Relevant bibliographies by topics / Star formation

Academic literature on the topic 'Star formation'

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Published: 4 June 2021
Last updated: 26 July 2024

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Journal articles on the topic "Star formation"

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Bromm, Volker, and Matthew R. Bate. "Star formation." Physics World 17, no. 10 (October 2004): 25–29. http://dx.doi.org/10.1088/2058-7058/17/10/29.

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Palla, Francesco. "Star Formation." International Astronomical Union Colloquium 120 (1989): 56–67. http://dx.doi.org/10.1017/s0252921100023484.

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Judging from the poster that the Organizing Committee has selected to announce the celebration of Guido Munch Jubilee, one can easily conclude that the main characteristics of the process of star formation as emerged in recent years through the combined efforts of multiwavelengths studies of molecular clouds, were already known, here in Granada, several centuries ago to the masters who built and enriched the enigmatic palace of the Alhambra. As we can appreciate from a quick inspection of the picture, it is rather obvious to infer that stars are the byproduct of a quite complex series of phenomena, each connected to, and somewhat dependent on, the others. Also, stars do not form in isolation, but rather in clusters or associations, with a strong tendency for the largest ones, also the most massive ones, to sit in the middle of the distribution. Moreover, smaller and less massive stars outnumber their massive counterparts, apparently obeying a power-law distribution. Finally, but with the benefit of doubt, it appears that the idea that the whole process reflects an intrinsic fractal nature was also put forward at the time. With this background in mind, let us now turn to the new emerging aspects of the study of star formation.
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Fritze, Uta. "Star cluster formation and star formation: the role of environment and star-formation efficiencies." Astrophysics and Space Science 324, no. 2-4 (November 4, 2009): 129–35. http://dx.doi.org/10.1007/s10509-009-0088-5.

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Hirai, Yutaka, Michiko S. Fujii, and Takayuki R. Saitoh. "SIRIUS project. I. Star formation models for star-by-star simulations of star clusters and galaxy formation." Publications of the Astronomical Society of Japan 73, no. 4 (May 20, 2021): 1036–56. http://dx.doi.org/10.1093/pasj/psab038.

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Abstract Most stars are formed as star clusters in galaxies, which then disperse into galactic disks. Upcoming exascale supercomputational facilities will enable simulations of galaxies and their formation by resolving individual stars (star-by-star simulations). This will substantially advance our understanding of star formation in galaxies, star cluster formation, and assembly histories of galaxies. In previous galaxy simulations, a simple stellar population approximation was used. It is, however, difficult to improve the mass resolution with this approximation. Therefore, a model for forming individual stars that can be used in simulations of galaxies must be established. In this first paper of a series from the SIRIUS (SImulations Resolving IndividUal Stars) project, we demonstrate a stochastic star formation model for star-by-star simulations. An assumed stellar initial mass function (IMF) is randomly assigned to newly formed stars in this model. We introduce a maximum search radius to assemble the mass from surrounding gas particles to form star particles. In this study, we perform a series of N-body/smoothed particle hydrodynamics simulations of star cluster formations from turbulent molecular clouds and ultra-faint dwarf galaxies as test cases. The IMF can be correctly sampled if a maximum search radius that is larger than the value estimated from the threshold density for star formation is adopted. In small clouds, the formation of massive stars is highly stochastic because of the small number of stars. We confirm that the star formation efficiency and threshold density do not strongly affect the results. We find that our model can naturally reproduce the relationship between the most massive stars and the total stellar mass of star clusters. Herein, we demonstrate that our models can be applied to simulations varying from star clusters to galaxies for a wide range of resolutions.
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Tan, Jonathan C. "Massive star and star cluster formation." Proceedings of the International Astronomical Union 2, S237 (August 2006): 258–64. http://dx.doi.org/10.1017/s1743921307001573.

