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Relevant bibliographies by topics / Maximum Luminosity

Academic literature on the topic 'Maximum Luminosity'

Author: Grafiati

Published: 10 December 2022

Last updated: 29 January 2023

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Journal articles on the topic "Maximum Luminosity"

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Lu, Wenbin, and Pawan Kumar. "The maximum luminosity of fast radio bursts." Monthly Notices of the Royal Astronomical Society: Letters 483, no. 1 (October 23, 2018): L93—L97. http://dx.doi.org/10.1093/mnrasl/sly200.

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Füllekrug, Martin, Stanislaus Nnadih, Serge Soula, Janusz Mlynarczyk, Micheal Stock, Jeff Lapierre, and Michael Kosch. "Maximum Sprite Streamer Luminosity Near the Stratopause." Geophysical Research Letters 46, no. 21 (November 11, 2019): 12572–79. http://dx.doi.org/10.1029/2019gl084331.

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Kanbur, S. M., M. A. Hendry, and D. Clarke. "Period-luminosity and period-luminosity-colour relations for Mira variables at maximum light." Monthly Notices of the Royal Astronomical Society 289, no. 2 (August 1, 1997): 428–42. http://dx.doi.org/10.1093/mnras/289.2.428.

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Andrei, Alexandre, Bruno Coelho, Leandro L. S. Guedes, and Alexandre Lyra. "The luminosity function of quasars by the Principle of Maximum Entropy." Monthly Notices of the Royal Astronomical Society 488, no. 1 (June 21, 2019): 183–90. http://dx.doi.org/10.1093/mnras/stz1627.

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ABSTRACT We propose a different way to obtain the distribution of the luminosity function of quasars by using the Principle of Maximum Entropy. The input data come from Richard et al 2006 quasar counts, extending up to redshift 5 and limited from apparent magnitude i = 15–19.1 at z ≲ 3 to i = 20.2 for z ≳ 3. Using only few initial data points, the principle allows us to estimate probabilities and hence that luminosity curve. We carry out statistical tests to evaluate our results. The resulting luminosity function compares well to earlier determinations, and our results remain consistent either when the amount or choice of sampled sources is unbiasedly altered. Besides this, we estimate the distribution of the luminosity function for redshifts in which there is only observational data in the vicinity.

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Dexter, A. C., G. Burt, P. K. Ambattu, V. Dolgashev, and R. Jones. "CLIC crab cavity design optimisation for maximum luminosity." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 657, no. 1 (November 2011): 45–51. http://dx.doi.org/10.1016/j.nima.2011.05.057.

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Luri, X., M. O. Mennessier, J. Torra, and F. Figueras. "A new maximum likelihood method for luminosity calibrations." Astronomy and Astrophysics Supplement Series 117, no. 2 (June 1996): 405–15. http://dx.doi.org/10.1051/aas:1996165.

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Vardanyan, Valeri, Daniel Weedman, and Lusine Sargsyan. "SEEKING THE EPOCH OF MAXIMUM LUMINOSITY FOR DUSTY QUASARS." Astrophysical Journal 790, no. 2 (July 8, 2014): 88. http://dx.doi.org/10.1088/0004-637x/790/2/88.

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Veshcherevich, V. G., V. A. Lebedev, P. V. Logachev, and V. P. Yakovlev. "Monochromatization as the way to maximum luminosity B-factories." Nuclear Physics B - Proceedings Supplements 27 (June 1992): 12–26. http://dx.doi.org/10.1016/0920-5632(92)90028-q.

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Mummery, Andrew. "A maximum X-ray luminosity scale of disc-dominated tidal destruction events." Monthly Notices of the Royal Astronomical Society 504, no. 4 (April 26, 2021): 5144–54. http://dx.doi.org/10.1093/mnras/stab1187.

