Dielectric properties of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msub><mml:mrow><mml:mi mathvariant="normal">TiC</mml:mi></mml:mrow><mml:mrow><mml:mi>x</mml:mi></mml:mrow></mml:msub></mml:mrow></mml:math>,<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msub><mml:mrow><mml:mi mathvariant="normal">TiN</mml:mi></mml:mrow><mml:mrow><mml:mi>x</mml:mi></mml:mrow></mml:msub></mml:mrow></mml:math>,<mml:math xmlns:mml="http://w

Pflüger, J.; Fink, J.; Weber, W.; Bohnen, K.‐P.; Crecelius, G.

doi:10.1103/physrevb.30.1155

Cited by 201 publications

(86 citation statements)

References 45 publications

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“…The bonding states are mainly derived from N 2p, whereas the antibonding states are mainly derived from Ti 3d. The DOS curves for the Ti 14 N 13 cluster are similar to those calculated by Pflüger et al [1].…”

Section: (C) the Square Efjk Of Hcp-ti Insupporting

confidence: 74%

“…The peaks of the energy loss of 24.5 eV in Figs. 5(e) and 6(e) were found to be similar to the energy loss of 24.9 eV due to excitation of plasmon for TiN, reported by Pflüger et al [1].…”

Section: (C) the Square Efjk Of Hcp-ti Insupporting

confidence: 59%

“…Titanium nitrides, TiN, formed by various techniques such as ion implantation, ion beam assisted deposition, magnetron sputtering, physical vapor deposition (PVD) and chemical vapor deposition (CVD), belong to the group of refractory compounds and have covalent property as well as metallic and ionic properties, which make it fascinating for both fundamental research and technological applications such as hard coatings and as diffusion barriers in microcircuits [1][2][3][4][5][6][7][8][9][10][11][12][13]. The great hardness is typical of compounds with strong covalent bonds [2,4], while the metallic properties result in good electrical conductivity [6][7][8][9][10][11][12][13].…”

Section: Introductionmentioning

confidence: 99%

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Characterization of Deposited and Nitrogen-implanted Titanium Films

Wang

Yamamura

Yamamoto

et al. 2005

e-J. Surf. Sci. Nanotechnol.

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Deposited Ti films and TiN films formed by nitrogen-implantation were investigated by transmission electron microscope (TEM) observation and electron energy loss spectroscopy (EELS). Titanium films in the thickness of 100 nm were deposited by an electron beam heating method onto thermally cleaned NaCl(001) surfaces held at room temperature under ultra-high vacuum. In the deposited Ti films, there coexist mainly (03 · 5)-oriented hcp-Ti and (110)

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Section: (C) the Square Efjk Of Hcp-ti Insupporting

confidence: 74%

“…The peaks of the energy loss of 24.5 eV in Figs. 5(e) and 6(e) were found to be similar to the energy loss of 24.9 eV due to excitation of plasmon for TiN, reported by Pflüger et al [1].…”

Section: (C) the Square Efjk Of Hcp-ti Insupporting

confidence: 59%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Characterization of Deposited and Nitrogen-implanted Titanium Films

Wang

Yamamura

Yamamoto

et al. 2005

e-J. Surf. Sci. Nanotechnol.

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“…The optical properties of such nanocrystals have so far not been determined in the laboratory. The optical properties of TiC in the bulk have been studied extensively (Lye & Logothetis 1966;Alward et al 1975;Ihara et al 1975;Lynch et al 1980;Pflüger et al 1984;Koide et al 1990Koide et al , 1993Delin et al 1996;Espinosa-Magaña et al 2002). Although these studies are focused on the high energy range (the longest wavelength presented is 12 µm), they consistently find a large free electron contribution to the optical properties in the infrared.…”

Section: Titanium Carbide Nano-crystalsmentioning

confidence: 99%

The circumstellar envelope of the C-rich post-AGB star HD 56126

Hony

Tielens

Waters

et al. 2003

A&A

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Abstract. We present a detailed study of the circumstellar envelope of the post-asymptotic giant branch "21 µm object" HD 56126. We build a detailed dust radiative transfer model of the circumstellar envelope in order to derive the dust composition and mass, and the mass-loss history of the star. To model the emission of the dust we use amorphous carbon, hydrogenated amorphous carbon, magnesium sulfide and titanium carbide. We present a detailed parametrisation of the optical properties of hydrogenated amorphous carbon as a function of H/C content. The mid-infrared imaging and spectroscopy is best reproduced by a single dust shell from 1.2 to 2.6 radius around the central star. This shell originates from a short period during which the mass-loss rate exceeded 10 −4 M /yr. We find that the strength of the "21" µm feature poses a problem for the TiC identification. The low abundance of Ti requires very high absorption cross-sections in the ultraviolet and visible wavelength range to explain the strength of the feature. Other nano-crystalline metal carbides should be considered as well. We find that hydrogenated amorphous carbon in radiative equilibrium with the local radiation field does not reach a high enough temperature to explain the strength of the 3.3-3.4 and 6-9 µm hydrocarbon features relative to the 11-17 µm hydrocarbon features. We propose that the carriers of these hydrocarbon features are not in radiative equilibrium but are transiently heated to high temperature. We find that 2 per cent of the dust mass is required to explain the strength of the "30" µm feature, which fits well within the measured atmospheric abundance of Mg and S. This further strengthens the MgS identification of the "30" µm feature.Key words. stars: individual: HD 56126 -stars: AGB and post-AGB -stars: carbon -circumstellar matterstars: mass-loss -infrared: stars IntroductionPost-asymptotic giant branch stars (post-AGBs) are objects in which the strong AGB mass-loss has ceased while the remaining star is not (yet) hot enough to ionise the surrounding material. These objects are characterised by a double-peaked spectral energy distribution (SED). In the ultraviolet (UV) and visible range the central star is visible. In the mid-infrared (IR) range the light is dominated by emission from the dusty circumstellar envelope (CSE). Post-AGB stars are the prime objects to study stellar evolution near the very end of the AGB because they are the most recent evolutionary descendants of the AGB stars. Mass loss near the tip of the AGB is not well understood. There are indications that the mass-loss rates near the end of the AGB exceed the values predicted by Send offprint requests to: S. Hony, e-mail: shony@rssd.esa.int Based on observations taken at the European Southern Observatory, La Silla, Chile and observation obtained with ISO, an ESA project with instruments funded by ESA Member states (especially the PI countries: France, Germany, The Netherlands and the UK) with the participation of ISAS and NASA. the existing dust driven wind models...

