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50,633 results on '"Applied Physics"'

51. Single molecule and single quantum dot photodynamics by polarization-rotating modulation microscopy

Author

Institute of Symbiotic Science and Technology, Department of Applied Physics, Graduate School of Engineering, Tokyo University of Agriculture and Technology, Tani, T., Sakai, H., Usukura, E., Suzuki, T., Oda, M., Institute of Symbiotic Science and Technology, Department of Applied Physics, Graduate School of Engineering, Tokyo University of Agriculture and Technology, Tani, T., Sakai, H., Usukura, E., Suzuki, T., and Oda, M.

Abstract

type:Journal Article, We present our recent study of polarization modulating fluorescence imaging microscopy on single CdSe colloidal quantum dots (QDs) and quantum rods (QRs) adsorbed on silica glass substrates at room temperatures. Simple optical setup is introduced to provide detection of emission profiles projected on to the sample plane as well as detection of rotating excitation polarization effect. While most studies so far in structural changes in biological or amorphous systems rely on extrinsic fluorophores with linear transition dipoles, those with twofold degenerate dipoles are noteworthy due to the intrinsic advantage for 3D orientation information. Performance of modulations is also evaluated in combination with tetramethylrodamine moieties as typical linear emitters. CdSe QDs with aspect ratio of 1.3 actually reveal plane-polarized emission at room temperature and, based on maximum-likelihood analysis, are exceptionally highly oriented on silica glass substrates., source:https://doi.org/10.1016/j.phpro.2010.01.228

Published
2017

52. Versatile implementation in angle-resolved optical microscopy: its application to local spectrometry of microcavities with PIC-J-aggregates

Author

Department of Applied Physics Graduate School of Engineering, Tokyo University of Agriculture and Technology, Obara, Y., K., Saitoh, Oda, M., Tani, T., Department of Applied Physics Graduate School of Engineering, Tokyo University of Agriculture and Technology, Obara, Y., K., Saitoh, Oda, M., and Tani, T.

Abstract

type:Journal Article, Versatile novel implementations in microspectroscopy are developed, which can provide angle-resolved optical spectroscopy at local sample areas almost in diffraction limit. By selecting focus position of light flux incident within the back focal plane of the objective lens radially from the position of the optical axis of the microscope with employing off-centered pinhole, we can obtain parallel beam with oblique incidence and its angle tuning at the sample surface. In this paper, we describe our specific optical setup and its practical working principle in detail. We report, as a demonstration of its performance, our latest studies on optical properties of cavity polariton states in the so-called quantum microcavity structures, which contain molecular J-aggregates of pseudoisocyanine (PIC) dye as active working materials. By using the microscope technique, we obtain a fair amount of improvement in the linewidth observation of cavity polariton spectra., source:https://doi.org/10.1155/2011/523017

Published
2017

53. Effects of hydrogen in working gas on valence states of oxygen in sputter-deposited indium tin oxide thin films

Author

Department of Materials Science, Kyushu Institute of Technology/ Liaoning Institute of Technology, Department of Materials Science, Kyushu Institute of Technology, Department of Applied Physics, Fukuoka University, National Institute for Materials Science, Tandem Accelerator Complex, University of Tsukuba, Kyushu Kyoritsu University, Luo, Suning, Kohiki, Shigemi, Okada, Koichi, Kohno, Atsushi, Tajiri, Takayuki, Arai, Masao, Ishii, Satoshi, Sekiba, Daiichiro, Mitome, Masanori, Shoji, Fumiya, Department of Materials Science, Kyushu Institute of Technology/ Liaoning Institute of Technology, Department of Materials Science, Kyushu Institute of Technology, Department of Applied Physics, Fukuoka University, National Institute for Materials Science, Tandem Accelerator Complex, University of Tsukuba, Kyushu Kyoritsu University, Luo, Suning, Kohiki, Shigemi, Okada, Koichi, Kohno, Atsushi, Tajiri, Takayuki, Arai, Masao, Ishii, Satoshi, Sekiba, Daiichiro, Mitome, Masanori, and Shoji, Fumiya

Abstract

type:Journal Article, X-ray photoelectron spectroscopy (XPS) and Rutherford backscattering spectroscopy-elastic recoil detection analysis (RBS-ERDA) revealed that hydrogen in working gas for dc-plasma sputter deposition resided in indium tin oxide (ITO) films and generated the O(-) state seen as the suboxide-like O 1s peak in XPS. Growth of the suboxide-like O 1s peak was parallel with an increase of the resided hydrogen quantified by RBS-ERDA. The first-principles band structure calculation revealed that the electronic structure of In(2)O(3) crystal was realized typically for the most conductive as-deposited film grown in the gas containing hydrogen of 1%. The as-deposited film grown in the gas containing hydrogen of more than 1% exhibited rather high density but low mobility of carriers and showed the electronic structure above 4 eV originated from the O(-) state due to the resided hydrogen in addition to that of the most conducting one. Both well preserved In(2)O(3) band structure and proper concentration of the O(2-) vacancy are indispensable for achieving the highest conductivity; however, the O(-) state lowers efficiency of the carrier doping using the O(2-) vacancy in the lattice and increases density of the ionized scattering center for the carriers., source:https://doi.org/10.1021/am9006676

