Relevant bibliographies by topics / Galactic formation

Academic literature on the topic 'Galactic formation'

Author: Grafiati
Published: 11 March 2023

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Journal articles on the topic "Galactic formation"

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Gnedin, Nickolay Y., Michael L. Norman, and Jeremiah P. Ostriker. "Formation of Galactic Bulges." Astrophysical Journal 540, no. 1 (September 2000): 32–38. http://dx.doi.org/10.1086/309322.

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Milosavljević, Miloš, and David Merritt. "Formation of Galactic Nuclei." Astrophysical Journal 563, no. 1 (December 10, 2001): 34–62. http://dx.doi.org/10.1086/323830.

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Peng, Chih-Han, and Ryoji Matsumoto. "Formation of Galactic Prominence in the Galactic Central Region." Astrophysical Journal 836, no. 2 (February 16, 2017): 149. http://dx.doi.org/10.3847/1538-4357/aa5be8.

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Larson, Richard B. "Galaxy Formation and Cluster Formation." Symposium - International Astronomical Union 126 (1988): 311–21. http://dx.doi.org/10.1017/s007418090004256x.

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A primary motivation for studying globular clusters is that, as the oldest known galactic fossils, they trace the earliest stages of galactic evolution; indeed, they may hold the key to understanding galaxy formation. Thus it is clearly of great importance to learn how to read the fossil record. To do this, we need to understand something about how the globular clusters themselves formed. Were they the first bound objects to form, or did they form in larger pre-existing systems of which they are just small surviving fragments? If the latter, what were the prehistoric cluster-forming systems like? And how did they manage to produce objects like globular clusters?
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Smilgys, Romas, and Ian A. Bonnell. "Star formation in Galactic flows." Monthly Notices of the Royal Astronomical Society 459, no. 2 (April 6, 2016): 1985–92. http://dx.doi.org/10.1093/mnras/stw791.

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Mo, H. J., S. Mao, and S. D. M. White. "The formation of galactic discs." Monthly Notices of the Royal Astronomical Society 295, no. 2 (April 1, 1998): 319–36. http://dx.doi.org/10.1046/j.1365-8711.1998.01227.x.

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Maddox, John. "Rates of galactic star formation." Nature 316, no. 6031 (August 1985): 761. http://dx.doi.org/10.1038/316761a0.

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Kennicutt, Robert C. "Star formation on galactic scales." Proceedings of the International Astronomical Union 2, S237 (August 2006): 311–16. http://dx.doi.org/10.1017/s1743921307001652.

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AbstractNew multi-wavelength data on nearby galaxies are providing a much more accurate and complete observational picture of star formation on galactic scales. Here I briefly report on recent results from the Spitzer Infrared Nearby Galaxies Survey (SINGS). These provide new constraints on the frequency and lifetime of deeply obscured star-forming regions in galaxies, the measurement of dust-corrected star formation rates in galaxies, and the form of the spatially-resolved Schmidt law.
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Tutukov, A. V. "Star Formation in Galactic Nuclei." Symposium - International Astronomical Union 121 (1987): 533–35. http://dx.doi.org/10.1017/s0074180900155573.

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The star formation in galactic open clusters leads, as a rule, to a complete disruption of the latter (Tutukov, 1978) because of the shallow potential wall of these clusters. The matter of dense galactic nuclei is in deep potential walls what drastically changes the star formation regime. The numerical dynamical model of the star formation in galactic nuclei with the mass 6 109 M⊙ and the radius ~ 430pc was proposed by Loose et al (1982). It includes old and newly-formed stars, gas and dust distributed initially as in the center of our Galaxy. The model takes into account the star formation, supernova explosions, stellar winds, the turbulent motion of the gas component, non-grey radiative energy transfer, the influx of gas from old stars and from the outside. The main parameter of our model is the time of dissipation of the kinetic energy of the gas component Td. Supernova explosions are the main source of this energy. The results of numerical experiments help to point out two main regimes of the star formation in galactic nuclei: stationary and bursting. In the stationary regime the rate of the star formation is constant and it equals to the rate of the gas input. The formation of a long-living superstar is possible in this case (Krügel, Tutukov, 198b). In the bursting regime the periods of an active star formation alternate with those of almost a complete absence of the star formation. The main reason for supressing the star formation process is supernova explosions which throw the gas out of the galactic nuclei.
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Lerner, E. J. "Galactic model of element formation." IEEE Transactions on Plasma Science 17, no. 2 (April 1989): 259–63. http://dx.doi.org/10.1109/27.24633.