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AbstractI review the status of massive star formation theories: accretion from collapsing, massive, turbulent cores; competitive accretion; and stellar collisions. I conclude the observational and theoretical evidence favors the first of these models. I then discuss: the initial conditions of star cluster formation as traced by infrared dark clouds; the cluster formation timescale; and comparison of the initial cluster mass function in different galactic environments.
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Elmegreen, B. G. "Star Formation During Galaxy Formation." EAS Publications Series 51 (2011): 59–71. http://dx.doi.org/10.1051/eas/1151005.

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Omukai, Kazuyuki. "First Star Formation." Progress of Theoretical Physics Supplement 147 (2002): 129–53. http://dx.doi.org/10.1143/ptps.147.129.

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Schaye, Joop. "Star Formation Thresholds." Proceedings of the International Astronomical Union 3, S244 (June 2007): 247–55. http://dx.doi.org/10.1017/s1743921307014056.

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AbstractTo make predictions for the existence of “dark galaxies”, it is necessary to understand what determines whether a gas cloud will form stars. Star formation thresholds are generally explained in terms of the Toomre criterion for gravitational instability. I contrast this theory with the thermo-gravitational instability hypothesis of Schaye (2004), in which star formation is triggered by the formation of a cold gas phase and which predicts a nearly constant surface density threshold. I argue that although the Toomre analysis is useful for the global stability of disc galaxies, it relies on assumptions that break down in the outer regions, where star formation thresholds are observed. The thermo-gravitational instability hypothesis can account for a number of observed phenomena, some of which were thought to be unrelated to star formation thresholds.
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Burrows, Adam. "Protoneutron Star Formation." Publications of the Astronomical Society of Australia 7, no. 4 (1988): 371–81. http://dx.doi.org/10.1017/s1323358000022487.

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AbstractThe theory of neutron star formation is addressed in the light of the detected neutrino burst from SN 1987A. A brief review of how supernova neutrino theory has evolved over the last 30 years and a general analysis of the SN 1987A detections is presented.
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Williams, Jonathan P. "Clustered star formation." Proceedings of the International Astronomical Union 1, S227 (May 2005): 128–34. http://dx.doi.org/10.1017/s1743921305004448.

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Dissertations / Theses on the topic "Star formation"

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Moeckel, Nickolas Barry. "Massive stars, disks, and clustered star formation." Connect to online resource, 2008. http://gateway.proquest.com/openurl?url_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:dissertation&res_dat=xri:pqdiss&rft_dat=xri:pqdiss:3303877.

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Kraus, Adam L. Brown Michael E. Hillenbrand Lynne A. "Multiple star formation." Diss., Pasadena, Calif. : California Institute of Technology, 2010. http://resolver.caltech.edu/CaltechETD:etd-08252009-233632.

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Ferreira, Carolina Gribel de Vasconcelos. "Connecting the cosmic star formation rate with the local star formation rate." Instituto Nacional de Pesquisas Espaciais (INPE), 2018. http://urlib.net/sid.inpe.br/mtc-m21b/2018/02.05.17.02.