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ABSTRACT We develop a model describing the dynamical and observed properties of disc-dominated tidal disruption events (TDEs) around black holes with the lowest masses (M ≲ few × 106M⊙). TDEs around black holes with the lowest masses are most likely to reach super-Eddington luminosities at early times in their evolution. By assuming that the amount of stellar debris that can form into a compact accretion disc is set dynamically by the Eddington luminosity, we make a number of interesting and testable predictions about the observed properties of bright soft-state X-ray TDEs and optically bright, X-ray dim TDEs. We argue that TDEs around black holes of the lowest masses will expel the vast majority of their gravitationally bound debris into a radiatively driven outflow. A large-mass outflow will obscure the innermost X-ray producing regions, leading to a population of low black hole mass TDEs that are only observed at optical and UV energies. TDE discs evolving with bolometric luminosities comparable to their Eddington luminosity will have near constant (i.e. black hole mass independent) X-ray luminosities, of order LX, max ≡ LM ∼ 1043 − 1044 erg s−1. The range of luminosity values stems primarily from the range of allowed black hole spins. A similar X-ray luminosity limit exists for X-ray TDEs in the hard (Compton scattering dominated) state, and we therefore predict that the X-ray luminosity of the brightest X-ray TDEs will be at the scale LM(a) ∼ 1043 − 1044 erg s−1, independent of black hole mass and accretion state. These predictions are in strong agreement with the properties of the existing population (∼40 sources) of observed TDEs.

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Gieles, M., S. S. Larsen, N. Bastian, and I. T. Stein. "The luminosity function of young star clusters: implications for the maximum mass and luminosity of clusters." Astronomy & Astrophysics 450, no. 1 (April 2006): 129–45. http://dx.doi.org/10.1051/0004-6361:20053589.

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Book chapters on the topic "Maximum Luminosity"

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García-Dabó, C. E., and J. Gallego. "Major Improvements to Estimate Luminosity Functions Using Maximum Likelihood Methods." In Highlights of Spanish Astrophysics III, 79–82. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-1778-6_17.

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Hekker, S., G. C. Angelou, Y. Elsworth, and S. Basu. "The Physical Origin of the Luminosity Maximum of the RGB-Bump." In Astrophysics and Space Science Proceedings, 273–75. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-55336-4_37.

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Masana, E., C. Jordi, and X. Luri. "Luminosity and Kinematic Calibration of FGK Stars Using a Maximum Likelihood Method." In Highlights of Spanish Astrophysics II, 217–20. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-017-1776-2_51.

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Kanbur, S. M., and S. Nikolaev. "An Estimate of H0 Using Cepheid Period Luminosity Relations at Maximum Light." In New Quests in Stellar Astrophysics: The Link Between Stars and Cosmology, 143–46. Dordrecht: Springer Netherlands, 2002. http://dx.doi.org/10.1007/978-94-010-0393-3_28.

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Luri, X., M. O. Mennessier, F. Figueras, J. Torra, and A. E. Gómez. "Luminosity and Kinematics: A Maximum Likelihood Algorithm for Exploitation of the Hipparcos Data." In Statistical Challenges in Modern Astronomy II, 433–35. New York, NY: Springer New York, 1997. http://dx.doi.org/10.1007/978-1-4612-1968-2_39.

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Ifeoma Onah, Costecia, Augustine A. Ubachukwu, and Finbarr C. Odo. "Evolution of Radio Source Components and the Quasar/Galaxy Unification Scheme." In Astronomy [Working Title]. IntechOpen, 2022. http://dx.doi.org/10.5772/intechopen.106244.

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In this work, a theoretical model is developed for explanation of temporal evolution of extragalactic radio sources via beaming, orientation effects and asymmetries. Equation of the form D≈P±q1+z−m is used to account for the D ∼ P/z relation. Also, D≈D01+z−1+z1+z2 accounted properly for Ω0=1 cosmology than the Ω0=0 counterpart in linear size versus redshift of radio sources. Similarly, D=Dc1∓lnPPc1/2 model explained redshift-luminosity relationship of extragalactic radio sources. The results from the regression analyses are q = +0.003 (r = 0.04) for sources with z < 1 and q = −1.59 (r = −0.6) for all z≥1 sources. A critical linear size, Dc of 316kpc which matches the maximum theoretical linear size, Dmax of 0.15D0 at a critical redshift zc∼1 and a critical luminosity Pc=26.33WHz−1 are obtained. The indication of all these results is that the linear size of radio sources evolves up to a certain limit in D–P plane and thereafter decreases with increasing luminosity as predicted in this work.