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Dissertations / Theses on the topic "Galactic formation"

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Peschken, Nicolas. "Formation and evolution of galactic discs." Thesis, Aix-Marseille, 2016. http://www.theses.fr/2016AIXM4732/document.

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Cette thèse explore la formation, l’évolution et la structure des galaxies spirales à l’aide de simulations, en mettant l’accent sur le disque. Elle s'appuie sur nos simulations hydrodynamiques à N-corps mettant en scène une fusion majeure entre deux galaxies à disque à haut redshift, chacune en possession d’un halo de gaz chaud. Les disques des progéniteurs sont détruits par la fusion, et un disque étendu se forme dans la galaxie ainsi obtenue à partir d’étoiles nouvellement formées, la formation stellaire étant alimentée par le halo de gaz. A la fin de la simulation, la nouvelle galaxie montre toutes les propriétés d’une galaxie spirale, prouvant pour la première fois avec des simulations comment une galaxie de type tardif peut être créée par une fusion majeure.Dans cette thèse sont analysées plusieurs propriétés des galaxies ainsi obtenues, comme la migration stellaire, la rotation angulaire de la barre, et les profils radiaux de densité surfacique. Ce dernier point en particulier constitue une partie importante de mon travail, le fit de ces profils permettant d'obtenir les grandeurs caractéristiques du disque. Nos disques montrent en effet un profil de type II (troncature vers le bas) dont il est possible d'extraire les longueurs d'échelle et le rayon de troncature. Le but est notamment de chercher ce qui module les valeurs de ces paramètres (ceux-ci étant très différents d'une simulation à l'autre), ainsi que les phénomènes à l'origine de ce profil spécifique. Enfin, certains disques de type III (troncature du profil vers le haut) obtenus pour des simulations de galaxies isolées sont présentés et analysés, afin de comprendre leur provenance
This thesis explores the formation, evolution and structure of spiral galaxies using simulations, with an emphasis on the disc component. It is based on our N-body/SPH simulations involving a major merger between two disc galaxies at high redshift, both in possession of a hot gaseous halo. The discs of the progenitors are destroyed by the merger, and a well-extended disc forms in the remnant galaxy from newly born stars, star formation being fuelled by the gaseous halo. By the end of the simulation, the remnant galaxy shows all the properties of a spiral galaxy, proving for the first time in simulations how a late-type galaxy can be created from a major merger.In this thesis, several properties of the remnant galaxy are analysed, such as the stellar migration, the bar pattern speed, and the surface density radial profiles. This last point in particular represents a significant part of my work, using fits of the profiles to obtain the characteristic parameters of the disc. Our discs show a type II profile (downbending truncation), so that we can derive their scalelengths and truncation radius. The goal is to understand what determines the values of these parameters (which are very different from one simulation to another), as well as the origin of this specific profile. Finally, some type III discs (upbending truncation) obtained for simulations of isolated galaxies are presented and analysed, in order to investigate their formation mechanism
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Puxley, Philip John. "Vigorous star formation in galactic nuclei." Thesis, University of Edinburgh, 1989. http://hdl.handle.net/1842/27222.

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Barnes, A. T. "A comparison of star formation within the galactic centre and galactic disc." Thesis, Liverpool John Moores University, 2018. http://researchonline.ljmu.ac.uk/8633/.

