Gotowe bibliografie tematyczne / Spectral line formation Congresses

Spis treści

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

Gotowa bibliografia na temat „Spectral line formation Congresses”

Autor: Grafiati
Data publikacji: 29 lipca 2024
Data aktualizacji: 31 lipca 2025

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Artykuły w czasopismach na temat "Spectral line formation Congresses"

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Paletou, F., and C. Peymirat. "Full non–LTE spectral line formation." Astronomy & Astrophysics 649 (May 2021): A165. http://dx.doi.org/10.1051/0004-6361/202040005.

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Radiative transfer out of local thermodynamic equilibrium (NLTE) has been increasingly adressed, mostly numerically, for about six decades now. However, the standard NLTE problem most often refers to the only deviation of the distribution of photons from their equilibrium, that is to say a Planckian distribution. Hereafter we revisit after Oxenius (1986, Kinetic theory of particles and Photons – Theoretical Foundations of non–LTE Plasma Spectroscopy, Springer) the so-called full NLTE problem, which considers coupling and therefore solving self–consistently for deviations from equilibrium distr
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Oxenius, J., and E. Simonneau. "Kinetic Theory of Spectral Line Formation." Annals of Physics 234, no. 1 (1994): 60–101. http://dx.doi.org/10.1006/aphy.1994.1074.

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Klevas, J., A. Kučinskas, M. Steffen, E. Caffau, and H. G. Ludwig. "Lithium spectral line formation in stellar atmospheres." Astronomy & Astrophysics 586 (February 2016): A156. http://dx.doi.org/10.1051/0004-6361/201526403.

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Peraiah, A., and M. Srinivasa Rao. "Compton broadening effect on spectral line formation." Astrophysics and Space Science 343, no. 1 (2012): 195–211. http://dx.doi.org/10.1007/s10509-012-1233-0.

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Nikoghossian, A. G. "Spectral line formation in a mesoturbulent atmosphere." Astrophysics 50, no. 2 (2007): 175–86. http://dx.doi.org/10.1007/s10511-007-0017-7.

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Vieytes, Mariela C., Lily L. Zhao, and Megan Bedell. "The Influence of Chromospheric Activity on Line Formation." Astrophysical Journal 981, no. 1 (2025): 4. https://doi.org/10.3847/1538-4357/adb0c6.

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Abstract One of the primary sources of stellar spectral variability is magnetic activity. While our current understanding of chromospheric activity is largely derived from specific lines sensitive to chromospheric heating, such as the Ca ii H and K doublet, previous observational studies have shown that other spectral lines are also affected. To investigate the influence of activity on line formation in greater detail, we constructed a set of stellar models for hypothetical G2 dwarf stars with varying levels of activity and calculated their synthetic spectra. A comparison of these spectra reve
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Grec, C., H. Uitenbroek, M. Faurobert, and C. Aime. "Measuring line formation depths by cross-spectral analysis." Astronomy and Astrophysics 514 (May 2010): A91. http://dx.doi.org/10.1051/0004-6361/200811455.

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Letunov, Andrey Yu, and Valery S. Lisitsa. "Review of Rydberg Spectral Line Formation in Plasmas." Atoms 11, no. 10 (2023): 133. http://dx.doi.org/10.3390/atoms11100133.

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The present review is dedicated to the problem of an array of transitions between highly-excited atomic levels. Hydrogen atoms and hydrogen-like ions in plasmas are considered here. The presented methods focus on calculation of spectral line shapes. Fast and simple methods of universal ionic profile calculation for the Hnα (Δn=1) and Hnβ (Δn=2) spectral lines are demonstrated. The universal dipole matrix elements formulas for the Hnα and Hnβ transitions are presented. A fast method for spectral line shape calculations in the presence of an external magnetic field using the formulas for univers
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Albrow, Michael D., and P. L. Cottrell. "Formation Depths of Spectral Lines in Cepheids." International Astronomical Union Colloquium 155 (1995): 373–74. http://dx.doi.org/10.1017/s0252921100037568.

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There has been a number of observational programmes that have endeavoured to investigate the atmospheric velocity fields in Cepheids (e.g., Sanford 1956, Wallerstein et al. 1992, Butler 1993). These studies measured the radial velocities of lines of different strength, excitation and ionisation potential as these provide an indication of line formation at different levels in the atmosphere. From these measurements, the presence of velocity gradients can be inferred, but determination of the magnitude of such gradients requires knowledge of the spectral line depth of formation. Through dynamica
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Dravins, Dainis. "Observed and computed spectral line profiles." Symposium - International Astronomical Union 176 (1996): 519–22. http://dx.doi.org/10.1017/s0074180900083534.

