Nanova, M.
Friedrich, S.
Metag, V.
Paryev, E. Ya.
Afzal, F. N.
Bayadilov, D.
Bantes, B.
Beck, R.
Becker, M.
Böse, S.
Brinkmann, K. -T.
Crede, V.
Drexler, P.
Eberhardt, H.
Elsner, D.
Frommberger, F.
Funke, Ch.
Gottschall, M.
Grüner, M.
Gutz, E.
Hammann, Ch.
Hannappel, J.
Hartmann, J.
Hillert, W.
Hoffmeister, Ph.
Honisch, Ch.
Jude, T.
Kaiser, D.
Kalischewski, F.
Keshelashvili, I.
Klein, F.
Koop, K.
Krusche, B.
Lang, M.
Makonyi, K.
Messi, F.
Müller, J.
Müllers, J.
Piontek, D.
Rostomyan, T.
Schaab, D.
Schmidt, Ch.
Schmieden, H.
Schmitz, R.
Seifen, T.
Sokhoyan, V.
Sowa, C.
Spieker, K.
Thiel, A.
Thoma, U.
Triffterer, T.
Urban, M.
van Pee, H.
Walther, D.
Wendel, Ch.
Werthmüller, D.
Wiedner, U.
Wilson, A.
Witthauer, L.
Wunderlich, Y.
Zaunick, H. -G.
Researchers have combined XML3D, which provides declarative, interactive 3D scene descriptions based on HTML5, with Xflow, a language for declarative, high-performance data processing. The result lets Web developers combine a 3D scene graph with data flows for dynamic meshes, animations, image processing, and postprocessing.
A class of Kaluza–Klein cosmological models in f(R, T) theory of gravity have been investigated. In the work, we have considered the functional f(R, T) to be in the form \(f(R,T)=f(R)+f(T)\) with \(f(R)=\lambda R\) and \(f(T)=\lambda T\). Such a choice of the functional f(R, T) leads to an evolving effective cosmological constant \(\Lambda \) which depends on the stress energy tensor. The source of the matter field is taken to be a perfect cosmic fluid. The exact solutions of the field equations are obtained by considering a constant deceleration parameter which leads to two different aspects of the volumetric expansion, namely a power law and an exponential volumetric expansion. Keeping an eye on the accelerating nature of the universe in the present epoch, the dynamics and physical behaviour of the models have been discussed. From statefinder diagnostic pair, we have found that the model with exponential volumetric expansion behaves more like a lambda cold dark matter model.
Klein, F.
Feldhahn, N.
Lee, S.
Wang, H.
Ciuffi, F.
von Elstermann, M.
Toribio, M. L.
Sauer, H.
Wartenberg, M.
Barath, V. S.
Kronke, M.
Wernet, P.
Rowley, J. D.
Muschen, M.
In this paper, we have investigated the five-dimensional Kaluza-Klein space time with wet dark fluid (WDF), which is a candidate for dark energy (DE), in the framework of f(R, T) gravity. R and T denote the Ricci scalar and the trace of the energy-momentum tensor, respectively (Harko et al. Phys. Rev. D, 84, 024020 (2011)). We have used equation of state in the form of WDF for the DE component of the universe. It is modeled on the equation of state p = omega(rho-rho*). With the help of the power law and exponential law of volumetric expansion, we have derived the exact solutions of the corresponding field equations. The geometrical and physical parameters for both the models are studied. The model obtained here may represent the inflationary era in the early universe and very late time of the universe. It is concluded that the model obtained here shows that even in the presence of WDF, the universe indicates accelerated expansion of the universe.
Gonser, S. G.
Klein, F.
Birmili, W.
Groess, J.
Kulmala, M.
Manninen, H. E.
Wiedensohler, A.
Held, A.