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We present a model that unifies the cosmic star formation rate (CSFR), obtained through the hierarchical structure formation scenario, with the (Galactic) local star formation rate (SFR). It is possible to use the SFR to generate a CSFR mapping through the density probability distribution functions (PDFs) commonly used to study the role of turbulence in the star-forming regions of the Galaxy. We obtain a consistent mapping from redshift z 20 up to the present (z = 0). Our results show that the turbulence exhibits a dual character, providing high values for the star formation efficiency (h"i 0.32) in the redshift interval z 3.5−20 and reducing its value to h"i = 0.021 at z = 0. The value of the Mach number (Mcrit), from which h"i rapidly decreases, is dependent on both the polytropic index (􀀀) and the minimum density contrast of the gas. We also derive Larsons first law associated with the velocity dispersion (hVrmsi) in the local star formation regions. Our model shows good agreement with Larsons law in the 0.1 − 30pc range (when our model is compared to the observational data), providing typical temperatures T0 2−50K for the gas associated with star formation. As a consequence, dark matter halos of great mass could contain a number of halos of much smaller mass, and be able to form structures similar to globular clusters. Thus, Larsons law emerges as a result of the very formation of large-scale structures, which in turn would allow the formation of galactic systems, including our Galaxy.
Apresentamos um modelo que unifica a Taxa Cósmica de Formação Estelar (CSFR em inglês), obtida atravez do cenário de formação de estruturas, com a taxa de formação estelar local (Galáctica) (SFR em inglês). É possível utilizar a SFR para gerar um mapa da CSFR através da função de distribuição de probabilidade (PDFs) da densidade comumente utilizada no estudo do papel da turbulência nas regiões de formação estelar na Galáxia. Obtemos um mapa consistente a partir de redshift z 20 até o presente (z = 0). Nossos resultados mostram que a turbulência exibe um caráter dual, resultando em altos valores para a eficiência de formação estelar (h"i 0.32) no intervalo de redshift z 3.5 − 20 e reduzindo seu valor para h"i = 0.021 em z = 0. O valor do número de Mach (Mcrit), para o qual h"i decresce rapidamente, é dependente em ambos do índice politrópico (􀀀) e do contraste de densidade do gás (scrit). Derivamos a primeira Lei de Larson associada a disperção de velocidade (hVrmsi) nas regiões de formação de estelar local. Nosso modelo mostra boa concordância com a Lei de Larson no intervalo 0.1 − 30pc (quando nosso modelo é comparado com dados observacionais), com temperaturas típicas T0 2 − 50K para o gás associado a formação estelar. Como consequência, os halos de matéria escura com maior massa poderiam conter halos de menor massa, formando estruturas semelhantes aos aglomerados globulares. Sendo assim, a Lei de Larson emerge como um resultado da formação estelar cosmológica e vinculada com a formação das estruturas em grande escala do universo, da qual possibilitaria a formação de sistemas galacticos, incluindo a nossa Galáxia.
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Belles, Pierre-Emmanuel Aime Marcel. "Formation of stars and star clusters in colliding galaxies." Thesis, University of Hertfordshire, 2013. http://hdl.handle.net/2299/10312.

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Mergers are known to be essential in the formation of large scale structures and to have a significant role in the history of galaxy formation and evolution. Besides a morphological transformation, mergers induce important bursts of star formation. These starburst are characterised by high Star Formation Efficiencies (SFEs) and Specific Star Formation Rates, i.e., high Star Formation Rates (SFR) per unit of gas mass and high SFR per unit of stellar mass, respectively, compared to spiral galaxies. At all redshifts, starburst galaxies are outliers of the sequence of star-forming galaxies defined by spiral galaxies. We have investigated the origin of the starburst-mode of star formation, in three local interacting systems: Arp 245, Arp 105 and NGC7252. We combined high-resolution JVLA observations of the 21-cm line, tracing the Hi diffuse gas, with UV GALEX observations, tracing the young star-forming regions. We probe the local physical conditions of the Inter- Stellar Medium (ISM) for independent star-forming regions and explore the atomic-to-dense gas transformation in different environments. The SFR/H i ratio is found to be much higher in central regions, compared to outer regions, showing a higher dense gas fraction (or lower Hi gas fraction) in these regions. In the outer regions of the systems, i.e., the tidal tails, where the gas phase is mostly atomic, we find SFR/H i ratios higher than in standard Hi-dominated environments, i.e., outer discs of spiral galaxies and dwarf galaxies. Thus, our analysis reveals that the outer regions of mergers are characterised by high SFEs, compared to the standard mode of star formation. The observation of high dense gas fractions in interacting systems is consistent with the predictions of numerical simulations; it results from the increase of the gas turbulence during a merger. The merger is likely to affect the star-forming properties of the system at all spatial scales, from large scales, with a globally enhanced turbulence, to small scales, with possible modifications of the initial mass function. From a high-resolution numerical simulation of the major merger of two spiral galaxies, we analyse the effects of the galaxy interaction on the star forming properties of the ISM at the scale of star clusters. The increase of the gas turbulence is likely able to explain the formation of Super Star Clusters in the system. Our investigation of the SFR–H i relation in galaxy mergers will be complemented by highresolution Hi data for additional systems, and pushed to yet smaller spatial scales.
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Crawford, John W. "Star formation in galaxies." Thesis, Queen Mary, University of London, 1988. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.437102.