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For the diagnostics of stellar surface structure, studies of “ordinary” line profiles may prove inadequate. However, hydrodynamic models may be constrained by second-order quantities, such as line asymmetries and wavelength shifts (and especially the differential behavior between lines of different excitation potential, ionization stage, and height of formation, as well as by the time dependence).
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Rozprawy doktorskie na temat "Spectral line formation Congresses"

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Gibb, Andrew Gordon. "Spectral line observations of two contrasting molecular clouds : Lynds 1630 and G34.3+0.2." Thesis, University of Kent, 1994. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.239827.

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Bedikoglou, Isidore. "A study of spectral line surveys for four regions related to star formation." Thesis, University of Manchester, 2009. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.514420.

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Star formation is a process that has been studied extensively during the last decades. With the advent of advanced instruments our knowledge has expanded beyond the point of general descriptions. From simple models of gravitational contraction of spherical clouds we have managed to give more detailed descriptions about the inner processes and the chemistry within the environment of proto stars and young stellar objects. Still there are several issues that have not been fully understood, such as the formation of stars with very large masses, the exact mechanism that generates strong bipolar out
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Lo, Wing-Chi Nadia Physics Faculty of Science UNSW. "A multi-molecular line study of an entire giant molecular cloud." Awarded by:University of New South Wales. Physics, 2009. http://handle.unsw.edu.au/1959.4/44587.

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A unified theory of star formation remains one of the major unsolved issues in astrophysics. Presented here are the results of multi-molecular lines mapping of the entire giant molecular cloud G333, comprised sites of low- and high-mass star forming regions in various evolution stages of star formation. The result shows the spatial distribution of CS, HCO+, HCN and HNC are similar on large scales, while N2H+ seems to trace preferentially the very densest regions, possibly due to the chemical difference, that N2H+ is sensitive to temperature and readily destroyed by CO. Two analysis methods wer
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Li, Shanghuo, Junzhi Wang, Zhi-Yu Zhang, et al. "Millimetre spectral line mapping observations towards four massive star-forming H ii regions." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/623847.

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We present spectral line mapping observations towards four massive star-forming regions Cepheus A, DR21S, S76E and G34.26+0.15 - with the IRAM 30-m telescope at the 2 and 3 mm bands. In total, 396 spectral lines from 51 molecules, one helium recombination line, 10 hydrogen recombination lines and 16 unidentified lines were detected in these four sources. An emission line of nitrosyl cyanide (ONCN, 14(0), 14-13(0), (13)) was detected in G34.26+0.15, as the first detection in massive star-forming regions. We found that c-C3H2 and NH2D show enhancement in shocked regions, as suggested by the evid
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Martinez, Osorio Yeisson Fabian. "Atomic Processes in Stellar Atmospheres : Inelastic Collisions and Effects on Late-type Spectra." Doctoral thesis, Uppsala universitet, Teoretisk astrofysik, 2015. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-249168.

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Chemical abundances as measured from stellar spectral lines are often subject to uncertainties due to lack of accurate data for inelastic collisions, which is needed for non-local thermodynamic equilibrium (non-LTE) modelling. For cool stars, understanding of collision processes with electrons and hydrogen atoms is required to achieve high precision measurements. In this thesis, I have investigated the role of these collisions on the non-LTE formation of Li and Mg spectral lines in late-type stars. In the case of Li, electron impact excitation processes were calculated using the R-matrix with
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Hindson, Luke Paul. "The G305 star forming complex : a panoramic view of the environment and star formation." Thesis, University of Hertfordshire, 2012. http://hdl.handle.net/2299/9197.

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This thesis presents molecular line and radio continuum observations of the giant molecular cloud (GMC) complex known as G305. The energy input from high-mass stars in the form of powerful winds and ionising radiation is one of the primary feedback mechanisms in GMCs. This feedback is thought to play a dual role both dispersing and destroying the natal environment but also sweeping up and compressing molecular gas and potentially triggering new episodes of star formation. Despite their importance to the evolution of GMCs and galaxies as a whole, the physical processes behind the formation and
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Pacheco-Vazquez, Susana. "Unbiased Spectral Survey towards the intermediate-mass Class 0 protostar Cep E-mm." Thesis, Grenoble, 2012. http://www.theses.fr/2012GRENY066/document.

