Gotowe bibliografie tematyczne / Stars of low metallicity

Spis treści

  1. Artykuły w czasopismach
  2. Rozprawy doktorskie
  3. Książki
  4. Części książek
  5. Streszczenia konferencji
  6. Raporty organizacyjne

Gotowa bibliografia na temat „Stars of low metallicity”

Autor: Grafiati
Data publikacji: 8 czerwca 2024
Data aktualizacji: 31 lipca 2025

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Artykuły w czasopismach na temat "Stars of low metallicity"

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Pakmor, Rüdiger, Christine M. Simpson, Freeke van de Voort, et al. "Formation and fate of low-metallicity stars in TNG50." Monthly Notices of the Royal Astronomical Society 512, no. 3 (2022): 3602–15. http://dx.doi.org/10.1093/mnras/stac717.

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ABSTRACT Low-metallicity stars give rise to unique spectacular transients and are of immense interest for understanding stellar evolution. Their importance has only grown further with the recent detections of mergers of stellar mass black holes that likely originate mainly from low-metallicity progenitor systems. Moreover, the formation of low-metallicity stars is intricately linked to galaxy evolution, in particular to early enrichment and to later accretion and mixing of lower metallicity gas. Because low-metallicity stars are difficult to observe directly, cosmological simulations are cruci
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Hirschi, Raphael, Cristina Chiappini, Georges Meynet, André Maeder, and Sylvia Ekström. "Stellar Evolution at Low Metallicity." Proceedings of the International Astronomical Union 3, S250 (2007): 217–30. http://dx.doi.org/10.1017/s1743921308020528.

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AbstractMassive stars played a key role in the early evolution of the Universe. They formed with the first halos and started the re-ionisation. It is therefore very important to understand their evolution. In this review, we first recall the effect of metallicity (Z) on the evolution of massive stars. We then describe the strong impact of rotation induced mixing and mass loss at very low Z. The strong mixing leads to a significant production of primary 14N, 13C and 22Ne. Mass loss during the red supergiant stage allows the production of Wolf-Rayet stars, type Ib,c supernovae and possibly gamma
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Sabach, Efrat. "Jsolated Stars of Low Metallicity." Galaxies 6, no. 3 (2018): 89. http://dx.doi.org/10.3390/galaxies6030089.

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We study the effects of a reduced mass-loss rate on the evolution of low metallicity Jsolated stars, following our earlier classification for angular momentum (J) isolated stars. By using the stellar evolution code MESA we study the evolution with different mass-loss rate efficiencies for stars with low metallicities of Z = 0 . 001 and Z = 0 . 004 , and compare with the evolution with solar metallicity, Z = 0 . 02 . We further study the possibility for late asymptomatic giant branch (AGB)—planet interaction and its possible effects on the properties of the planetary nebula (PN). We find for al
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Bouret, J. C., T. Lanz, F. Martins, et al. "Massive stars at low metallicity." Astronomy & Astrophysics 555 (June 18, 2013): A1. http://dx.doi.org/10.1051/0004-6361/201220798.

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Hirschi, R. "Very low-metallicity massive stars:." Astronomy & Astrophysics 461, no. 2 (2006): 571–83. http://dx.doi.org/10.1051/0004-6361:20065356.

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Karakas, Amanda I., Maria Lugaro, and Simon W. Campbell. "The slow-neutron capture process in low-metallicity asymptotic giant branch stars." Proceedings of the International Astronomical Union 5, S265 (2009): 57–60. http://dx.doi.org/10.1017/s1743921310000165.

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AbstractElements heavier than iron are produced in asymptotic giant branch (AGB) stars via the slow neutron capture process (s process). Recent observations of s-process-enriched Carbon Enhanced Metal-Poor (CEMP) stars have provided an unprecedented wealth of observational constraints on the operation of the s-process in low-metallicity AGB stars. We present new preliminary full network calculations of low-metallicity AGB stars, including a comparison to the composition of a few s-process rich CEMP stars. We also discuss the possibility of using halo planetary nebulae as further probes of low-
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Garcia, Miriam, Artemio Herrero, Francisco Najarro, et al. "Low-metallicity (sub-SMC) massive stars." Proceedings of the International Astronomical Union 12, S329 (2016): 313–21. http://dx.doi.org/10.1017/s1743921317003088.

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AbstractThe double distance and metallicity frontier marked by the SMC has been finally broken with the aid of powerful multi-object spectrographs installed at 8-10m class telescopes. VLT, GTC and Keck have enabled studies of massive stars in dwarf irregular galaxies of the Local Group with poorer metal-content than the SMC. The community is working to test the predictions of evolutionary models in the low-metallicity regime, set the new standard for the metal-poor high-redshift Universe, and test the extrapolation of the physics of massive stars to environments of decreasing metallicity. In t
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Martayan, Christophe, Dietrich Baade, Juan Zorec, Yves Frémat, Juan Fabregat, and Sylvia Ekström. "Massive Oe/Be stars at low metallicity: candidate progenitors of long GRBs?" Proceedings of the International Astronomical Union 6, S272 (2010): 300–301. http://dx.doi.org/10.1017/s1743921311010660.