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Stars are of fundamental importance to the entire field of astronomy. The conversion of elements and the distribution of energy throughout the lifetime of stars drives the evolution of the Universe. Despite this, we do not have a unified understanding of the formation process for all stars. This thesis attempts to move forward this understanding, by focussing on the question: How do the initial conditions of star-forming regions vary across environments, and do these influence the process of star formation? To investigate the initial conditions of star formation, regions on the verge of forming stars have to be first identified and analysed. These regions have to be untouched by the disruptive effects of stellar feedback, such that the natal conditions of the gas – e.g. kinematics and chemistry – are not destroyed. Quiescent regions that are expected to form low-mass stars have been well studied over the past few decades, and the general process of low-mass star formation is well understood. Only relatively recently, however, has a group of objects being identified as being potential hosts of these initial stages of high-mass star formation: Infrared Dark Clouds (IRDCs). The study of these objects is difficult, due to both their rarity and complexity. An end-to-end understanding of high-mass star formation is, therefore, much less developed compared to their lower mass counterparts. This thesis presents the study of a sample of IRDCs within the Disc and Centre of the Milky Way; two very different environments. Several key aspects of the star formation process within IRDCs from these environments are investigated. Firstly, a chemical signpost – the deuterium fraction of N2H+ – is used to identify the regions of dense and cold gas on the verge of forming high-mass stars within a quiescent Disc IRDC, which can be used to study the initial conditions for star formation. Omitting potential beam dilution effects, chemical modelling suggests that the cloud could have reached a global chemical equilibrium, and, if so, would also be dynamically old (survived for several free-fall times). This timescale, with estimates of the embedded stellar mass, is used to determine star formation rates and efficiencies. Secondly, the kinematic structures within two apparently similar Disc IRDCs are identified using dense gas tracers – C18O and N2H+. The properties of these structures appear to be very similar, hinting at a similar formation scenario for both clouds, or, potentially, that these may be inherent to the larger Disc IRDC population. The dynamics of these filaments also show that they may be merging, which would suggest a compressive mode of turbulence driving. These structures are then linked to the larger kinematic structures – identified using a lower density tracing molecule, 13CO – and found to show good coherence with the brightest, most extended structures. These are then placed in the context of the previously identified Galactic scale structures, and in doing so show that IRDCs could be the densest parts of the much larger arm or inter-arm filamentary structures. Thirdly, the level of star formation within the Galactic Centre is investigated on both global (∼ 100 pc) and local (∼ 1 pc) scales. On a global scale, the star formation rate has been determined from all the available observational star formation diagnostics – i.e. direct counting of young stellar objects and integrated light measurements – and found to be in agreement with previous studies; i.e. around one-to-two orders of magnitude lower than predicted by the star formation models. On individual cloud scales, the star formation efficiency per free-fall time is in better agreement with the model predictions. However, uncertainties on the properties of these regions, such as the mode of turbulence driving, limit the further verification or falsification of the star formation theories. Lastly, the investigation of the local scale star formation within the Galactic Centre highlighted a particular part of the parameter space as the most promising to further test the star formation theories. In light of this, high-spatial resolution ALMA observations have been taken of two Galactic Centre clouds within this regime. Early results show that they have a complex structure, similar to that seen within Disc IRDCs, containing both filamentary and core-like features. Investigation of the brightest, most compact core region shows that it contains a very rich chemistry, and, of particular interest, is the rigorous detection of the pre-biotic molecule formamide (NH2CHO). When placing the results of this thesis in the bigger context of star formation theory, they appear to show interesting implications for the initially posed question – what is the influence of environment on the process of star formation? It is found here that despite the very different cloud scale properties of these regions, the star formation efficiency per free-fall time is surprisingly similar. To investigate this, the properties of the individual sites of high-mass star formation, the high-mass star-forming cores, are compared. Interestingly, despite the different environmental conditions, several key properties of the cores, such as their size and mass distribution, are also found to be very similar. The similarity of high-mass core properties and star formation rate per free fall time implies that once a region has produced high-mass cores, the evolution of these cores towards star formation must be similar. The difference in the global/environmental properties of the gas must then be setting the total star formation rate within these regions, by limiting the number of cores that can form. In particular, the mode of turbulence driving may play a major role in governing the fraction of gas that can be converted into stars per free-fall time within these two environments.
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Haehnelt, Martin. "Quasars and the formation of galactic nuclei." Thesis, University of Cambridge, 1994. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.319491.

