Academic literature on the topic 'AlMn Binary Alloy'
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Journal articles on the topic "AlMn Binary Alloy"
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Snitovsky, Yuri P. "Changes in the physical and mechanical properties of aluminum depending on the composition of the alloying elements." Yugra State University Bulletin 18, no. 4 (January 14, 2023): 68–76. http://dx.doi.org/10.18822/byusu20220468-76.
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Subject of research: the influence of the concentration and composition of alloying elements Mn, Ti, Cr, Y, Mo, W, V on the change in the aluminum recrystallization temperature.
Purpose of research: to find the optimal concentration of alloying additives, at which the recrystallization temperature reaches its maximum value.
Methods and objects of research: using the methods of thermodynamic analysis of binary state diagrams of aluminum with alloying additives, it has been established that the nature of the change in the recrystallization temperature depends on what type of eutectic or peritectic reaction the formation of intermetallic compounds belongs to. It is shown that aluminides act as alloy modifiers and impart high mechanical properties to products.
Main results of research: it was found that for the AlMn system, the optimal content of Mn should be considered 0.2%, for the AlCr system, the maximum increase in the Al recrystallization temperature is observed at 0.6% Cr, for the AlY system, the mechanical properties of Al at elevated temperatures maximum at 1% Y.
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Mollaamin, Fatemeh. "Increasing corrosion resistance of binary Al-Alloy through implanting with some transition elements and heteroatom organic compounds." Acta Chimica Asiana 6, no. 2 (June 23, 2023): 328–42. http://dx.doi.org/10.29303/aca.v6i2.166.
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Decorating of Transition metals (TMs) on the "AlMg" nanoalloy has been studied on the basis of Langmuir adsorption applying "ONIOM" model with three levels of «high, medium and low» by using "LANL2DZ /6-31+G(d,p)/EPR-III", "semi-empirical" and "MM2" functions. The fluctuation of "NQR" has estimated the inhibiting role of pyridine and alkylpyridines containing 2-picoline (2Pic), 3-picoline (3Pic) ,4-picoline (4Pic), and 2,4-lutidine (24Lut) for (Sc, Ti, Cr, Ni, Cu, Zn)-doped AlMg alloy nanosheet due to "N" atom in the benzene cycle of heterocyclic carbenes being near the monolayer surface of ternary "TM–(Al–Mg)" (TM= Sc, Ti, Cr, Ni, Cu, Zn) nanoalloys. The "NMR" spectroscopy has remarked In fact, the NMR results of the adsorption of pyridine and alkylpyridines of 2Pic, 3Pic, 4Pic and 24Lut molecules represent spin polarization on the TM (Sc, Ti, Cr, Ni, Cu, Zn)-doped Al–Mg nanoalloy surfaces that these surfaces can be employed as the magnetic N-heterocyclic carbene sensors. In fact, "TM" sites in "TM–(Al–Mg)" nanoalloy surfaces have bigger interaction energy amount from "Van der Waals’ forces" with pyridine and its nitrogen heterocyclic family that might cause them large stable towards coating data on the nanosurface. It has been estimated that the criterion for choosing the surface linkage of "N" atom in pyridine and alkylpyridines in adsorption sites can be impacted by the existence of close atoms of aluminum and magnesium in the "TM–(AlMg)" surfaces. Moreover, "IR" spectroscopy has exhibited that (Sc, Ti, Cr, Ni, Cu, Zn)-doped AlMg alloy nanosheet with the fluctuation in the frequency of intra-atomic interaction leads us to the most considerable influence in the vicinage elements generated due to inter-atomic interaction. Comparison to amounts versus dipole moment has illustrated a proper accord among measured parameters based on the rightness of the chosen isotherm for the adsorption steps of the formation of Py@Sc–(Al–Mg), Py@Ti–(Al–Mg), Py@Cr–(Al–Mg), Py@Ni–(Al–Mg), Py@Cu–(Al–Mg), and Py@Zn–(Al–Mg) complexes. Thus, the interval between nitrogen atom in pyridine during interaction with transition metals of "Sc, Ti, Cr, Ni, Cu, Zn" in "TM–(Al–Mg)" nanoalloys, (N→TM), has been estimated with relation coefficient of R² = 0.9284. Thus, the present has exhibit the influence of "TMs" doped on the "Al–Mg" surface for adsorption of N-heterocyclic carbenes of pyridine and alkylpyridines by using theoretical methods.