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Les protoétoiles de masse intermédiaire (IM) (2 ≤ M* ≤ 8 Msun) sont le lien entre les étoiles de faible et haute masse car elles couvrent également un intervalle intermédiaire de luminosités, de densités et de températures [Fuente et al., 2012]. Même si les « IM-YSOs » jouent un rôle important dans l'étude de la formation des étoiles, on a très peu de connaissances sur la formation et l'évolution des premières étapes des protoétoiles de masse intermédiaire. Les études systématiques spectrales sont un outil puissant pour caractériser la composition chimique d'un objet astrophysique, et la seule
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Collet, Remo. "On the Chemical Composition of Metal-Poor Stars : Impact of Stellar Granulation and Departures from Local Thermodynamic Equilibrium on the Formation of Spectral Lines." Doctoral thesis, Uppsala University, Department of Astronomy and Space Physics, 2006. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-7121.

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<p>The information about the chemical compositions of stars is encoded in their spectra. Accurate determinations of these compositions are crucial for our understanding of stellar nucleosynthesis and Galactic chemical evolution. The determination of elemental abundances in stars requires models for the stellar atmospheres and the processes of line formation. Nearly all spectroscopic analyses of late-type stars carried out today are based on one-dimensional (1D), hydrostatic model atmospheres and on the assumption of local thermodynamic equilibrium (LTE). This approach can lead to large systema
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Benredjem, Djamel. "Etude théorique du déplacement des raies spectrales par effet de polarisation dans les plasmas denses : cas des raies de l'hélium hydrogenoïde." Paris 6, 1986. http://www.theses.fr/1986PA066016.

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Le déplacement des raies de l'hélium hydrogenoïde émises dans les plasmas denses a été calculé en considérant l'effet des électrons libres et celui des ions perturbateurs sur l'émetteur. Le premier, déterminé par une méthode de potentiel auto-consistant, induit un déplacement vers le rouge alors que le second, calcule par perturbation, décale les raies vers le bleu. Deux méthodes de calcul de cette grandeur ont été développées : l'une permet d'évaluer le déplacement comme moment spectral du profil complet; l'autre, plus simple, séparé les deux contributions et peut s'appliquer à des états très
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García, Pérez Ana Elia. "On the Abundances of Li, Be and O in Metal-Poor Stars in the Galaxy." Doctoral thesis, Uppsala University, The Uppsala Astronomical Observatory, 2005. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-4814.

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<p>Stellar atmospheres constitute excellent environments to study the chemical evolution of our Galaxy. The chemical composition of these atmospheres reflects the composition of the gas from where these stars were born. As the Galaxy evolves, the composition of the gas changes from being primordial (Big-Bang nucleosynthesis) to being enriched in heavy elements (stellar and interstellar nucleosynthesis). The abundances of fragile chemical elements can be affected by stellar mixing processes. Precise lithium, beryllium and oxygen abundance determinations in old stars are presented in this thesis
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Książki na temat "Spectral line formation Congresses"

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International, Conference on Spectral Line Shapes (14th 1998 State College Pennsylvania). Spectral line shapes. American Institute of Physics, 1999.

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Marco, Zoppi, and Ulivi Lorenzo, eds. Spectral line shapes. American Institute of Physics, 1997.

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Spain) International Conference on Spectral Line Shapes (19th 2008 Valladolid. Spectral line shapes: 19th International Conference on Spectral Line Shapes, Valladolid, Spain, 15-20 June 2008. Edited by Gigosos Marco A and González, Manuel A. (Manuel Angel). American Institute of Physics, 2008.

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Ala.) International Conference on Spectral Line Shapes (18th 2006 Auburn. Spectral line shapes: 18th International Conference on Spectral Line Shapes, Auburn, Alabama, 4-9 June 2006. Edited by Oks, E. A. (Evgeniĭ Aleksandrovich), Pindzola M. S, and American Institute of Physics. American Institute of Physics, 2006.

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International Conference on Spectral Line Shapes (12th 1994 Toronto, Ont.). Spectral line shapes.: 12th ICSLS, Toronto, Canada, June 1990. Edited by May A. David, Drummond J. R, and Oks E. A. American Institute of Physics, 1995.

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Serbian, Conference on Spectral Line Shapes in Astrophysics (6th 2007 Sremski Karlovci Serbia). Spectral line shapes in astrophysics: VI Serbian Conference on Spectral Line Shapes in Astrophysics (VI SCSLSA), Sremski Karlovci, Serbia, 11-15 June 2007. American Institute of Physics, 2007.

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Serbian, Conference on Spectral Line Shapes in Astrophysics (6th 2007 Sremski Karlovci Serbia). Spectral line shapes in astrophysics: VI Serbian Conference on Spectral Line Shapes in Astrophysics (VI SCSLSA), Sremski Karlovci, Serbia, 11-15 June 2007. American Institute of Physics, 2007.