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Brown, Richard Joseph Norman. "The formation and evolution of elliptical galaxies." Thesis, University of Birmingham, 2003. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.273922.

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Quinn, Lyshia Jane. "Maser hunting in the galactic plane." Thesis, University of Manchester, 2010. https://www.research.manchester.ac.uk/portal/en/theses/maser-hunting-in-the-galactic-plane(efee9222-ec4e-4153-aa6a-4047c08430f9).html.

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The process of massive star formation greatly influences its surroundings through their outflows, vast UV output and shocks from their supernova death. They form at great distances from the Earth, enshrouded by dust and gas and have relatively short lifetimes. Astrophysical masers which form in these environments may act as locators of the star forming regions. The aim of this thesis is to study massive star formation using masers to probe these regions. The three main masers used in this thesis are the Class I and Class II methanol masers and the 6035 MHz ex-OH maser. The methanol masers are divided into two groups, Class I and Class II, based on their distance from a central source. The Class I masers are separated 1-2 pc from a central source, the central source is the star forming region. The Class II masers are associated close to a star forming source. They are often associated with a 6035 MHz ex-OH maser. The 6035 MHz ex-OH masers are less common than the 6668 MHz Class I methanol masers. They are often found at sites of the 6668 MHz Class I masers and 1665/7 MHz OH masers. This thesis presents two maser surveys, the Methanol Multibeam (MMB) survey and the Class I survey. The MMB survey is currently surveying the entire Galactic Plane for the 6668 MHz Class II methanol maser and the 6035 MHz ex-OH maser. Over 60\% of the survey in the Southern hemisphere is now complete using the Parkes telescope. Over 900 6668 MHz Class I methanol masers and 110 6035 MHz ex-OH masers have been detected, with all of these masers pinpoint the location of newly forming high mass stars. Follow up observations to determine the precise locations of the 6668 MHz methanol and 6035 MHz ex-OH masers are currently underway. The first ever unbiased Class I survey has observed 1 sq degree of the Galactic Plane for the 44 GHz Class I methanol masers using the Mopra telescope in Australia. The 44 GHz Class II methanol masers are hypothesised to be associated with the outflows of high mass stellar objects. The Class I survey has detected 25 44 GHz methanol masers, with 23 being new detections. A smaller survey for 36 GHz Class I masers was also conducted using the Mopra telescope centered on the region with the highest population of 44 GHz Class I masers.
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Smilgys, Romas. "Formation of stars and stellar clusters in galactic environment." Thesis, University of St Andrews, 2018. http://hdl.handle.net/10023/13229.

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Star and stellar cluster formation in spiral galaxies is one of the biggest questions of astrophysics. In this thesis, I study how star formation, and the formation of stellar clusters, proceeds using SPH simulations. These simulations model a region of 400 pc and 107 solar masses. Star formation is modelled through the use of sink particles which represent small groups of stars. Star formation occurs in high density regions, created by galactic spiral arm passage. The spiral shock compresses the gas and generates high density regions. Once these regions attain sufficiently high density, self-gravity becomes dominant and drives collapse and star formation. The regions fragment hierarchically, forming local small groups of stars. These fall together to form clusters, which grow through subsequent mergers and large scale gas infall. As the individual star formation occurs over large distances before forming a stellar cluster, this process can result in significant age spreads of 1-2 Myrs. One protocluster is found to fail to merge due to the large scale tidal forces from the nearby regions, and instead expands forming a dispersed population of young stars such as an OB association.
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Bailin, Jeremy. "Alignment of galactic components in models of galaxy formation." Diss., The University of Arizona, 2004. http://hdl.handle.net/10150/280672.