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Kowalski, W., B. Grushko, Włodzimierz Bogdanowicz, and M. Surowiec. "Complex Intermetallics in the Al-Rich Part of Al-Pd-Cr System." Solid State Phenomena 163 (June 2010): 272–77. http://dx.doi.org/10.4028/www.scientific.net/ssp.163.272.
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The Al-Pd-Cr alloy system was investigated at 680 to 990°C in the compositional range above 60 at.% Al. The binary Al-Cr , μ and phases dissolves up to 1 at.% of Al, the η-phase extends up to 2 at.% of Pd and the 2-phase extends up to 3 at.% of Pd, respectively. The binary Al-Pd -phases dissolves up to 3 at.% of Cr and -phase up to 4 at.% Cr. Close to the high-Pd limit of the -range a ternary phase is formed between about Al78Pd4Cr18, Al77Pd10Cr13 and Al74Pd7Cr19. Its structure is orthorhombic with lattice parameters: a = 1.47, b = 1.24 and c = 1.25 nm, resembling the lattice parameters of the high-temperature Al3Mn phase. A hexagonal structure with a = 1.77 and c = 1.25 nm resembling Al-Ni(Cu)-Cr ζ-phase [1-3] was revealed around Al81.5Pd1.5Cr27 and another hexagonal structure with very close lattice parameters around Al73Pd11Cr16. Another ternary phase was found in 970°C around the Al77.5Pd1.5Cr21 composition. It has orthorhombic structure with a = 1.24, b = 3.46 and c = 2.04 nm resembling the ternary -phase in Al-Ni-Cr. An additional orthorhombic phase with a = 2.48, b= 3.87 and c = 2.04 nm was found to be formed between about Al82Pd4Cr14, Al79Pd4Cr17 and Al79Pd9Cr12.
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Wang, Tian, Dmytro Kevorkov, Ahmad Mostafa, and Mamoun Medraj. "Experimental Investigation of the Phase Equilibria in the Al-Mn-Zn System at 400°C." Journal of Materials 2014 (July 17, 2014): 1–13. http://dx.doi.org/10.1155/2014/451587.
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Al-Mn-Zn ternary system is experimentally investigated at 400°C using diffusion couples and key alloys. Phase relationships and homogeneity ranges are determined for binary and ternary compounds using EPMA, SEM/EDS, and XRD. Reported ternary compound T3 (Al11Mn3Zn2) is confirmed in this study and is denoted as τ2 in this paper. Two new ternary compounds (τ1 and τ3) are observed in this system at 400°C. τ1 is determined as a stoichiometric compound with the composition of Al31Mn8Zn11. τ3 has been found to have homogeneity range of AlxMnyZnz (x=9–13 at%; y=11–15 at%; z=75–77 at%). The binary compounds Al4Mn and Al11Mn4 exhibit limited solid solubility of around 6 at% and 4 at% Zn, respectively. Terminal solid solution Al8Mn5 is found to have maximum ternary solubility of about 10 at% Zn. In addition, ternary solubility of Al-rich β-Mn′ at 400°C is determined as 4 at% Zn. Zn-rich β-Mn′′ has a ternary solubility of 3 at% Al. The solubility of Al in Mn5Zn21 is measured as 5 at%. Based on the current experimental results, the isothermal section of Al-Mn-Zn ternary system at 400°C has been constructed.
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Gallardo Cava, Iván, Valentín Bujarrabal, Javier Alcolea, Miguel Gómez-Garrido, Arancha Castro-Carrizo, Hans Van Winckel, and Miguel Santander-García. "Rotating and Expanding Gas in Binary Post-AGB Stars." Astronomy 1, no. 2 (August 2, 2022): 84–92. http://dx.doi.org/10.3390/astronomy1020008.
