Dissertations / Theses on the topic 'Stellar associations'
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An, Deokkeun. "Improving the Local Distance Scale from Empirically Calibrated Stellar Isochrones." The Ohio State University, 2008. http://rave.ohiolink.edu/etdc/view?acc_num=osu1218593380.
Full textBalog, Zoltan, Nick Siegler, G. H. Rieke, L. L. Kiss, James Muzerolle, R. A. Gutermuth, Cameron P. M. Bell, et al. "PROTOPLANETARY AND TRANSITIONAL DISKS IN THE OPEN STELLAR CLUSTER IC 2395." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622451.
Full textGrether, Daniel Andrew Physics Faculty of Science UNSW. "Statistical analyses of extrasolar planets and other close companions to nearby stars." Awarded by:University of New South Wales. School of Physics, 2006. http://handle.unsw.edu.au/1959.4/29182.
Full textSmilgys, Romas. "Formation of stars and stellar clusters in galactic environment." Thesis, University of St Andrews, 2018. http://hdl.handle.net/10023/13229.
Full textMcCarthy, Kyle. "Characterizing the Nearest Young Moving Groups." UKnowledge, 2015. http://uknowledge.uky.edu/physastron_etds/30.
Full textMiret, Roig Núria. "COSMIC-DANCE : A comprehensive census of nearby star forming regions." Thesis, Bordeaux, 2020. http://www.theses.fr/2020BORD0327.
Full textUnderstanding how stars form is one of the fundamental questions which astronomy aims to answer. Currently, it is well accepted that the majority of stars form in groups and that their predominant mechanism of formation is the core-collapse. However, several mechanisms have been suggested to explain the formation of substellar objects, and their contribution is still under debate. The main goal of this thesis is to determine the initial mass function, the mass distribution of stars at birth time, in different associations and star-forming regions. The mass function constitutes a fundamental observational parameter to constrain stellar and substellar formation theories since different formation mechanisms predict different fraction of stellar and substellar objects. We used the Gaia Data Release 2 catalogue together with ground-based observations from the COSMIC-DANCe project to look for high probability members via a probabilistic model of the distribution of the observable quantities in both the cluster and background populations. We applied this method to the 30 Myr open cluster IC 4665 and the 1 - 10 Myr star-forming region Upper Scorpius (USC) and r Ophiuchi (r Oph). We found very rich populations of substellar objects which largely exceed the numbers predicted by core-collapse models. In USC, where our sensitivity is best, we found a large number of free-floating planets and we suggest that ejection from planetary systems must have a similar contribution than core-collapse in their formation. The age is a fundamental parameter to study the formation and evolution of stars and is essential to accurately convert luminosities to masses. For that, we also presented a strategy to study the dynamical traceback age of young local associations through an orbital traceback analysis. We applied this method to determine the age of the b Pictoris moving group and in the future, we plan to apply it to other regions such as USC. The members we identified with the membership analysis are excellent targets for follow-up studies such as a search for discs, exoplanets, characterisation of brown dwarfs and free-floating planets. I this thesis, we presented a search for discs hosted by members of IC 4665 and we found six excellent candidates to be imaged with ALMA or the JWST. The tools we developed, are ready to be used in other regions such as USC and r Oph, where we expect to find a larger number of disc-host stars
Da, Rio Nicola, Jonathan C. Tan, Kevin R. Covey, Michiel Cottaar, Jonathan B. Foster, Nicholas C. Cullen, John Tobin, et al. "IN-SYNC. V. Stellar Kinematics and Dynamics in the Orion A Molecular Cloud." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/625776.
Full textZOCCHI, ALICE. "OBSERVATIONAL TESTS ON THE DYNAMICS OF GLOBULAR CLUSTERS." Doctoral thesis, Università degli Studi di Milano, 2014. http://hdl.handle.net/2434/235122.
Full textKastner, Joel H., David A. Principe, Kristina Punzi, Beate Stelzer, Uma Gorti, Ilaria Pascucci, and Costanza Argiroffi. "M STARS IN THE TW HYA ASSOCIATION: STELLAR X-RAYS AND DISK DISSIPATION." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621232.
Full textNakamura, Toshio. "Expression of the Na+/Ca2+ exchanger emerges in hepatic stellate cells after activation in association with liver fibrosis." Kyoto University, 1998. http://hdl.handle.net/2433/182267.
Full textMurata, Toru. "Inhibitory effect of Y-27632,a ROCK inhibitor,on progression of rat liver fibrosis in association with inactivation of hepatic stellate cells." Kyoto University, 2002. http://hdl.handle.net/2433/149343.
Full textBurgess, Andrew. "Exploration de la fonction de faible masse initiale dans les amas jeunes et les r ´egions de formation stellaire." Phd thesis, Université de Grenoble, 2010. http://tel.archives-ouvertes.fr/tel-00576460.
Full textDe, Gennaro Steven Andrew. "White dwarfs and the ages of stellar populations." Thesis, 2009. http://hdl.handle.net/2152/ETD-UT-2009-12-441.
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Couture, Dominic. "Recherche d'un âge cinématique de l'association β Pictoris." Thesis, 2019. http://hdl.handle.net/1866/24368.
Full textYoung moving groups (YMGs) are associations of young stars, mainly M dwarfs, that share a common kinematics, located in the solar neighbourhood and formed at the same epoch by the collapse of a molecular cloud that is unique to every association. They are ideal laboratories for the study of the last steps of stellar formation and the direct imaging of exoplanets. The β Pictoris moving group (βPMG) is one of the youngest and closest YMGs, although its age remains uncertain: ages found using isochrones or the lithium depletion boundary (LDB; 21 − 24 Myr) are inconsistent with traceback ages (11 − 13 Myr), found by tracing back the trajectories of member stars up to the epoch when the size of the YMG was minimal, which coincides with the epoch of stellar formation. This study presents a new numerical method, called Traceback, capable of finding a kinematic age for a YMG by traceback with data from the Gaia Data Release 2 (DR2) catalog. Its maximal theoretical precision is calculated and two important biases are characterized: a bias due to measurement errors (∼ −4.5 Myr) and a ∆v_r, grav = 0.5 km/s bias on radial velocity (v_r ; vitesse radiale) measurements due to gravitational redshift (∼ −1.8 Myr). When this method is applied to a sample of 46 validated members of βPMG, a corrected kinematic age of 17 − 19 Myr, in agreement with isochrones and LDB ages, is found by minimizing the median absolute deviation (MAD), a measure of the size of the association that is robust against outliers in the data, and the X-U covariance between the X positions and the U velocities of member stars. Furthermore, the use of a minimum spanning tree (MST) is shown not to be advantageous.
"Clustering of Stars in Nearby Galaxies: Probing the Range of Stellar Structures." Doctoral diss., 2011. http://hdl.handle.net/2286/R.I.14465.
Full textDissertation/Thesis
Ph.D. Astrophysics 2011