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Conference papers on the topic "Maximum Luminosity"

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Petreus, Dorin, Daniel Moga, Adina Rusu, Toma Patarau, and Stefan Daraban. "A Maximum Power Point tracker for a photovoltaic system under changing luminosity conditions." In 2010 IEEE International Symposium on Industrial Electronics (ISIE 2010). IEEE, 2010. http://dx.doi.org/10.1109/isie.2010.5637829.

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Ermash, A. A., S. V. Pilipenko, E. V. Mikheeva, and V. N. Lukash. "Contribution to the confusion noise from various sources." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.145.

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The maximum possible depth of future far infrared and submillimetre telescopes will be limited by the confusion noise. Herewe use the deﬁnition of the confusion noise as the width of the left side of the pixel histogram. In this paper we investigatethe inﬂuence of the large-scale structure of the Universe and gravitational lensing on the confusion noise estimates. We alsoestimate the redshift and luminosity intervals of objects that give maximum contribution. The dependence on the diameterof the main mirror is also discussed.

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Andreev, V., A. Belova, A. Galoyan, S. Gerassimov, G. Golovanov, P. Goncharov, A. Gribowsky, et al. "OFFLINE SOFTWARE AND COMPUTING FOR THE SPD EXPERIMENT." In 9th International Conference "Distributed Computing and Grid Technologies in Science and Education". Crossref, 2021. http://dx.doi.org/10.54546/mlit.2021.80.69.001.

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The SPD (Spin Physics Detector) is a planned spin physics experiment in the second interaction pointof the NICA collider that is under construction at JINR. The main goal of the experiment is the test ofbasic of the QCD via the study of the polarized structure of the nucleon and spin-related phenomena inthe collision of longitudinally and transversely polarized protons and deuterons at the center-of-massenergy up to 27 GeV and luminosity up to 1032 1/(cm2 s). The data rate at the maximum designluminosity is expected to reach 0.2 Tbit/s. Current approaches to SPD computing and offline softwarewill be presented. The plan of the computing and software R&D in the scope of the SPD TDRpreparation will be discussed.

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Gatti, M., R. Gaudron, C. Mirat, L. Zimmer, and T. Schuller. "A Comparison of the Transfer Functions and Flow Fields of Flames With Increasing Swirl Number." In ASME Turbo Expo 2018: Turbomachinery Technical Conference and Exposition. American Society of Mechanical Engineers, 2018. http://dx.doi.org/10.1115/gt2018-76105.

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The frequency response of premixed swirled flames is investigated by comparing their Transfer Function (FTF) between velocity and heat release rate fluctuations. The equivalence ratio and flow velocity are kept constant and four different swirling injectors are tested with increasing swirl numbers. The first injector features a vanishing low swirl number S = 0.20 and produces a flame anchored by the recirculating flow in the wake of a central bluff body. The three other swirling injectors produce highly swirled flows (S > 0.6) leading to a much larger internal recirculation region, which size increases with the swirl level. When operating the burner at S = 0.20, the FTF gain curve smoothly increases to reach a maximum and then smoothly decreases towards zero. For the highly swirled flames (S > 0.6), the FTF gain curve shows a succession of valleys and peaks attributed to interferences between axial and azimuthal velocity fluctuations at the injector outlet. The FTF phase-lag curves from the vanishing low and highly swirled flames are the same at low frequencies despite their large differences in flame length and flame aspect ratio. Deviations between the FTF phase lag curves of the different swirled flames start above the frequency corresponding to the first valley in the FTF gain of the highly swirled flames. Phase averaged images of the axial flow fields and of the flame chemiluminescence are used to interpret these features. At forcing frequencies corresponding to peak FTF gain values, the cold flow response of all flames investigated is dominated by large coherent vortical structures shed from the injector lip. At forcing frequencies corresponding to a valley in the FTF gain curve of the highly swirled flames, the formation of large coherent structures is strongly hindered in the cold flow response. These observations contrast with previous interpretations of the mechanisms associated to the low FTF response of swirled flames. It is finally found that for flames stabilized with a large swirl number, heat release rate fluctuations result both from large flame luminosity oscillations and large flame volume oscillations. For conditions leading to a small FTF gain value, both the flame luminosity and flame volume fluctuations are suppressed confirming the absence of strong perturbations within the flow at these frequencies. The experiments made in this work reveal a purely hydrodynamic mechanism at the origin of the low response of swirling flames at certain specific frequencies.