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There is a class of binary post-AGB stars (binary system including a post-AGB star) that are surrounded by Keplerian disks and outflows resulting from gas escaping from the disk. To date, there are seven sources that have been studied in detail through interferometric millimeter-wave maps of CO lines (ALMA/NOEMA). For the cases of the Red Rectangle, IW Carinae, IRAS 08544-4431, and AC Herculis, it is found that around ≥85% of the total nebular mass is located in the disk with Keplerian dynamics. The remainder of the nebular mass is located in an expanding component. This outflow is probably a disk wind consisting of material escaping from the rotating disk. These sources are the disk-dominated nebulae. On the contrary, our maps and modeling of 89 Herculis, IRAS 19125+0343, and R Scuti, which allowed us to study their morphology, kinematics, and mass distribution, suggest that, in these sources, the outflow clearly is the dominant component of the nebula (∼75% of the total nebular mass), resulting in a new subclass of nebulae around binary post-AGB stars: the outflow-dominated sources.Besides CO, the chemistry of this type of source has been practically unknown thus far. We also present a very deep single-dish radio molecular survey in the 1.3, 2, 3, 7, and 13 mm bands (∼600 h of telescope time). Our results and detections allow us to classify our sources as O- or /C-rich. We also conclude that the calculated abundances of the detected molecular species other than CO are particularly low, compared with AGB stars. This fact is very significant in those sources where the rotating disk is the dominant component of the nebula.
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Graver, Brit, Antonius van Helvoort, John Charles Walmsley, and Kemal Nisancioglu. "Surface Segregation of Indium by Heat Treatment of Aluminium." Materials Science Forum 519-521 (July 2006): 673–78. http://dx.doi.org/10.4028/www.scientific.net/msf.519-521.673.
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High temperature heat treatment of aluminium alloys causes surface enrichment of the trace elements in Group IIIA - VA, specifically the low melting point elements Pb, Bi, In and Sn. The phenomenon has practical significance in promoting certain types of localised corrosion, such as galvanic and filiform corrosion, while mitigating other types, such as pitting corrosion of the bare surface. The purpose of this paper is to investigate the surface enrichment and microstructure of indium relative to the available data for Pb. Model binary AlIn alloys, containing 20-1000 ppm of In, were used after heat treatment at various temperatures. In addition to electrochemical investigations, the microstructures were characterised by field emission scanning electron microscopy (FEG SEM) and field emission transmission electron microscopy (FEG TEM). Heat treatment at temperatures as low as 300°C gave significant segregation of In as opposed to 600°C for Pb. As a result of this and yet unresolved oxide film breakdown mechanism on aluminium, In was significantly more effective than Pb in anodically activating aluminium. These results suggest the possibility that significant activation earlier observed on certain commercial alloys as a result of low temperature heat treatment may be due to the trace elements In.
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Martinez–Brunner, Rafael, Simon Casassus, Sebastián Pérez, Antonio Hales, Philipp Weber, Miguel Cárcamo, Carla Arce-Tord, et al. "High-resolution ALMA observations of V4046 Sgr: a circumbinary disc with a thin ring." Monthly Notices of the Royal Astronomical Society 510, no. 1 (November 27, 2021): 1248–57. http://dx.doi.org/10.1093/mnras/stab3440.
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ABSTRACT The nearby V4046 Sgr spectroscopic binary hosts a gas-rich disc known for its wide cavity and dusty ring. We present high resolution (∼20 mas or 1.4 au) ALMA observations of the 1.3 mm continuum of V4046 Sgr which, combined with SPHERE–IRDIS polarised images and a well-sampled spectral energy distribution (SED), allow us to propose a physical model using radiative transfer predictions. The ALMA data reveal a thin ring at a radius of 13.15 ± 0.42 au (Ring13), with a radial width of 2.46 ± 0.56 au. Ring13 is surrounded by a ∼10 au-wide gap, and it is flanked by a mm-bright outer ring (Ring24) with a sharp inner edge at 24 au. Between 25 and ∼35 au the brightness of Ring24 is relatively flat and then breaks into a steep tail that reaches out to ∼60 au. In addition, central emission is detected close to the star which we interpret as a tight circumbinary ring made of dust grains with a lower size limit of 0.8 mm at 1.1 au. In order to reproduce the SED, the model also requires an inner ring at ∼5 au (Ring5) composed mainly of small dust grains, hiding under the IRDIS coronagraph, and surrounding the inner circumbinary disc. The surprisingly thin Ring13 is nonetheless roughly 10 times wider than its expected vertical extent. The strong near-far disc asymmetry at 1.65 $\rm{\mu m}$ points at a very forward-scattering phase function, and requires grain radii of no less than 0.4 $\rm{\mu m}$.
