project studied the effect of varying the alkyl chain length on structurally similar triarylamine-based hole transport materials on their thermal, optical, electrochemical and charge transport properties as well as their molecular packing and solar cell parameters, thus providing insightful information on the design of hole transport materials in the future. The methoxy derivative showed the best semiconductive properties with the highest charge mobility, better interfacial charge transfer properties and highest PCE value (5.63%). The use of p-type semiconducting polymers are advantageous over small molecules because of their simple deposition, low cost and reproducibility. Styrenic triarylamines (Chapter 4) were prepared by the Hartwig-Buchwald coupling followed by their radical polymerization. All monomers and polymers were fully characterised through electrochemical, spectroscopic and computational techniques showing suitable HOMO energy levels and desirable optoelectrochemical properties. The properties and performance of these monomers and polymers as HTMs in perovskite solar cells were compared in terms of their structure. Despite the lower efficiencies, the polymers showed superior reproducibility on each of the device parameters in comparison with the monomers and spiro-OMeTAD. Finally, star-shaped structures combine the advantages of both small molecules, like well-defined structures and physical properties, and polymers such as good thermal stability. Two star-shaped triarylamine-based molecules (Chapter 5) were synthesised, fully characterised and their function as hole-transport materials in perovskite solar cells studied. These materials afford a PCE of 13.63% and high reproducibility and device stability. In total this work provided three series of triarylamine-based hole transport materials for perovskite solar cells application and enabled a comparison of the pros and cons of different design structures: small-molecule, polymeric and star-shaped.
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Benbakoura, Mansour. "Evolution des étoiles de faible masse en interaction : observations multi-techniques et modélisation des systèmes multiples." Thesis, Université de Paris (2019-....), 2019. http://www.theses.fr/2019UNIP7027.

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Cette thèse est consacrée à l'étude des étoiles de faible masse ayant dans leur environnement proche d'autres étoiles ou des planètes. Nous nous sommes concentrés sur l'influence des interactions avec ces compagnons sur l'évolution stellaire ainsi que leurs conséquences observables.Dans la première partie, nous présentons le modèle d'évolution des systèmes étoile–planète que nous avons développé au cours de cette thèse, nommé ESPEM (Évolution des Systèmes Planétaires Et Magnétisme). Ce modèle prend en compte de façon ab-initio des effets du vent stellaire magnétisé et de la dissipation de marée sur la rotation stellaire et l'orbite planétaire, simultanément avec l'évolution structurelle de l'étoile. Premièrement, nous l'utilisons pour étudier l'évolution séculaire de la rotation des étoiles hôtes de systèmes planétaires et montrons notamment que cette évolution peut être significativement différente de celle des étoiles isolées. Ensuite, nous examinons les prédictions de ce modèle concernant l'architecture orbitale des systèmes étoile–planète. Nos résultats suggèrent une interprétation aux distributions de périodes orbitales et de de rotation stellaire observées.Dans la deuxième partie, nous montrons en quoi l'observation d'étoiles binaires évoluées permet de tester les théories astrophysiques, notamment l'astérosismologie et l'interaction de marée. Dans un premier temps, nous présentons les résultats d'un programme d'observations que nous avons mené pendant plus de deux ans et qui nous a permis de caractériser 16 systèmes binaires à éclipses. Ensuite, nous comparons ces résultats avec ceux que nous avons obtenus en analysant cet échantillon à l'aide d'outils astérosismiques dans le but de vérifier l'exactitude de ces derniers. Enfin, en élargissant l'échantillon étudié à 30 autres étoiles binaires évoluées, nous testons la théorie de l'évolution de marée. Ceci nous permet à la fois de valider la théorie et de comprendre l'évolution des systèmes observés dans ce travail.Ce travail met en avant deux aspects de la spécificité des systèmes multiples. Premièrement, il montre en quoi l'évolution des étoiles est impactée par la présence d'un compagnon stellaire ou planétaire. Deuxièmement, il met en avant l'intérêt des étoiles binaires pour tester les théories astrophysiques et renforce la compréhension actuelle de l'évolution stellaire<br>This thesis is devoted to the study of low-mass stars having other stars or planets in their immediate environment. We focused on the influence of interactions with these companions on stellar evolution and their observable consequences.In the first part, we present the model of evolution of star–planet systems that we developed during this thesis, called ESPEM (French acronym for Evolution of Planetary Systems and Magnetism). This model incorporates ab-initio prescriptions to quantify the effects of magnetized stellar wind and tidal dissipation on stellar rotation and planetary orbit, simultaneously with the star's structural evolution. First, we use it to study the secular evolution of the rotation of planet-host stars and show that this evolution can be significantly different from that of isolated stars. Next, we examine the predictions of this model regarding the orbital architecture of star–planet systems. Our results suggest an interpretation to the observed distributions of orbital and stellar rotation periods.In the second part of the manuscript, we show how the observation of advanced binary stars allows us to test astrophysical theories, in particular asteroseismology and tidal interaction. First, we present the results of an observation program that we conducted for more than two years and that allowed us to characterize 16 eclipsing binary systems. Then, we compare these results with those obtained by analyzing this sample using asteroseismic tools to verify the accuracy of the latter. Finally, by extending the studied sample to 30 other advanced binary stars including an evolved primary, we test the theory of tidal evolution. This allows us both to validate the theory and to understand the evolution of the systems observed in this work.This work highlights two aspects of the specificity of multiple systems. First, it shows how the evolution of stars is affected by the presence of a stellar or planetary companion. Second, it emphasizes the interest of binary stars in testing astrophysical theories and reinforces the current understanding of stellar evolution
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Hawkins, Keith A. "Searching for Solar-Type Hypervelocity Stars." Ohio University Honors Tutorial College / OhioLINK, 2013. http://rave.ohiolink.edu/etdc/view?acc_num=ouhonors1367583430.