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Glenn, Jason 1968. "Millimeter-wave polarimetry of star formation regions and evolved stars." Diss., The University of Arizona, 1997. http://hdl.handle.net/10150/282440.

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A new λ = 1.3 mm polarimeter, Cyclops, was constructed to make observations of dust continuum emission from star formation regions. The polarization of the inner arcminute of DR 21 was mapped with Cyclops. The polarization percentage and position angle are remarkably constant, indicating a uniform magnetic field throughout the cloud. Turbulent gas motions are a more significant source of support against self gravity in the cloud core than thermal pressure or magnetic fields. The polarization toward the cloud core increases slightly from λ = 100 μm to λ = 2 mm and is consistent with the standard dust composition of silicates and graphite. A small continuum polarization survey of cloud cores with embedded protostars was made with Cyclops and combined with observations from the literature. There is no clear tendency for any preferred alignment of cloud core elongations with respect to magnetic field lines, especially for the bright, high mass star forming regions. This confirms that the massive cloud cores are magnetically supercritical. The magnetic field lines appear randomly oriented with respect to the local Galactic plane position angles, implying that the random component of the Galactic magnetic field dominates the spiral component in this sample. Three-σ upper limits of 0.4%, 1.2%, and 1.2% were placed on the polarization of the HCO⁺ J = 1-0 emission line from the DR 21 and Mon R2 molecular outflows, and the CS J = 2-1 line from the IRAS 16293-2422 molecular outflow, respectively. These polarizations are an order of magnitude lower than predicted by theoretical models. In the case of DR 21, the lack of polarization is probably due to a disordered magnetic field in clumpy, turbulent gas, although multiple scattering may also diminish the polarization. CS J = 2-1 polarizations of 0.9% ± 0.1% and 5.1% ± 1.5% were observed from the envelopes of the evolved stars IRC+10216 and CRL 2688, respectively. An anisotropic optical depth to escape of infrared photons from the central star, perhaps caused by a toroidal dust distribution, could generate the IRC+10216 polarization.
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Cernohorsky, Jan. "Neutrino driven neutron star formation." Amsterdam : Amsterdam : Rodopi ; Universiteit van Amsterdam [Host], 1990. http://dare.uva.nl/document/91884.

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Dale, J. E. "Feedback in star cluster formation." Thesis, University of Cambridge, 2004. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.598249.

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Massive stars emit strong fluxes of ionising radiation and their dynamical impact on their natal clusters is expected to be severe. The outflows generated expel residual gas from the cluster and can potentially gravitationally disrupt it. The loss of its reserves of molecular gas also prevents the cluster forming more stars. Star-formation and star cluster evolution cannot be fully understood without a proper treatment of feedback. I present a novel technique I have developed to allow the inclusion of the effects of ionising radiation in smoothed particle hydrodynamics (SPH) simulations of star clusters. The new algorithm is able to reproduce the results of simple analytical models and also gives results in good agreement with a more sophisticated Monte Carlo radiative transfer code when tested under highly anisotropic conditions. I simulate the effects of ionising radiation in globular clusters and compare my results with one-dimensional calculations with which I find good agreement. I investigate three cases in which different quantities of gas are distributed in my model cluster such that the as becomes fully ionised either during the HII region’s formation phase, or during its expansion phase, or such that the HII region is trapped inside the cluster core. I find gas expulsion to be quite efficient in the calculations in which the HII region escapes the core. I observe an instability in the second calculation which causes the shocked shell driven by the ionisation front to fragment as the HII region exits the core. The instability produces new structure from the smooth gas in the system, but this structure is rapidly destroyed by the radiation field and the effect of the instability on the evolution of the system is minimal. I also simulate feedback in the context of young embedded clusters, a highly inhomogeneous and anisotropic environment. I find that, again, photoionisation is able to produce novel structure in the ambient gas, causing it to fragment into filaments and beads. This fragmentation of the neutral gas, together with compression by hot ionised gas, which decreases the Jeans mass, lead me to conclude that feedback promotes star formation.
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Bretherton, Derek. "Star formation in molecular clouds." Thesis, Liverpool John Moores University, 2003. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.402927.