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AbstractAt low metallicity B-type stars rotate faster than at higher metallicity, typically in the SMC. As a consequence, a larger number of fast rotators is expected in the SMC than in the Galaxy, in particular more Be/Oe stars. With the ESO-WFI in its slitless mode, we examined the SMC open clusters and found an occurence of Be stars 3 to 5 times larger than in the Galaxy. The evolution of the angular rotational velocity seems to be the main key on the understanding of the specific behaviour and stellar evolution of such stars at different metallicities. With the results of this WFI study an
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Bomans, Dominik J., and Kerstin Weis. "Massive variable stars at very low metallicity?" Proceedings of the International Astronomical Union 6, S272 (2010): 265–70. http://dx.doi.org/10.1017/s1743921311010519.

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AbstractObservational contraints on the evolution and instabilities of massive stars at very low metallicities are limited. Most of the information come from HST observations of one target, I Zw 18. Recent distance estimates of I Zw 18 put it at 17 Mpc, moving detailed studies of single stars clearly beyond the range of current ground based telescopes. Since massive stars with metallcities of 1/10 of solar and below are our best proxies for massive stars in (proto-) galaxies around the time of reionization, finding them and studying their evolution and instabilities is of premium importance fo
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Omukai, Kazuyuki. "Formation of Very Low-metallicity Stars." Proceedings of the International Astronomical Union 18, S361 (2022): 521–27. http://dx.doi.org/10.1017/s1743921322002988.

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AbstractI describe (i) our recent updates on first star formation, with particular emphasis on their binaries, (ii) formation of low-metallicity stars and the transition of their initial mass functions with metal enrichment, and finally (iii) formation of supermassive stars from slightly metal-enriched gas by the newly found super-competitive accretion channel.
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Rozprawy doktorskie na temat "Stars of low metallicity"

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Masters, Craig Eugene Ashman Keith M. "The formation of low metallicity globular clusters." Diss., UMK access, 2007.

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Thesis (Ph. D.)--Dept. of Physics and Dept. of Mathematics. University of Missouri--Kansas City, 2007.<br>"A dissertation in physics and mathematics." Advisor: Keith M. Ashman. Typescript. Vita. Title from "catalog record" of the print edition Description based on contents viewed Nov. 13, 2007. Includes bibliographical references (leaves 67-70). Online version of the print edition.
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Szécsi, Dorottya [Verfasser]. "The evolution of low-metallicity massive stars / Dorottya Szécsi." Bonn : Universitäts- und Landesbibliothek Bonn, 2016. http://d-nb.info/1113688262/34.

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Fukushima, Hajime. "Radiative feedback from massive stars in low-metallicity environments." Kyoto University, 2019. http://hdl.handle.net/2433/242603.

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Krawchuk, Curtis A. P. "The determination of metallicity and temperature of low-mass stars using broad-band photometry." Thesis, National Library of Canada = Bibliothèque nationale du Canada, 1997. http://www.collectionscanada.ca/obj/s4/f2/dsk2/tape15/PQDD_0035/MQ27361.pdf.

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Lindgren, Sara. "Metallicity determination of M dwarfs." Doctoral thesis, Uppsala universitet, Observationell astrofysik, 2017. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-332102.

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M dwarfs constitute around 70% of all stars in the local Galaxy. Their multitude together with their long main-sequence lifetimes make them important for studies of global properties of the Galaxy such as the initial mass function or the structure and kinematics of stellar populations. In addition, the exoplanet community is showing an increasing interest for those small, cold stars. However, very few M dwarfs are well characterized, and in the case of exoplanetary systems the stellar parameters have a direct influence on the derived planet properties. Stellar parameters of M dwarfs are diffic
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Verdugo, Salgado Celia Anahi. "Star formation in low gas density and low metallicity environments." Observatoire de Paris, 2015. https://hal.science/tel-02095302.

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Dans les galaxies proches, la relation empirique de Kennicutt-Schmidt (KS) a été établie entre la densité surfacique de formation d’étoiles et la densité surfacique de gaz. Elle est forte et presque linéaire quand on considère le gaz moléculaire (H2) mais devient moins valable lorsque l’hydrogène n’est qu’atomique (HI). Ces régions de densité de gaz faible sont d’une importance cruciale dans le domaine de la formation d’étoiles, car elles possèdent les mêmes conditions que dans les galaxies de l’univers jeune, de faible métallicité. Cette thèse compile les données observationnelles obtenues au
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Rajpurohit, Arvind Singh. "Low-mass stars as tracers of the milky way populations : investigating the effects of metallicity in cool atmosphere." Thesis, Besançon, 2013. http://www.theses.fr/2013BESA2023/document.