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Notsu, Yuta. "Observational studies on solar-type superflare stars." Kyoto University, 2019. http://hdl.handle.net/2433/242613.

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Corporon, Patrice. "La binarité des étoiles Ae/Be de Herbig vue par l'optique adaptative et la spectroscopie : une étude du système triple TY CrA." Phd thesis, Université Joseph Fourier (Grenoble), 1998. http://tel.archives-ouvertes.fr/tel-00724469.

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Les étoiles multiples sont nombreuses, tant parmi les objets jeunes de faible masse, les étoiles T Tauri, que parmi les astres de la Séquence Principale (SP). En ce qui concerne les étoiles jeunes de masse intermédiaire, les étoiles Ae/Be de Herbig (HAeBe), le statut de la binarité est peu connu. Nous avons réalisé une recherche systématique de binaires HAeBe en utilisant deux techniques: l'imagerie à haute résolution angulaire avec la méthode de l'Optique Adaptative d'une part, et la spectroscopie visible à haute résolution d'autre part. Ces techniques complémentaires nous ont permis d'identifier plus d'une vingtaine de nouvelles étoiles binaires; la fréquence de binarité déduite est d'au moins 50 %, voir supérieure à cause des biais observationnels discutés dans la thèse. Pour la première fois, les types spectraux des compagnons ont pu être déterminés dans une vingtaine de systèmes visuels. Les implications de nos observations pour la présence de disques de poussières et la détection d'émission X dans les étoiles HAeBe sont présentées. Les contraintes apportées pour les théories de formation des binaires sont discutées. Une partie importante de la thèse est consacrée à une étude approfondie de l'étoile triple TY CrA, l'unique système spectroscopique hiérarchisé parmi les étoiles Ae/Be de Herbig. Après une description complète des paramètres orbitaux et stellaires, la modélisation de la dynamique de cet objet particulier a été réalisée. Nos calculs théoriques montrent que la cohésion du système est assurée par effet de marée à l'oeuvre dans la binaire à éclipse centrale. L'environnement circumstellaire de TY CrA a également été étudié à partir d'observations spectroscopiques infrarouges avec le télescope spatial ISO et à partir d'images en Optique Adaptative dans le proche infrarouge.
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Hamilton, Devon. "Observational signatures of convection in solar type stars." Thesis, National Library of Canada = Bibliothèque nationale du Canada, 2001. http://www.collectionscanada.ca/obj/s4/f2/dsk3/ftp04/NQ58914.pdf.