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Blain, Andrew William. "Star formation in distant galaxies." Thesis, University of Cambridge, 1995. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.360569.

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Books on the topic "Star formation"

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Bodenheimer, Peter H. Principles of Star Formation. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-15063-0.

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Bodenheimer, Peter. Principles of star formation. Berlin: Springer, 2011.

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Stamatellos, Dimitris, Simon Goodwin, and Derek Ward-Thompson, eds. The Labyrinth of Star Formation. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-03041-8.

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Pudritz, Ralph E., and Michel Fich, eds. Galactic and Extragalactic Star Formation. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2973-9.

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de Castro, A. I. Gómez, M. Heyer, E. Vázquez-Semadeni, R. Rebolo, M. Tagger, and R. E. Pudritz, eds. Magnetic Fields and Star Formation. Dordrecht: Springer Netherlands, 2004. http://dx.doi.org/10.1007/978-94-017-0491-5.

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Accretion processes in star formation. Cambridge, UK: Cambridge University Press, 2000.

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author, Whitworth Anthony P., ed. An Introduction to Star Formation. Cambridge: Cambridge University Press, 2011.

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Accretion processes in star formation. Cambridge, UK: Cambridge University Press, 1998.

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Hartmann, Lee. Accretion processes in star formation. 2nd ed. New York: Cambridge University Press, 2009.

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NATO Advanced Study Institute on Galactic and Extragalactic Star Formation (1987 Whistler, B.C.). Galactic and extragalactic star formation. Dordrecht: Kluwer Academic Publishers, 1988.

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Book chapters on the topic "Star formation"

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Goodwin, Simon. "Star Formation." In Planets, Stars and Stellar Systems, 243–77. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5615-1_5.

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Kundt, Wolfgang. "Star Formation." In Astronomy and Astrophysics Library, 83–85. Berlin, Heidelberg: Springer Berlin Heidelberg, 2001. http://dx.doi.org/10.1007/978-3-662-04347-9_7.

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Bisnovatyi-Kogan, G. S. "Star Formation." In Stellar Physics, 1–23. Berlin, Heidelberg: Springer Berlin Heidelberg, 2002. http://dx.doi.org/10.1007/978-3-662-22639-1_1.

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Beech, Martin. "Star Formation." In Introducing the Stars, 45–67. Cham: Springer International Publishing, 2019. http://dx.doi.org/10.1007/978-3-030-11704-7_2.

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Carraro, Giovanni. "Star Formation." In UNITEXT for Physics, 341–56. Cham: Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-75293-4_16.

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Basu, Shantanu, and Pranav Sharma. "Star Formation." In Essential Astrophysics, 47–68. Boca Raton: CRC Press, 2021. http://dx.doi.org/10.1201/9781003215943-3.

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Bisnovatyi-Kogan, Gennady S. "Star Formation." In Stellar Physics, 1–23. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-642-14734-0_1.

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Fritze-v. Alvensleben, Uta. "Star Formation Efficiencies and Star Cluster Formation." In Starbursts, 209–14. Dordrecht: Springer Netherlands, 2005. http://dx.doi.org/10.1007/1-4020-3539-x_36.

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Zinnecker, Hans. "From Local Star Formation to Global Star Formation." In The Evolution of Galaxies, 147–58. Dordrecht: Springer Netherlands, 2002. http://dx.doi.org/10.1007/978-94-017-3311-3_29.

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Schulz, Norbert S. "Massive Star Formation." In The Formation and Early Evolution of Stars, 217–51. Berlin, Heidelberg: Springer Berlin Heidelberg, 2012. http://dx.doi.org/10.1007/978-3-642-23926-7_9.