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Les étoiles de petite masse (naines M) forment la composante stellaire dominante de notre galaxie et contribuent à la majeure partie de la matière baryonique dans la galaxie. Notre compréhension de la galaxie repose donc sur la connaissance de cette composante peu lumineuse. Par ailleurs, un nombre grandissant d’exoplanètes sont découverte autour de naines M, y compris des super-terres. L’étude des naines M a ainsi des implications importantes sur la physique stellaire, permettant de comprendre les processus en jeu dans ces atmosphères froides. Ces astres restent cependant peu connus du fait d
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Ramachandran, Varsha [Verfasser], and Wolf-Rainer [Akademischer Betreuer] Hamann. "Massive star evolution, star formation, and feedback at low metallicity : quantitative spectroscopy of OB stars in the Magellanic Clouds / Varsha Ramachandran ; Betreuer: Wolf-Rainer Hamann." Potsdam : Universität Potsdam, 2019. http://d-nb.info/1218405058/34.

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Kunawicz, Nadya. "Any old iron? : astrochemical modelling of star-forming regions at low metallicity." Thesis, University of Manchester, 2010. https://www.research.manchester.ac.uk/portal/en/theses/any-old-iron--astrochemical-modelling-of-starforming-regions-at-low-metallicity(2a356b1a-429c-40b5-b9c0-2b4cdab12ea8).html.

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Two pseudo-time-dependent chemical models have been utilised - one of a dark cloud,and one of a hot core - in order to model these clouds in low metallicity environments, such as other galaxies. The dark cloud model uses gas-phase chemistry, whereas the hot core model includes both gas-phase and surface chemistry. The simulations have been calculated with varying initial elemental abundances of C, O, N, S and the heavy metals Fe, Mg and Na (henceforth, M). These initial abundances are taken from observations of HII regions in the Galaxy, the Large Magellanic Cloud and the Small Magellanic Clou
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Lombardo, Linda. "Explorer l'histoire de la Galaxie grâce à la spectroscopie stellaire." Electronic Thesis or Diss., Université Paris sciences et lettres, 2022. http://www.theses.fr/2022UPSLO011.

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Ce travail de thèse présente plusieurs études qui utilisent la spectroscopie à haute résolution pour déterminer les propriétés chimiques des différentes populations stellaires de la Voie Lactée. Le document est structuré comme suit : Le premier chapitre de la thèse, divisée en 3 sections, est une introduction générale à la structure de la Voie lactée et à ses populations stellaires, suivie d'une partie décrivant les différentes méthodes utilisées pour mesurer les abondances chimiques des étoiles. La première section décrit les différents scénarios concernant la structure et la formation de la
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Książki na temat "Stars of low metallicity"

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United States. National Aeronautics and Space Administration., ed. Chromospherically active stars. National Aeronautics and Space Administration, 1993.

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United States. National Aeronautics and Space Administration., ed. Chromospherically active stars. National Aeronautics and Space Administration, 1993.

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R, Rebolo, Zapatero Osorio Maria Rosa, and "Three-Islands" Euroconference on "Stellar Clusters and Associations" (1st : 1998 : Palma, Canary Islands), eds. Very low-mass stars and brown dwarfs. Cambridge University Press, 2000.

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Dupree, A. K., and M. T. V. T. Lago, eds. Formation and Evolution of Low Mass Stars. Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-3037-7.

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K, Dupree Andrea, Lago, M. T. V. T., and North Atlantic Treaty Organization. Scientific Affairs Division., eds. Formation and evolution of low mass stars. Kluwer Academic Publishers, 1988.

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Reid, I. Neill. New light on dark stars: Red dwarfs, low-mass stars, brown dwarfs. Springer, 2000.

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Hill, Randal C. Spotlight on sports stars. Steck-Vaughn Co., 1989.

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Prusti, Timo Juhani. Infrared studies of low mass formation. Rijksuniversiteit Groningen, 1992.

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Reipurth, Bo, and Claude Bertout, eds. Herbig-Haro Flows and the Birth of Low Mass Stars. Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-011-5608-0.

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W, Romani Roger, and United States. National Aeronautics and Space Administration., eds. EUV/soft x-ray spectra for low B neutron stars. National Aeronautics and Space Administration, 1995.

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Części książek na temat "Stars of low metallicity"

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Beers, T. C. "The Metallicity Distribution Function of Extremely Low-Metallicity 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_18.