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Guélin, M., N. A. Patel, M. Bremer, J. Cernicharo, A. Castro-Carrizo, J. Pety, J. P. Fonfría, et al. "IRC +10 216 in 3D: morphology of a TP-AGB star envelope." Astronomy & Astrophysics 610 (February 2018): A4. http://dx.doi.org/10.1051/0004-6361/201731619.
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During their late pulsating phase, AGB stars expel most of their mass in the form of massive dusty envelopes, an event that largely controls the composition of interstellar matter. The envelopes, however, are distant and opaque to visible and NIR radiation: their structure remains poorly known and the mass-loss process poorly understood. Millimeter-wave interferometry, which combines the advantages of longer wavelength, high angular resolution and very high spectral resolution is the optimal investigative tool for this purpose. Mm waves pass through dust with almost no attenuation. Their spectrum is rich in molecular lines and hosts the fundamental lines of the ubiquitous CO molecule, allowing a tomographic reconstruction of the envelope structure. The circumstellar envelope IRC +10 216 and its central star, the C-rich TP-AGB star closest to the Sun, are the best objects for such an investigation. Two years ago, we reported the first detailed study of the CO(2–1) line emission in that envelope, made with the IRAM 30-m telescope. It revealed a series of dense gas shells, expanding at a uniform radial velocity. The limited resolution of the telescope (HPBW 11″) did not allow us to resolve the shell structure. We now report much higher angular resolution observations of CO(2–1), CO(1–0), CN(2–1) and C4H(24–23) made with the SMA, PdB and ALMA interferometers (with synthesized half-power beamwidths of 3″, 1″ and 0.3″, respectively). Although the envelope appears much more intricate at high resolution than with an 11″ beam, its prevailing structure remains a pattern of thin, nearly concentric shells. The average separation between the brightest CO shells is 16″ in the outer envelope, where it appears remarkably constant. Closer to the star (<40″), the shell pattern is denser and less regular, showing intermediary arcs. Outside the small (r< 0.3′′) dust formation zone, the gas appears to expand radially at a constant velocity, 14.5 km s-1, with small turbulent motions. Based on that property, we have reconstructed the 3D structure of the outer envelope and have derived the gas temperature and density radial profiles in the inner (r< 25′′) envelope. The shell-intershell density contrast is found to be typically 3. The over-dense shells have spherical or slightly oblate shapes and typically extend over a few steradians, implying isotropic mass loss. The regular spacing of shells in the outer envelope supports the model of a binary star system with a period of 700 yr and a near face-on elliptical orbit. The companion fly-by triggers enhanced episodes of mass loss near periastron. The densification of the shell pattern observed in the central part of the envelope suggests a more complex scenario for the last few thousand years.
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Gu, Z., J. H. Edgar, E. A. Payzant, H. M. Meyer, L. R. Walker, A. Sarua, and M. Kuball. "Sublimation Growth of Aluminum Nitride-Silicon Carbide Alloy Crystals on SiC (0001) Substrates." MRS Proceedings 831 (2004). http://dx.doi.org/10.1557/proc-831-e3.1.
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ABSTRACTThick (up to 1 mm) AlN-SiC alloy crystals were grown on off-axis Si-face 6H-SiC (0001) substrates by the sublimation-recondensation method from a mixture of AlN and SiC powders at 1860–1990 °C in a N2 atmosphere. The color of the crystals changed from clear to dark green with increasing growth temperature. Raman spectroscopy and x-ray diffraction (XRD) confirmed an AlN-SiC alloy was formed with the wurtzite structure and good homogeneity. Three broad peaks were detected in the Raman spectra, with one of those related to an AlN-like and another one to a SiC-like mode, both shifted relative to their usual positions in the binary compounds, and the third broad peak with possible contributions from both AlN and SiC. Scanning Auger microanalysis (SAM) and electron probe microanalysis (EPMA) demonstrated the alloy crystals had an approximate composition of (AlN)0.75(SiC)0.25 with a stoi chiometric ratio of Al:N and Si:C. The substrate mi sorientati on ensured a two-dimensional growth mode confirmed by scanning electron microscopy (SEM).