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Mamajek, Eric E. "Identification and characterization of young, nearby, solar-type stars." Diss., The University of Arizona, 2004. http://hdl.handle.net/10150/280625.

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Post-T Tauri stars (PTTSs) are low-mass, pre-MS stars which have ceased accreting, and are not necessarily near star-forming molecular clouds. Historically, they have been difficult to identify due to their benign spectroscopic signatures. With recent all-sky X-ray surveys and proper motion catalogs, it is now possible to find PTTSs in large numbers. The nearest PTTSs will be important targets for future imaging surveys characterizing dust disks and planetary systems around young solar analogs. The goal of this work is to systematically identify samples of PTTSs, investigate the evolution of circumstellar disks, to infer the fossil star-formation history of molecular clouds, and to estimate kinematic distances to young stars lacking trigonometric parallaxes. We present the results of a spectroscopic survey which identified 110 PTTS members of the nearest OB association (Sco-Cen). We find that 2/3rds of the low-mass star-formation in each OB subgroup occurred in <5 Myr, and that only ∼1% of solar-type stars with mean age ∼13 Myr shows signs of accretion from a circumstellar disk. In order to assess how long circumstellar material is detectable around PTTSs, we conducted a 10 μm imaging survey of post-T Tauri members of the ∼30-Myr-old Tuc-Hor association. The goal was to find evidence of either remnant accretion disks or dusty debris disks with orbital radii of ≲10 AU. Combined with data from other surveys, we conclude that mid-IR emission from warm dust grains in the terrestrial planet zones around young stars become undetectable compared to the stellar photosphere for nearly all stars by age ∼20 Myr. Lastly, we present a technique for calculating distances isolated young field stars that currently lack trigonometric parallax measurements. The technique is a generalization of the classical cluster parallax method, but can handle anisotropic velocity dispersions and non-zero Oort parameters. Distances and isochronal ages are estimated for a subsample of PTTSs included in the Formation and Evolution of Planetary Systems (FEPS) Spitzer Space Telescope (SST) Legacy Science program. The techniques developed in this thesis will allow one to efficiently conduct a systematic survey to identify the nearest, youngest stars to the Sun using existing databases.
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Books on the topic "Solar-type star"

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Hamilton, Devon. Observational signatures of convection in solar type stars. Graduate Department of Astronomy and Astrophysics, University of Toronto, 2001.

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Rüdiger, G. Differential rotation and stellar convection: Sun and solar-type stars. Gordon and Breach Science Publishers, 1989.

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Rüdiger, Günther. Differential rotation and stellar convection: Sun and solar-type stars. Gordon and Breach Science Publishers, 1989.

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Space Telescope Science Institute (U. Survey of Chromospheric Emission and Rotation Among Solar-Type Stars in the Solar Neighborhood. s.n, 1985.

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Hotta, Hideyuki. Thermal Convection, Magnetic Field, and Differential Rotation in Solar-type Stars. Springer Japan, 2015. http://dx.doi.org/10.1007/978-4-431-55399-1.

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(Translator), Svetlana Knyazeva, ed. Solar-Type Activity in Main-Sequence Stars. Springer, 2005.

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Gershberg, Roald E. Solar-Type Activity in Main-Sequence Stars. Springer, 2008.

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Gershberg, Roald E. E., and Svetlana Knyazeva. Solar-Type Activity in Main-Sequence Stars. Springer, 2010.

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Solar-Type Activity in Main-Sequence Stars. Springer-Verlag, 2005. http://dx.doi.org/10.1007/3-540-28243-2.

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Hotta, Hideyuki. Thermal Convection, Magnetic Field, and Differential Rotation in Solar-type Stars. Springer, 2015.

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Book chapters on the topic "Solar-type star"

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Hartquist, T. W., and R. Rosner. "Models of Solar-type Coronae." In Activity in Cool Star Envelopes. Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2951-7_31.

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Tuominen, I., G. Rüdiger, and A. Brandenburg. "Observational Constraints for Solar-Type Dynamos." In Activity in Cool Star Envelopes. Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2951-7_2.

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Mamajek, Eric E. "Solar-Type Post-T Tauri Stars in the Nearest OB Subgroups." In Open Issues in Local Star Formation. Springer Netherlands, 2003. http://dx.doi.org/10.1007/1-4020-2600-5_4.