In this work, we examined the interaction of ions and neutral particles during atmospheric new particle formation (NPF) events. The analysis is based on simultaneous field measurements of atmospheric ions and total particles using a neutral cluster and air ion spectrometer (NAIS) across the diameter range 2-25 nm. The Waldstein research site is located in a spruce forest in NE Bavaria, Southern Germany, known for enhanced radon concentrations, presumably leading to elevated ionization rates. Our observations show that the occurrence of the ion nucleation mode preceded that of the total particle nucleation mode during all analyzed NPF events. The time difference between the appearance of 2 nm ions and 2 nm total particles was typically about 20 to 30 min. A cross correlation analysis showed a rapid decrease of the time difference between the ion and total modes during the growth process. Eventually, this time delay vanished when both ions and total particles did grow to larger diameters. Considering the growth rates of ions and total particles separately, total particles exhibited enhanced growth rates at diameters below 15 nm. This observation cannot be explained by condensation or coagulation, because these processes would act more efficiently on charged particles compared to neutral particles. To explain our observations, we propose a mechanism including recombination and attachment of continuously present cluster ions with the ion nucleationmode and the neutral nucleation mode, respectively.
Adolph, C.
Aghasyan, M.
Akhunzyanov, R.
Alexeev, M. G.
Alexeev, G. D.
Amoroso, A.
Andrieux, V.
Anfimov, N. V.
Anosov, V.
Augsten, K.
Augustyniak, W.
Austregesilo, A.
Azevedo, C. D. R.
Badełek, B.
Balestra, F.
Ball, M.
Barth, J.
Beck, R.
Bedfer, Y.
Bernhard, J.
Bicker, K.
Bielert, E. R.
Birsa, R.
Bodlak, M.
Bordalo, P.
Bradamante, F.
Braun, C.
Bressan, A.
Büchele, M.
Chang, W.-C.
Chatterjee, C.
Chiosso, M.
Choi, I.
Chung, S.-U.
Cicuttin, A.
Crespo, M. L.
Curiel, Q.
Torre, S. Dalla
Dasgupta, S. S.
Dasgupta, S.
Denisov, O. Yu.
Dhara, L.
Donskov, S. V.
Doshita, N.
Dreisbach, Ch.
Duic, V.
Dünnweber, W.
Dziewiecki, M.
Efremov, A.
Eversheim, P. D.
Eyrich, W.
Faessler, M.
Ferrero, A.
Finger, M.
Finger, M.
Fischer, H.
Franco, C.
von Vijayan Hohenesche, N. du Fresne
Friedrich, J. M.
Frolov, V.
Fuchey, E.
Gautheron, F.
Gavrichtchouk, O. P.
Gerassimov, S.
Giarra, J.
Giordano, F.
Gnesi, I.
Gorzellik, M.
Grabmüller, S.
Grasso, A.
Perdekamp, M. Grosse
Grube, B.
Grussenmeyer, T.
Guskov, A.
Haas, F.
Hahne, D.
Hamar, G.
von Harrach, D.
Heinsius, F. H.
Heitz, R.
Herrmann, F.
Horikawa, N.
d’Hose, N.
Hsieh, C.-Y.
Huber, S.
Ishimoto, S.
Ivanov, A.
Ivanshin, Yu.
Iwata, T.
Jary, V.
Joosten, R.
Jörg, P.
Kabuß, E.
Ketzer, B.
Khaustov, G. V.
Khokhlov, Yu. A.
Kisselev, Yu.
Klein, F.
Klimaszewski, K.
Koivuniemi, J. H.
Kolosov, V. N.
Kondo, K.
Königsmann, K.
Konorov, I.
Konstantinov, V. F.
Kotzinian, A. M.
Kouznetsov, O. M.
Krämer, M.
Kremser, P.
Krinner, F.
Kroumchtein, Z. V.
Kulinich, Y.
Kunne, F.
Kurek, K.
Kurjata, R. P.
Lednev, A. A.
Lehmann, A.
Levillain, M.
Levorato, S.
Lian, Y.-S.
Lichtenstadt, J.
Longo, R.
Maggiora, A.
Magnon, A.
Makins, N.
Makke, N.
Mallot, G. K.
Marianski, B.
Martin, A.
Marzec, J.
Matoušek, J.
Matsuda, H.
Matsuda, T.
Meshcheryakov, G. V.
Meyer, M.
Meyer, W.
Mikhailov, Yu. V.
Mikhasenko, M.
Mitrofanov, E.
Mitrofanov, N.
Miyachi, Y.