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“…The optical properties of such nano-crystals have so far not been determined in the laboratory. The optical properties of TiC in the bulk have been studied extensively (Lye & Logothetis 1966;Alward et al 1975;Ihara et al 1975;Lynch et al 1980;Pflüger et al 1984;Koide et al 1990Koide et al , 1993Delin et al 1996;Espinosa-Magaña et al 2002). Although these studies are focused on the high energy range (the longest wavelength presented is 12 µm), they consistently find a large free electron contribution to the optical properties in the infrared.…”

Section: Titanium Carbide Nano-crystalsmentioning

confidence: 99%

Infrared light on the composition of the dust surrounding carbon-rich stars

Hony¹

2003

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Alle rechten voorbehouden. Niets uit deze uitgave mag worden verveelvoudigd, opgeslagen in een geautomatiseerd gegevensbestand, of openbaar gemaakt, in enige vorm of op enige wijze, hetzij elektronisch, mechanisch, door fotokopieën, opnamen of enige andere manier, zonder voorafgaande schriftelijke toestemming van de uitgever. PrefaceMy first contact with astrophysics was during the introductory astronomy lectures taught by Ed van den Heuvel. From this very first moment I have been captured by a certain charm present throughout astrophysics. Of course the beauty of simplicity, to reduce any given system to its essentials, can be found in astrophysics and physics alike. However, the charm of astrophysics lies also in a totally different beauty. The beauty to do things in a clumsy, impractical way. For astronomy is a science with a history. In every corner of astronomy you find tantalising relics: habits, methods and units inherited from the past. They range from 'O Be A Fine Girl, Kiss Me' to plotting-axes that run the "wrong" way . Of course such silly details sometimes make me want to bang my head on the table, especially when converting ergs/cm 2 /s/Å/sr to Jansky again and taking again more than three tries to get it right. But still, the fact that we have to use the observations from 1987 to study supernova 1987a, gives another dimension to the field.On top of these charms, the study of the stars never fails to trigger a slight surprise in me. The same surprise that you will hear in the voice of non-astronomers: "How can we learn so much about the stars, when they are so far away and all you get is a little bit of light?".After finishing undergraduate astronomy it was very clear to me that I was trained for doing research. I am happy that Rens Waters and Xander Tielens asked me to do a research project under their supervision. That research has resulted in this thesis. I have certainly received a lot of support while doing my research and this is the place where I would like to express my gratitude.First of all, I want to thank Xander and Rens for allowing me the independence I need to work well. Rens; your enthusiasm has often kept me going when I; after weeks of staring; could not find anything interesting anymore in the things that I was doing. Xander, I have enjoyed your practical approach and your encyclopedic knowledge of solid-state physics and literature. I will never forget that time when you took a paper with a only few references scribbled on it from your notebook and handed it to me. You didn't remember what references these were but you said: "Maybe they are of some use." and they were.Words of thanks to Caroline and Els for the very fruitful collaborations that we have had. We started our PhD projects around the same time and I have learned much from observing the way you both handled things. I have always appreciated the support and the gentle way in which you could criticise me: "Maybe have another look at this?". Ciska, you also started your PhD project together with me and we shared office...

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Dielectric properties ofTiCx,TiNx,
J. Pflüger
¹
,
J. Fink
²
,
W. Weber
³

et al.

Cited by 201 publications

References 45 publications

Characterization of Deposited and Nitrogen-implanted Titanium Films

Characterization of Deposited and Nitrogen-implanted Titanium Films

The circumstellar envelope of the C-rich post-AGB star HD 56126

Infrared light on the composition of the dust surrounding carbon-rich stars

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Dielectric properties ofTiCx,TiNx,J. Pflüger1, J. Fink2, W. Weber3 et al.

Cited by 201 publications

References 45 publications

Characterization of Deposited and Nitrogen-implanted Titanium Films

Characterization of Deposited and Nitrogen-implanted Titanium Films

The circumstellar envelope of the C-rich post-AGB star HD 56126

Infrared light on the composition of the dust surrounding carbon-rich stars

Contact Info

Product

Resources

About

Dielectric properties ofTiCx,TiNx,
J. Pflüger
¹
,
J. Fink
²
,
W. Weber
³

et al.