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Conference papers on the topic "Star formation"

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Feigelson, Eric D. "Dispersed T Tauri stars and galactic star formation." In The seventh astrophysical conference: Star formation, near and far. AIP, 1997. http://dx.doi.org/10.1063/1.52743.

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Lery, Thibaut. "Star Formation Histories." In MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures. AIP, 2005. http://dx.doi.org/10.1063/1.2077178.

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Myers, P. C. "Early star formation." In The seventh astrophysical conference: Star formation, near and far. AIP, 1997. http://dx.doi.org/10.1063/1.52733.

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Nakamura, Fumitaka, and Zhi-Yun Li. "Present-day star formation: Protostellar outflows and clustered star formation." In FIRST STARS IV – FROM HAYASHI TO THE FUTURE –. AIP, 2012. http://dx.doi.org/10.1063/1.4754324.

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Madau, Piero. "Cosmic star formation history." In The seventh astrophysical conference: Star formation, near and far. AIP, 1997. http://dx.doi.org/10.1063/1.52821.

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Clarke, C. J. "Star formation in clusters." In The seventh astrophysical conference: Star formation, near and far. AIP, 1997. http://dx.doi.org/10.1063/1.52801.

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Garay, Guido. "Star and planet formation." In From Planets to Dark Energy: the Modern Radio Universe. Trieste, Italy: Sissa Medialab, 2008. http://dx.doi.org/10.22323/1.052.0058.

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Zinchenko, I. I. "HIGH MASS STAR FORMATION." In 48-th International student's conferences "Physics of Space". Ural University Press, 2020. http://dx.doi.org/10.15826/b978-5-7996-2935-9.02.

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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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Omukai, Kazuyuki, Hajime Susa, Marcel Arnould, Sydney Gales, Tohru Motobayashi, Christoph Scheidenberger, and Hiroaki Utsunomiya. "Low-metallicity Star Formation." In TOURS SYMPOSIUM ON NUCLEAR PHYSICS AND ASTROPHYSICS—VII. AIP, 2010. http://dx.doi.org/10.1063/1.3455911.

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Reports on the topic "Star formation"

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Collins, David C. "Magnetic Fields in Star Formation". Office of Scientific and Technical Information (OSTI), April 2013. http://dx.doi.org/10.2172/1074570.

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Kane, J. O., D. A. Martinez, M. W. Pound, R. F. Heeter, B. Villette, A. Casner, and R. C. Mancini. Long Duration Directional Drives for Star Formation and Photoionization. Office of Scientific and Technical Information (OSTI), June 2015. http://dx.doi.org/10.2172/1229856.

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Smullen, Rachel, Christopher Fryer, and Jennifer Donley. Seeing is Believing? Understanding the Interplay Between Observations and Simulations of Star Formation. Office of Scientific and Technical Information (OSTI), January 2021. http://dx.doi.org/10.2172/1760564.

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Kane, J. O., D. A. Martinez, M. W. Pound, R. F. Heeter, B. Villette, A. Casner, and R. C. Mancini. Response to FESAC survey, Non-Fusion Connections to Fusion Energy Sciences. Long Duration Directional Drives for Star Formation and Photoionization. Office of Scientific and Technical Information (OSTI), June 2015. http://dx.doi.org/10.2172/1229852.

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Patil, Bhimanagouda S., Ron Porat, G. K. Jayaprakasha, and K. N. C. Murthy. Optimization of Postharvest Storage Conditions to Maintain Fruit Quality and Health Maintaining Properties of Grapefruit. United States Department of Agriculture, January 2010. http://dx.doi.org/10.32747/2010.7613879.bard.