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Serbian Conference on Spectral Line Shapes in Astrophysics (6th 2007 Sremski Karlovci, Serbia). Spectral line shapes in astrophysics: VI Serbian Conference on Spectral Line Shapes in Astrophysics (VI SCSLSA), Sremski Karlovci, Serbia, 11-15 June 2007. Edited by Popović Luka Č, Dimitrijević Milan S, and Serbia Ministarstvo nauke. American Institute of Physics, 2007.

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Č, Popović Luka, Dimitrijević Milan S, and Serbia Ministarstvo nauke, eds. Spectral line shapes in astrophysics: VI Serbian Conference on Spectral Line Shapes in Astrophysics (VI SCSLSA), Sremski Karlovci, Serbia, 11-15 June 2007. American Institute of Physics, 2007.

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International, Conference on Spectral Line Shapes (15th 2000 Berlin Germany). Spectral line shapes: 15th ICSLS, Berlin, Germany, 10-14 July 2000. American Institute of Physics, 2001.

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Części książek na temat "Spectral line formation Congresses"

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Maciel, Walter J. "Spectral Line Formation." In Astrophysics of the Interstellar Medium. Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4614-3767-3_3.

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Hack, M. "Observational Problems in Spectral Line Formation." In Progress in Stellar Spectral Line Formation Theory. Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5372-7_22.

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Jaeglé, P., G. Jamelot, and A. Carillon. "Line Formation in Laboratory Plasmas." In Progress in Stellar Spectral Line Formation Theory. Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5372-7_21.

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Nordlund, Å. "NLTE Spectral Line Formation in Three Dimensions." In Stellar Atmospheres: Beyond Classical Models. Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3554-2_7.

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Oxenius, J. "Kinetic Aspects of Redistribution in Spectral Lines." In Progress in Stellar Spectral Line Formation Theory. Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5372-7_3.

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Beckman, John E. "A Review of Line Formation in Molecular Clouds." In Progress in Stellar Spectral Line Formation Theory. Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5372-7_32.

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Kunasz, P. B. "The Theory of Line Transfer in Expanding Atmospheres." In Progress in Stellar Spectral Line Formation Theory. Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5372-7_25.

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Ferrero, R. Freire. "Some Comments Upon the Line Emission Profile Ψν." In Progress in Stellar Spectral Line Formation Theory. Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5372-7_6.

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Linsky, Jeffrey L. "Observed and Computed Stellar Line Profiles: The Roles Played by Partial Redistribution, Geometrical Extent and Expansion." In Progress in Stellar Spectral Line Formation Theory. Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5372-7_1.

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Heinzel, Petr, and Ivan Hubený. "Partial Redistribution Interlocking in the Solar Chromosphere." In Progress in Stellar Spectral Line Formation Theory. Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5372-7_10.

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Streszczenia konferencji na temat "Spectral line formation Congresses"

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Dulieu, Olivier. "Ultracold Molecules: Formation, Detection." In SPECTRAL LINE SHAPES. AIP, 2002. http://dx.doi.org/10.1063/1.1525491.

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Pichler, Goran. "Formation and Detection of Ultracold Molecules." In SPECTRAL LINE SHAPES. AIP, 2002. http://dx.doi.org/10.1063/1.1525490.

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Yurovsky, V. A. "Formation of a molecular Bose-Einstein condensate and an entangled atomic gas by time-dependent Feshbach resonance." In SPECTRAL LINE SHAPES. AIP, 2002. http://dx.doi.org/10.1063/1.1525489.

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Rosato, J., John Lewis, and Adriana Predoi-Cross. "Modeling of Coherence Effects on Spectral Line Formation Using the Quantum Phase Space Formalism." In 20TH INTERNATIONAL CONFERENCE ON SPECTRAL LINE SHAPES. AIP, 2010. http://dx.doi.org/10.1063/1.3517586.

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Kuzmanovska, Olgica. "Numerical methods for solution of spectral line formation problems in the stellar atmospheres." In 10th Jubilee International Conference of the Balkan Physical Union. Author(s), 2019. http://dx.doi.org/10.1063/1.5091215.

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Kewley, L. J. "Emission Line Diagnostics of Star Formation: Nearby and at High Redshift." In THE SPECTRAL ENERGY DISTRIBUTIONS OF GAS-RICH GALAXIES: Confronting Models with Data; International Workshop. AIP, 2005. http://dx.doi.org/10.1063/1.1913915.

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Luz, A. M. G., D. Balint, and K. Nikbin. "A Multiscale NDT System for Damage Detection in Thermal Barrier Coatings." In ASME 2009 International Mechanical Engineering Congress and Exposition. ASMEDC, 2009. http://dx.doi.org/10.1115/imece2009-10694.