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Shakhovskaya, N. I. "Some Physical Consequences from the Flare Statistics of the UV Cet Type Stars in the Solar Neighbourhood." In Flare Stars in Star Clusters, Associations and the Solar Vicinity. Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-0607-5_13.

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Altrock, Richard C. "Coronal-Hole Detectability on Solar-Type Stars." In Radio Stars. Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5420-5_34.

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Reetz, Johannes. "Oxygen Abundances in Solar-Type Stars." In Galaxy Evolution: Connecting the Distant Universe with the Local Fossil Record. Springer Netherlands, 1999. http://dx.doi.org/10.1007/978-94-011-4213-7_27.

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Hartmann, L. "Mass Loss From Solar-Type Stars." In Progress in Solar Physics. Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-4588-3_29.

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Reetz, Johannes. "Oxygen Abundance in Solar-Type Stars." In Chemical Evolution from Zero to High Redshift. Springer Berlin Heidelberg, 1999. http://dx.doi.org/10.1007/978-3-540-48360-1_14.

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Bertout, Claude, and Francois Ménard. "The Nature of Young Solar-Type Stars." In The Origin of Stars and Planetary Systems. Springer Netherlands, 1999. http://dx.doi.org/10.1007/978-94-011-4509-1_10.

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Bouchy, François, and Fabien Carrier. "Present Observational Status of Solar-Type Stars." In Asteroseismology Across the HR Diagram. Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0799-2_4.

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Conference papers on the topic "Solar-type star"

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Dimitrijević, Milan S., Cristiana Dumitrache, Vasile Mioc, and Nedelia A. Popescu. "Influence of Collisions with Charged Particles on Solar Type Star Spectra; Investigations on Belgrade Astronomical Observatory." In Flows, Boundaries, Interactions. AIP, 2007. http://dx.doi.org/10.1063/1.2790350.

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Farkas, Ladislau, Vasile Mioc, Cristiana Dumitrache, and Nedelia A. Popescu. "The Beta Cephei Type Variable Star BW Vulpeculae." In EXPLORING THE SOLAR SYSTEM AND THE UNIVERSE. AIP, 2008. http://dx.doi.org/10.1063/1.2993689.

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Michaud, George. "Particle transport in solar type stars." In AIP Conference Proceedings Vol.126. AIP, 1985. http://dx.doi.org/10.1063/1.35165.

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Honda, Satoshi, Yuta Notsu, Hiroyuki Maehara, et al. "Lithium Abundance of the Solar-Type Superflare Stars." In Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016). Journal of the Physical Society of Japan, 2017. http://dx.doi.org/10.7566/jpscp.14.020303.

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Fekel, Francis C., B. Zuckerman, Michael H. Williamson, Gregory W. Henry, M. P. Muno, and Eric Stempels. "The Dusty, Solar Type Spectroscopic Binary BD +20 307." 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/10.1063/1.3099246.

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Bondar’, N. I., M. M. Katsova, and M. A. Livshits. "CYCLES ON SOLAR-TYPE STARS AND MORE COOL DWARFS." In All-Russia Conference on Solar and Solar-Terrestrial Physics. The Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo, 2018. http://dx.doi.org/10.31725/0552-5829-2018-67-70.

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Giampapa, Mark, William Sherry, Eric Craine, Roy Tucker, and Eric Stempels. "Photometric variability of solar-type members of the Pleiades open cluster." 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/10.1063/1.3099197.

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Claudi, R. U., S. Benatti, E. Carolo, A. Bonanno, and Eric Stempels. "Detection of p-modes in solar type stars with SARG@TNG." 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/10.1063/1.3099214.

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Chabrier, G., I. Baraffe, J. Leconte, J. Gallardo, T. Barman, and Eric Stempels. "The mass-radius relationship from solar-type stars to terrestrial planets: a review." 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/10.1063/1.3099078.

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Strom, Stephen E., Suzan Edwards, and Michael F. Skrutskie. "Evolutionary timescales for circumstellar disks associated with solar-type pre-main sequence stars." In Astrophysics from the Moon. AIP, 1990. http://dx.doi.org/10.1063/1.39359.

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