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In this thesis, we study the relationship between the angular momentum and shape of galactic disks, satellite galaxies, dark matter halos, and large scale structure using N-body simulations in the context of current models of galaxy formation. In warped galactic disks, the angular momenta of the inner and outer disk are misaligned. We have calculated the torques a misaligned halo imparts on an embedded galactic disk. N-body simulations of disks subject to torques of this strength indicate that the disk tilts in response and develops a trailing warp of the same magnitude as the Milky Way warp. We have investigated whether the warp of the Milky Way's disk is caused by nearby satellite galaxies. The misaligned warp angular momentum is anti-aligned with the orbital angular momentum of the Sgr dSph, and is of the same magnitude. This suggests that Sgr is responsible for the warp. However, N-body simulations of such disk-satellite interactions indicate that the warps excited by Sgr with its current mass and orbit are much smaller than the warp of the Milky Way. The alignment of the shapes and angular momenta of dark matter halos and the large scale environment has been studied in cosmological dark matter simulations. We have analyzed several late snapshots of such a simulation and found rotation of the triaxial figure of the halos. The figure rotates about the minor axis in most cases, at a rate that follows a log-normal distribution centred on Ωp = 0.148 h km s⁻¹ kpc⁻¹. Halos have triaxial shapes that become more spherical at larger radii. The principal axes of individual halos show strong internal alignment, as does the angular momentum, which is usually oriented along the minor axis. This alignment is not perfect, and the median misalignment is large enough to cause galactic warps. The minor axes of halos tend to point perpendicular to filaments and sheets. Major axes show a weaker tendency to point along filaments. These alignments are much stronger for higher mass halos. The angular momenta of galaxy mass halos tend to point along filaments and sheets, while those of group mass halos point perpendicular to the surrounding mass distribution.
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Renda, Agostino. "The formation of stellar halos in late-type galaxies." Swinburne Research Bank, 2007. http://hdl.handle.net/1959.3/34778.

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Thesis (PhD) - Swinburne University of Technology, 2007.
Submitted for the degree of Doctor of Philosophy, Swinburne University of Technology - 2007. Typescript. "May 2007". Bibliography: p. 225-237.
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Chamcham, Khalil. "The evolution of galactic discs with a star formation threshold." Thesis, University of Sussex, 1995. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.262321.

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Books on the topic "Galactic formation"

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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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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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Italy) Multi-Spin Galaxies (Conference) (2013 Naples. Multi-Spin Galaxies: Proceedings of a conference held at INAF-Osservatorio Astronomico di Capodimonte, Napoli, Italy, 30 September-3 October 3 2013. San Francisco: Astronomical Society of the Pacific, 2014.

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Galaxy wars: Stellar populations and star formation in interacting galaxies : proceedings of a conference held at East Tennessee State University, Johnson City, Tennessee, USA, 19-22 July 2009. San Francisco: Astronomical Society of the Pacific, 2010.

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Kaper, Lex, Edward P. J. van den Heuvel, and Patrick A. Woudt, eds. Black Holes in Binaries and Galactic Nuclei: Diagnostics, Demography and Formation. Berlin, Heidelberg: Springer Berlin Heidelberg, 2001. http://dx.doi.org/10.1007/b75143.

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Bahcall, John N. NASA astrophysical theory grant NAG5-2882, formation of structure in the universe: Final report. [Washington, D.C: National Aeronautics and Space Administration, NASA Headquarters, 1997.

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Karl, Fisher, and United States. National Aeronautics and Space Administration., eds. NASA astrophysical theory grant NAG5-2882, formation of structure in the universe: Final report. [Washington, D.C: National Aeronautics and Space Administration, NASA Headquarters, 1997.

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Symposium, International Astronomical Union. Formation and evolution of galaxy bulges: Proceedings of the 245th Symposium of the International Astronomical Union, held in Oxford, United Kingdom, July 16-20, 2007. Cambridge, U.K: Cambridge University Press, 2008.

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(Japan), Kokuritsu Tenmondai, Astronomical Society of the Pacific, Subaru International Conference (3rd : 2011 : Shuzenji-chō, Japan), and NAOJ Symposium (1st : 2011: Shuzenji-chō, Japan), eds. Galactic archaeology: Near-field cosmology and the formation of the Milky Way. San Francisco: Astronomical Society of the Pacific, 2012.

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AGN feedback in galaxy formation: Proceedings of the workshop held in Vulcano, Italy, May 18--22, 2008. New York: Cambridge University Press, 2011.