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Progress in aero-engines and land-based gas turbines is continuously linked with a rise of the operating temperature. TBCs are multilayered structures which function together to effectively lower the temperature of its load-bearing superalloy substrate while simultaneously providing oxidation protection against high temperature combustion environments during operation. They typically comprise of a ceramic top coat for thermal insulation and a metallic bond coat that provides oxidation/corrosion resistance and enhances the adhesion of the YSZ to the superalloy substrate. Due to high-temperature
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Hayes, John M., Wook Hyun Kim, and Gerald J. Small. "Spectral Hole Burning In Hyperquenched Films." In Spectral Hole-Burning and Luminescence Line Narrowing: Science and Applications. Optica Publishing Group, 1992. http://dx.doi.org/10.1364/shbl.1992.tub9.

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An apparatus for the deposition of doped, thin, amorphous films has been developed. This apparatus is based on the hyperquenching technique of Mayer (1). In this technique aqueous aerosol, i.e. water clusters, is expanded through an orifice and deposited onto a cryoplate. In Mayer’s work the aerosol was produced by an ultrasonic nebulizer and transferred with a carrier gas through an aperture and then onto the cryoplate. In our apparatus the aerosol is formed and deposited from a thermospray nozzle source (2). Use of the thermospray nozzle permits formation of films uncontaminated by condensat
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Horie, Kazuyuki, Norio Murase, and Makoto Ikemoto. "Wavelength Dependence of Photochemical Hole-Burning Efficiency and Vibronic Structure in an Absorption Band." In Spectral Hole-Burning and Luminescence Line Narrowing: Science and Applications. Optica Publishing Group, 1992. http://dx.doi.org/10.1364/shbl.1992.fa2.

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Photochemical hole-burning(PHB) is a good tool for understanding the dynamics of host polymers as well as for realizing a high performance optical storage. The quantum efficiency for persistent hole formation, ϕ, is one of the essential parameters for the PHB phenomenon. If one is aware of some kinds of application, its value is preferable to be large. This is why the quantum efficiencies for several series of substances are measured and the efforts to find out the dominant factor for controlling these values are continued.1) As ever, these values are measured near the peaks of the lowest ener
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Horie, Kazuyuki. "New Mechanisms and New Systems of Hole Formation in Spectral Hole Burning." In Spectral Hole-Burning and Related Spectroscopies: Science and Applications. Optica Publishing Group, 1994. http://dx.doi.org/10.1364/shbs.1994.thf1.

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A variety of studies on persistent spectral hole burning (PSHB) have been carried out for the last twenty years [1-4], since the discovery of this phenomenon in 1974. The elucidation of electron-phonon interaction, the nature of a zero-phonon line and spectral diffusion in PSHB have been studied intensively together with the research aiming at its possible applicability to ultra-high density optical storage. However, as for the PSHB materials, most of the works have been carried out with porphyrins, phthalocyanines, and quinizarin including their derivatives, several organic dyes, samarium and
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Raporty organizacyjne na temat "Spectral line formation Congresses"

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Heinola, Kalle. Atomic Data for Vapour Shielding in Fusion Devices. IAEA Nuclear Data Section, 2019. http://dx.doi.org/10.61092/iaea.zzjz-hsb9.

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The First Research Coordination Meeting of the Coordinated Research Project on Atomic Data for Vapour Shielding in Fusion Devices was held at the IAEA Headquarters in Vienna on 13 – 15 March 2019. Nine experts representing nine research institutes globally (Australia, China, India, Italy, Netherlands, North Macedonia, Spain, Syria, USA) in the field of atomic collisional physics and vapour formation for magnetic confinement fusion devices met together with the IAEA staff. The participants were theorists and modellers of plasma and vapour particle collisional processes, experimentalists of spec
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Heinola, K. Summary Report of the Second Research Coordination Meeting on Atomic Data for Vapour Shielding in Fusion Devices. IAEA Nuclear Data Section, 2021. http://dx.doi.org/10.61092/iaea.gd9j-0nr6.

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The Second Research Coordination Meeting of the Coordinated Research Project on Atomic Data for Vapour Shielding in Fusion Devices was held as a virtual meeting on 7 – 9 October 2020. Eight experts representing eight research institutes globally (Australia, China, India, Netherlands, Spain, Syria, USA) in the field of atomic collisional physics and vapour formation for magnetic confinement fusion devices met together with the IAEA staff. Participants were theorists and modellers of plasma and vapour par-ticle collisional processes, experimentalists of spectral line properties, and vapour forma
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