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Antioxidant activity of fruits is gaining wide interest among consumers due to its importance in counteracting oxidative stress, free radicals and preventing DNA damage. Oxygen radical absorbance capacity (ORAC) assay is one of the commonly used assays to measure the antioxidant activity, which is based on hydrogen atom transfer mechanism. Furocoumarins present in grapefruit are reported to have antiproliferative activity, induce GST activity, inhibit biofilm formation and increase bioavailability of drugs. In the present project ORAC values were measured of Star Ruby grapefruit undergone ethylene degreening treatment, cold storage and temperature conditioning treatment, and modified atmosphere packaging which were stored at different temperatures for prolonged period. In addition, furocoumarins were quantified in Star Ruby grapefruits from cold storage and conditioning experiment conducted in Israel. Conditioning treatment is practiced prior cold storage to reduce chilling injury in grapefruits during cold storage for prolonged period. Levels of 6,7-dihyrdoxy bergamottin decreased during storage period in all three treatments.
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6

Sinha, N., M. A. Sitek, and S. A. Lottes. Modeling of Water Film Formation on a Stay-Cable. Office of Scientific and Technical Information (OSTI), August 2019. http://dx.doi.org/10.2172/1557626.

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Rehm, K. E., C. L. Jiang, and M. Paul. Exploring the {sup 18}F(p,{gamma}){sup 19}Ne gateway to the formation of heavy elements in hot stars. Office of Scientific and Technical Information (OSTI), August 1997. http://dx.doi.org/10.2172/521612.

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8

O'Boyle, Ernest. Meta-Analysis and Systematic Reviews for the Social Sciences. Instats Inc., 2023. http://dx.doi.org/10.61700/7qu4pskuz9ke8469.

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This meta-analysis seminar will teach you how to confidently conduct a meta-analysis, from start to finish, in whatever substantive area interests you the most. This seminar will show you that the underlying statistics and analytic procedures are straightforward, but meta-analyses are anything but easy and require care, transparency, and accuracy through every step of the process -- from idea formation to interpretation and presentation of results. This seminar will cover all of this in detail so you can confidently plan and conduct your own meta-analyses. An official Instats certificate of completion is provided and 2 ECTS Equivalent points are offered for European PhD students.
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TABUNOV, I. A., A. P. LAPINA, M. M. KOSTYCHEV, P. S. BEREZINA, and A. V. NIKIFOROVA. METHODOLOGICAL RECOMMENDATIONS FOR COACHES WORKING WITH CHILD ATHLETES ENGAGED IN ROCK CLIMBING. SIB-Expertise, December 2022. http://dx.doi.org/10.12731/er0621.06122022.

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The methodological guide will present aspects that will be useful for coaches in working with their students, in particular psychological work with athletes during the training process and during the competition, and specifically in the pre-start period. It is important for the coach to teach the athlete the techniques of psychological protection, including restoring the stability control system, reducing feelings of anxiety and countering it. It is important to carry out special psychological training. Including effective preparation for competition, based on: social values; formation of mental "internal support"; overcoming psychological barriers. Every day the degree of development and influence of sports reaches a new level. Also, the requirements for athletes in technical, physical and tactical readiness are increasing, respectively, the result of competitive activity will already be determined by readiness and psychological attitude. Psychological preparation is a process aimed at creating a state of mental readiness for competition in athletes. This should be considered the subject of psychological preparation for competitions in sports.
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Clark, Shelley, Sarah Brauner-Otto, and Mahjoube AmaniChakani. Family Change and Diversity in Canada. The Vanier Institute of the Family, June 2024. http://dx.doi.org/10.61959/s2876856c.

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Families in Canada, like those in other high-income countries, have undergone major changes in recentdecades. Women are having fewer children and are less likely to get married, resulting in smaller familyhouseholds and a growing proportion of children being raised by single or cohabiting parents. Divorcerates are declining, indicating that couples who do marry are more likely to stay married. Decisionsabout whether and when to marry or to have children are strongly influenced by ever-changingsocioeconomic factors and cultural values. Certain groups, including immigrants, visible minorities, and Indigenous peoples, follow distinctive patterns of family formation. Geography also shapesfamilies. Quebec and Nunavut stand out with very high cohabitation rates, and fertility is roughly 50% higher in rural than in urban Canada. These profound changes and striking variations have critical implications for the wellbeing of children and their families. Understanding these changes and the diversity in family patterns offers important guidance for developing tailored and effectivesocial policies regarding family, health, education, and housing.
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