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Book chapters on the topic "Galactic formation"

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Pudritz, Ralph E., and Michel Fich. "Galactic Star Formation." In Galactic and Extragalactic Star Formation, 645–50. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2973-9_44.

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Wada, Keiichi, and Asao Habe. "Primeval Starburst and Bulge Formation." In Galactic Bulges, 397–98. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_69.

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Palouš, Jan. "Cloud Disruption and Formation." In Active Galactic Nuclei, 314–15. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0963-2_93.

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Sofue, Yoshiaki. "Star Formation and Death." In Galactic Radio Astronomy, 57–99. Singapore: Springer Singapore, 2017. http://dx.doi.org/10.1007/978-981-10-3445-9_3.

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Pfenniger, Daniel. "Delayed Formation of Bulges by Dynamical Processes." In Galactic Bulges, 387–90. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_65.

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Renzini, Alvio. "Formation and Evolution of Stars in Galactic Bulges." In Galactic Bulges, 151–68. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_10.

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Fridman, A. M., and V. L. Polyachenko. "On the Formation Mechanisms for Ellipticals and Bulges." In Galactic Bulges, 377–80. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_61.

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Silk, Joseph. "Bimodal Star Formation, Starbursts, and Galaxy Formation." In Galactic and Extragalactic Star Formation, 503–17. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2973-9_30.

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Nuritdinov, S. N. "Bulges and ellipticals: can formation mechanisms be the same?" In Galactic Bulges, 403–4. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_72.

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Rocca-Volmerange, B., and O. K. Sil’Chenko. "On the Difference in Formation History between Bulges and Ellipticals." In Galactic Bulges, 431–32. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-0922-2_86.

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Conference papers on the topic "Galactic formation"

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Gnedin, Nickolay Y., Michael L. Norman, and Jeremiah P. Ostriker. "Formation of galactic bulges." In AFTER THE DARK AGES. ASCE, 1999. http://dx.doi.org/10.1063/1.58634.

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Peletier, Reynier, Marc Balcells, Jesus Falcon-Barroso, and Alister Graham. "The formation of galactic bulges." In Baryons in Dark Matter Halos. Trieste, Italy: Sissa Medialab, 2004. http://dx.doi.org/10.22323/1.014.0060.

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Nipoti, Carlo, Victor P. Debattista, and C. C. Popescu. "Are Galactic Coronae Thermally Unstable?" In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458472.

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Marinacci, F., J. Binney, F. Fraternali, C. Nipoti, L. Ciotti, P. Londrillo, Victor P. Debattista, and C. C. Popescu. "Galactic Fountains and Gas Accretion." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458477.

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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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Cooper, A. P., S. Cole, C. S. Frenk, S. D. M. White, G. De Lucia, A. Helmi, A. J. Benson, et al. "Galactic Stellar Haloes in the CDM Model." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458514.

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Courty, Stéphanie, Brad K. Gibson, Romain Teyssier, Victor P. Debattista, and C. C. Popescu. "The Circum-Galactic Gas Around Cosmologically Simulated Disks." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458467.

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Jalali, Behrang, Markus Kissler-Patig, Karl Gebhardt, Eva Noyola, Nadine Neumayer, Victor P. Debattista, and C. C. Popescu. "Intermediate Mass Black Holes in Galactic Globular Clusters." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458500.

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Weiner, Benjamin J., Sebastian Heinz, and Eric Wilcots. "Star Formation Driven Galactic Winds at z∼1.4." In THE MONSTER’S FIERY BREATH: FEEDBACK IN GALAXIES, GROUPS, AND CLUSTERS. AIP, 2009. http://dx.doi.org/10.1063/1.3293019.

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Peterson, Bradley, and Catherine Grier. "Masses of Black Holes in Active Galactic Nuclei." In Nuclei of Seyfert galaxies and QSOs - Central engine & conditions of star formation. Trieste, Italy: Sissa Medialab, 2013. http://dx.doi.org/10.22323/1.169.0030.

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Reports on the topic "Galactic formation"

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Shomer, Ilan, Ruth E. Stark, Victor Gaba, and James D. Batteas. Understanding the hardening syndrome of potato (Solanum tuberosum L.) tuber tissue to eliminate textural defects in fresh and fresh-peeled/cut products. United States Department of Agriculture, November 2002. http://dx.doi.org/10.32747/2002.7587238.bard.