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Duncan, D. "Key Questions for Low Metallicity Stars." In Space Sciences Series of ISSI. Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-011-5116-0_17.

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Ann, Hong Bae, and Yong Hee Kang. "Age-Metallicity Relation for F-Stars." In Third Asian-Pacific Regional Meeting of the International Astronomical Union. Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4496-1_50.

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Beers, T. C., S. Rossi, J. E. Norris, S. G. Ryan, P. Molaro, and R. Rebolo. "The Low Metallicity Tail of the Halo Metallicity Distribution Function." In Space Sciences Series of ISSI. Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-011-5116-0_13.

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Castro, S., B. Barbuy, and T. Richtler. "Metallicity of Two Stars in Baade’s Window." In Galactic Bulges. Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_25.

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Peterson, R. C. "Disentangling Metallicity and Age for Turnoff 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_89.

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Prantzos, Nikos. "Stars (Low Mass)." In Encyclopedia of Astrobiology. Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-11274-4_1505.

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Jahreiss, Hartmut. "Low Mass Stars." In Science with Astronomical Near-Infrared Sky Surveys. Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0946-8_14.

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Nissen, P. E. "Age and Metallicity Distributions Among Galactic Disk Stars." In Stellar Populations. Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-011-0125-7_10.

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Hernández, X., and A. Ferrara. "Cosmological Origin of the Lowest Metallicity Halo Stars." In New Quests in Stellar Astrophysics: The Link Between Stars and Cosmology. Springer Netherlands, 2002. http://dx.doi.org/10.1007/978-94-010-0393-3_13.

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Streszczenia konferencji na temat "Stars of low metallicity"

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de Mink, S. E., M. Cottaar, and O. R. Pols. "Can Low—Metallicity Binaries Avoid Merging?" In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905545.

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Pignatari, M., and R. Gallino. "The Weak s‐Process at Low Metallicity." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905575.

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Lai, David K., Sara Lucatello, Michael Bolte, Debra A. Fischer, and Jennifer A. Johnson. "A Search for Binary Stars at Low Metallicity." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905523.

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Omukai, Kazu, Naoki Yoshida, Daniel J. Whalen, Volker Bromm, and Naoki Yoshida. "Low-Metallicity Star Formation." In THE FIRST STARS AND GALAXIES: CHALLENGES FOR THE NEXT DECADE. AIP, 2010. http://dx.doi.org/10.1063/1.3518838.

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Stancliffe, Richard J., Maria A. Lugaro, Amanda I. Karakas, and Carlos Rijs. "The s-process at low metallicity." In FIRST STARS IV – FROM HAYASHI TO THE FUTURE –. AIP, 2012. http://dx.doi.org/10.1063/1.4754347.

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Iwamoto, Nobuyuki, Takuma Suda, Takaya Nozawa, et al. "Lithium synthesis in low metallicity AGB stars." In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: The 10th International Symposium on Origin of Matter and Evolution of Galaxies: From the Dawn of Universe to the Formation of Solar System. AIP, 2008. http://dx.doi.org/10.1063/1.2943562.

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Hirschi, Raphael, Cristina Chiappini, Georges Meynet, et al. "Mass Loss and Very Low-metallicity Stars." In UNSOLVED PROBLEMS IN STELLAR PHYSICS: A Conference in Honor of Douglas Gough. AIP, 2007. http://dx.doi.org/10.1063/1.2818999.

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Yoon, S. ‐C, M. Cantiello, and N. Langer. "Evolution of Massive Stars at Very Low Metallicity, Including Rotation and Binary Interactions." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905548.

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de Mink, S. E., O. R. Pols, and S. ‐C Yoon. "Binaries at Low Metallicity: Ranges For Case A, B and C Mass Transfer." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905549.

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Doi, Kentaro, Hajime Susa, and Kazuyuki Omukai. "Dissipation of magnetic fields in low-metallicity clouds." In FIRST STARS IV – FROM HAYASHI TO THE FUTURE –. AIP, 2012. http://dx.doi.org/10.1063/1.4754383.

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Raporty organizacyjne na temat "Stars of low metallicity"

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Whitaker, Stephen. Rocky intertidal community monitoring at Channel Islands National Park: 2018–19 annual report. National Park Service, 2023. http://dx.doi.org/10.36967/2299674.

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Channel Islands National Park includes the five northern islands off the coast of southern California (San Miguel, Santa Rosa, Santa Cruz, Anacapa, and Santa Barbara Islands) and the surrounding waters out one nautical mile. There are approximately 176 miles of coastline around the islands, about 80% of which is composed of rock. The diversity and undisturbed nature of the tidepools of this rocky coastline were recognized as special features of the islands in the enabling legislation. To conserve these communities unimpaired for future generations, the National Park Service has been monitoring
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