| 1. |
- Adeyev, V.M., et al.
(författare)
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Features of auger-investigations of ultrathin periodic metallic film structures
- 2006
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Ingår i: Metallofizika i novejsie tehnologii. - 1024-1809. ; 28:2, s. 193-200
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Tidskriftsartikel (refereegranskat)abstract
- In the presented work the applicability of Auger Electron Spectroscopy for studying layered metal film structures Fe/(Au, Cu)/Tb on Si substrate with thickness of layers up to 30 Å was shown. It was ascertained that Fe layer is interacting with Si substrate and as a result Fe-silicide is formed. The thickness of buffer layers aimed to protect Fe layer appeared to be insufficient for complete suppression of silicide formation
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| 2. |
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| 3. |
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| 4. |
- Irani, Ido, et al.
(författare)
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SN 2022oqm-A Ca-rich Explosion of a Compact Progenitor Embedded in C/O Circumstellar Material
- 2024
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Ingår i: Astrophysical Journal. - 0004-637X .- 1538-4357. ; 962:2
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Tidskriftsartikel (refereegranskat)abstract
- We present the discovery and analysis of SN 2022oqm, a Type Ic supernova (SN) detected <1 day after the explosion. The SN rises to a blue and short-lived (2 days) initial peak. Early-time spectral observations of SN 2022oqm show a hot (40,000 K) continuum with high ionization C and O absorption features at velocities of 4000 km s−1, while its photospheric radius expands at 20,000 km s−1, indicating a pre-existing distribution of expanding C/O material. After ∼2.5 days, both the spectrum and light curves evolve into those of a typical SN Ic, with line velocities of ∼10,000 km s−1, in agreement with the evolution of the photospheric radius. The optical light curves reach a second peak at t ≈ 15 days. By t = 60 days, the spectrum of SN 2022oqm becomes nearly nebular, displaying strong Ca ii and [Ca ii] emission with no detectable [O i], marking this event as Ca-rich. The early behavior can be explained by 10−3M⊙ of optically thin circumstellar material (CSM) surrounding either (1) a massive compact progenitor such as a Wolf–Rayet star, (2) a massive stripped progenitor with an extended envelope, or (3) a binary system with a white dwarf. We propose that the early-time light curve is powered by both the interaction of the ejecta with the optically thin CSM and shock cooling (in the massive star scenario). The observations can be explained by CSM that is optically thick to X-ray photons, is optically thick in the lines as seen in the spectra, and is optically thin to visible-light continuum photons that come either from downscattered X-rays or from the shock-heated ejecta. Calculations show that this scenario is self-consistent.
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| 5. |
- Tynkova, A., et al.
(författare)
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Interdiffusion in Au(120 nm)/Ni(70 nm) thin films at the low-temperature annealing in the different atmospheres
- 2013
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Ingår i: Vacuum. - : Elsevier BV. - 0042-207X .- 1879-2715. ; 87, s. 69-74
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Tidskriftsartikel (refereegranskat)abstract
- The development of the interdiffusion processes and the surface morphology changes in thin films of Au(120 nm)/Ni(70 nm) during annealing at 200 degrees C for 20 min in vacuum with different residual atmosphere pressures of 10(-3) and 10(-6) Pa and in an environment of hydrogen at a pressure of 5 x 10(2) Pa have been studied. Secondary ion mass spectrometry, Auger electron spectroscopy, X-ray diffraction, optical microscopy, atomic force microscopy and scanning electron microscopy were used. Surface microdefects that form in the films are related to the local oxidation of nickel and to the stress that arises due to interdiffusion. Defect formation and reactions at the surface are found to be controlling factors in the transport of nickel to the surface and in the observed morphology.
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