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Abstract:
The project sought to understand factors and mechanisms involved in the hardening of potato tubers. This syndrome inhibits heat softening due to intercellular adhesion (ICA) strengthening, compromising the marketing of industrially processed potatoes, particularly fresh peeled-cut or frozen tubers. However, ICA strengthening occurs under conditions which are inconsistent with the current ideas that relate it to Ca-pectate following pectin methyl esterase (PME) activity or to formation of rhamnogalacturonan (RG)-II-borate. First, it was necessary to induce strengthening of the middle lamellar complex (MLX) and the ICA as a stress response in some plant parenchyma. As normally this syndrome does not occur uniformly enough to study it, we devised an efficient model in which ICA-strengthening is induced consistently under simulated stress by short-chain, linear, mono-carboxylic acid molecules (OAM), at 65 oC [appendix 1 (Shomer&Kaaber, 2006)]. This rapid strengthening was insufficient for allowing the involved agents assembly to be identifiable; but it enabled us to develop an efficient in vitro system on potato tuber parenchyma slices at 25 ºC for 7 days, whereas unified stress was reliably simulated by OAMs in all the tissue cells. Such consistent ICA-strengthening in vitro was found to be induced according to the unique physicochemical features of each OAM as related to its lipophilicity (Ko/w), pKa, protonated proportion, and carbon chain length by the following parameters: OAM dissociation constant (Kdiss), adsorption affinity constant (KA), number of adsorbed OAMs required for ICA response (cooperativity factor) and the water-induced ICA (ICAwater). Notably, ICA-strengthening is accompanied by cell sap leakage, reflecting cell membrane rupture. In vitro, stress simulation by OAMs at pH<pKa facilitated the consistent assembly of ICAstrengthening agents, which we were able to characterize for the first time at the molecular level within purified insoluble cell wall of ICA-strengthened tissue. (a) With solid-state NMR, we established the chemical structure and covalent binding to cell walls of suberin-like agents associated exclusively with ICA strengthening [appendix 3 (Yu et al., 2006)]; (b) Using proteomics, 8 isoforms of cell wall-bound patatin (a soluble vacuolar 42-kDa protein) were identified exclusively in ICA-strengthened tissue; (c) With light/electron microscopy, ultrastructural characterization, histochemistry and immunolabeling, we co-localized patatin and pectin in the primary cell wall and prominently in the MLX; (d) determination of cell wall composition (pectin, neutral sugars, Ca-pectate) yielded similar results in both controls and ICA-strengthened tissue, implicating factors other than PME activity, Ca2+ or borate ions; (e) X-ray powder diffraction experiments revealed that the cellulose crystallinity in the cell wall is masked by pectin and neutral sugars (mainly galactan), whereas heat or enzymatic pectin degradation exposed the crystalline cellulose structure. Thus, we found that exclusively in ICA-strengthened tissue, heat-resistant pectin is evident in the presence of patatin and suberinlike agents, where the cellulose crystallinity was more hidden than in fresh control tissue. Conclusions: Stress response ICA-strengthening is simulated consistently by OAMs at pH< pKa, although PME and formation of Ca-pectate and RG-II-borate are inhibited. By contrast, at pH>pKa and particularly at pH 7, ICA-strengthening is mostly inhibited, although PME activity and formation of Ca-pectate or RG-II-borate are known to be facilitated. We found that upon stress, vacuolar patatin is released with cell sap leakage, allowing the patatin to associate with the pectin in both the primary cell wall and the MLX. The stress response also includes formation of covalently bound suberin-like polyesters within the insoluble cell wall. The experiments validated the hypotheses, thus led to a novel picture of the structural and molecular alterations responsible for the textural behavior of potato tuber. These findings represent a breakthrough towards understanding of the hardening syndrome, laying the groundwork for potato-handling strategies that assure textural quality of industrially processed particularly in fresh peeled cut tubers, ready-to-prepare and frozen preserved products.
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