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Ishino, Yojiro, Naoki Hayashi, Yuta Ishiko, Ahmad Zaid Nazari, Kimihiro Nagase, Kazuma Kakimoto, and Yu Saiki. "Schlieren 3D-CT Reconstruction of Instantaneous Density Distributions of Spark-Ignited Flame Kernels of Fuel-Rich Propane-Air Premixture." In ASME 2016 Heat Transfer Summer Conference collocated with the ASME 2016 Fluids Engineering Division Summer Meeting and the ASME 2016 14th International Conference on Nanochannels, Microchannels, and Minichannels. American Society of Mechanical Engineers, 2016. http://dx.doi.org/10.1115/ht2016-7423.

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For 3D observation of high speed flames, non-scanning 3D-CT technique using a multi-directional quantitative schlieren system with flash light source, is proposed for instantaneous density distribution of unsteady premixed flames. This “Schlieren 3D-CT” is based on (i) simultaneous acquisition of flash-light schlieren images taken from numerous directions, and (ii) 3D-CT reconstruction of the images by an appropriate CT algorithm. In this technique, for simultaneous schlieren photography, the custom-made 20-directional schlieren camera has been constructed and used. This camera consists of 20 optical systems of single-directional quantitative schlieren system. Each system is composed of two convex achromatic lenses of 50 mm in diameter and 300 mm in focal length, a light source unit, a schlieren stop of a vertical knife edge and a digital camera. The light unit has a flash (9 micro-sec duration) light source of a uniform luminance rectangular area of 1 mm × 1 mm. Both of the uniformity of the luminosity and the definite shape are essential for a quantitative schlieren observation. Sensitivity of the digital cameras are calibrated with a stepped neutral density filter. Target flames are located at the center of the camera. The image set of 20 directional schlieren images are processed as follows. First the schlieren picture brightness is shifted by no-flame-schlieren picture brightness in order to obtain the real schlieren brightness images. Second, brightness of these images is scaled by Gladstone-Dale constant of air. Finally, the scaled brightness is horizontally integrated to form “density thickness images”, which can be used for CT reconstruction of density distribution. The density thickness images are used for CT reconstruction by MLEM (maximum likelihood-expectation maximization) CT-algorithm to obtain the 3D reconstruction of instantaneous density distribution. In this investigation, the “density thickness” projection images of 400(H) × 500(V) pixel (32.0 mm × 40.0 mm) are used for 3D-CT reconstruction to produce 3D data of 400(x) × 400(y) × 500(z) pixel (32.0 mm × 32.0 mm × 40.0 mm). The voxel size is 0.08 mm each direction. In this investigation, the target flame is spark-ignited flame kernels. The flame kernels are made by spark ignition for a fuel-rich propane-air premixed gas. First, laminar flow is selected as the premixed gas flow to establish the spherically expanding laminar flame. The CT reconstruction result show the spherical shape of flame kernel with a pair of deep wrinkles. The wrinkle is considered to be caused by spark electrodes. Next turbulent flows behind turbulence promoting grid is selected. The corrugated shape flame kernel is obtained. The schlieren 3D-CT measurements are made for the complicated kernels. CT results expresses the instantaneous 3D turbulent flame kernel shapes.

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Kopylova, F., and A. Kopylov. "Study of groups/clusters of galaxies with the SDSS." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.148.

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For a large sample of groups/clusters of galaxies (N =185), we obtained the scaling relations among of their photometricaland dynamical parameters. We ﬁnd:0.77±0.011. that in the virialized regions of the galaxy systems the total luminosity increase with mass L K ∝ M 200(M K <−21. m 0);2. that the new halo boundary of the galaxy systems corresponds to the splashback radius R sp . These radius is deﬁnedby the observed intergrated distribution of the number of galaxies as a function of the angular distance from thegroup/cluster center squared;3. that the fraction of galaxies with quenched star formation is maximal in the central regions of the galaxy systems,and it decreases to the radius R sp , but remains higher than in the ﬁeld on ∼ 27%.

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