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Wood, C. M., J. C. A. Miller-Jones, A. Bahramian, S. J. Tingay, T. D. Russell, A. J. Tetarenko, D. Altamirano, et al. "Time-dependent visibility modelling of a relativistic jet in the X-ray binary MAXI J1803−298." Monthly Notices of the Royal Astronomical Society, March 30, 2023. http://dx.doi.org/10.1093/mnras/stad939.
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Abstract Tracking the motions of transient jets launched by low-mass X-ray binaries (LMXBs) is critical for determining the moment of jet ejection, and identifying any corresponding signatures in the accretion flow. However, these jets are often highly variable and can travel across the resolution element of an image within a single observation, violating a fundamental assumption of aperture synthesis. We present a novel approach in which we directly fit a single time-dependent model to the full set of interferometer visibilities, where we explicitly parameterise the motion and flux density variability of the emission components, to minimise the number of free parameters in the fit, while leveraging information from the full observation. This technique allows us to detect and characterize faint, fast-moving sources, for which the standard time binning technique is inadequate. We validate our technique with synthetic observations, before applying it to three Very Long Baseline Array (VLBA) observations of the black hole candidate LMXB MAXI J1803−298 during its 2021 outburst. We measured the proper motion of a discrete jet component to be 1.37 ± 0.14 mas hr−1, and thus we infer an ejection date of MJD $59348.08_{-0.06}^{+0.05}$, which occurs just after the peak of a radio flare observed by the Australia Telescope Compact Array (ATCA) and the Atacama Large Millimeter/Sub-Millimeter Array (ALMA), while MAXI J1803−298 was in the intermediate state. Further development of these new VLBI analysis techniques will lead to more precise measurements of jet ejection dates, which, combined with dense, simultaneous multi-wavelength monitoring, will allow for clearer identification of jet ejection signatures in the accretion flow.
Dissertations / Theses on the topic "AlMn Binary Alloy"
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Meddour, Athmane. "Structure electronique d'alliages metalliques amorphes et quasicristallins : systemes binaires pdy et almn." Paris 6, 1988. http://www.theses.fr/1988PA066696.
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Etude realisee par spectroscopie optique et photoelectronique. Les echantillons sont prepares par pulverisation cathodique sous forme de couches minces. On obtient des echantillons amorphes et quasicristallins par melange ionique a partir de couches multiples. Discussion de l'evolution des spectres optiques des alliages al-mn lorsqu'on passe d'un etat cristallin ordonne a un etat quasi ordonne et enfin a un etat totalement desordonne
Book chapters on the topic "AlMn Binary Alloy"
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Igor, Vurgaftman. "Binary Compound Semiconductors." In Bands and Photons in III-V Semiconductor Quantum Structures, 171–96. Oxford University Press, 2020. http://dx.doi.org/10.1093/oso/9780198767275.003.0006.
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To apply the band structure models discussed in Part I (extended to structures with quantum confinement in Part III and applied to photonic devices in Part IV), a reliable set of input parameters is necessary. The chapter overviews the literature related to these parameters that has appeared since our published reviews. It also recommends specific values for all of them, including the dependence on temperature and alloy composition. If reliable experimental reports are available, they are used preferentially in the recommendations. Otherwise, it falls back to extrapolations from the existing data and theoretical estimates to fill in the gaps. It starts by reviewing and tabulating band parameters for the III–V compound semiconductors GaAs, AlAs, InAs, GaSb, AlSb, InSb, GaP, AlP, InP, GaN, AlN, and InN. The parameters include energy gaps, electron and hole mass parameters, deformation potentials, elastic constants, band offsets, and their temperature dependences.