Published
2017

54. Effect of Nd-Rich Phase on c-Axis Orientation of Nd-Fe-B Melt-Spun Magnet and its Domain Structure

Author

Department of Applied Science for Integrated System Engineering, Graduate School of Engineering, Kyushu Institute of Technology, Department of Applied Physics, Graduate School of Engineering, Tohoku University, Energy Electronics Laboratory, Sojo University, Takezawa, M., Aiba, K., Yasuda, H., Morimoto, Y., Hidaka, T., Yamasaki, J., Kato, H., Yagi, M., Department of Applied Science for Integrated System Engineering, Graduate School of Engineering, Kyushu Institute of Technology, Department of Applied Physics, Graduate School of Engineering, Tohoku University, Energy Electronics Laboratory, Sojo University, Takezawa, M., Aiba, K., Yasuda, H., Morimoto, Y., Hidaka, T., Yamasaki, J., Kato, H., and Yagi, M.

Abstract

type:Journal Article, X-ray diffraction and domain observation were performed to evaluate an effect of Nd-rich phase on the c-axis orientation of the Nd–Fe–B melt-spun ribbon. It was found that adequate addition of Nd-rich phase promotes the c-axis orientation of the Nd–Fe–B ribbon. The (Nd2Fe14B1)95(Nd-rich phase)5 ribbon has c-axis orientation in the entire body from bottom to top when melt-spun at wheel speed of 10.0 m/s.

Published
2017

55. Computer simulations on sprite initiation for realistic lightning models with higher‐frequency surges

Author

Department of Electronic Engineering, University of Electro-Communications, Air Weather Group, Japan Air Self-Defense Force, Solar-Terrestrial Environment Laboratory, Nagoya University, Institute of Applied Physics, Russian Academy of Sciences, Kyushu Institute of Technology, Asano, T., Suzuki, T., Hiraki, Y., Mareev, E., Cho, M., Hayakawa, M., Department of Electronic Engineering, University of Electro-Communications, Air Weather Group, Japan Air Self-Defense Force, Solar-Terrestrial Environment Laboratory, Nagoya University, Institute of Applied Physics, Russian Academy of Sciences, Kyushu Institute of Technology, Asano, T., Suzuki, T., Hiraki, Y., Mareev, E., Cho, M., and Hayakawa, M.

Abstract

type:Journal Article, [1] Computer simulations on transient luminous emissions in the mesosphere and lower ionosphere have been performed for realistic lightning modelings with fast-varying current surges (M components) superimposed on the lightning continuing current (CC). The algorithm used here is an electromagnetic (EM) code, which enables us to estimate self-consistently the reduced electric field, electron density, conductivity, and luminosity as a function of space and time by solving the Maxwell equations. It is found that M components in the CC with small amplitudes, but with a fast-varying EM effect, can initiate or enhance the occurrence of sprites. Even for a return stroke (RS) without CC, subsequent high-frequency current variations (like M components) are found to lead to dramatic changes in the sprite occurrence. The physics underlying these changes is studied by means of, e.g., temporal and spatial variations of luminosity, electron density, and conductivity. As the conclusion, the RS is a fundamental agency for spites, but high-frequency variations as EM effects exhibit an additional essential influence on sprite occurrence. These computational results are used to offer some useful ideas concerning the unsolved problems of sprites and halos, including polarity asymmetry, long-delay characteristics, and morphological shapes of sprites., source:http://onlinelibrary.wiley.com/doi/10.1029/2008JA013651/full

Published
2017

56. Correlation between resistivity and oxygen vacancy of hydrogen-doped indium tin oxide thin films

Author

Department of Materials Science, Kyushu Institute of Technology, Department of Materials Science, Kyushu Institute of Technology/Liaoning Institute of Technology, Tandem Accelerator Complex, University of Tsukuba, National Institute for Materials Science, Department of Applied Physics, Fukuoka University, Kyushu Kyoritsu University, Okada, Koichi, Kohiki, Shigemi, Luo, Suning, Sekiba, Daiichiro, Ishii, Satoshi, Mitome, Masanori, Kohno, Atsushi, Tajiri, Takayuki, Shoji, Fumiya, Department of Materials Science, Kyushu Institute of Technology, Department of Materials Science, Kyushu Institute of Technology/Liaoning Institute of Technology, Tandem Accelerator Complex, University of Tsukuba, National Institute for Materials Science, Department of Applied Physics, Fukuoka University, Kyushu Kyoritsu University, Okada, Koichi, Kohiki, Shigemi, Luo, Suning, Sekiba, Daiichiro, Ishii, Satoshi, Mitome, Masanori, Kohno, Atsushi, Tajiri, Takayuki, and Shoji, Fumiya

Abstract

type:Journal Article, Thin films of indium tin oxide (ITO) sputter-deposited by dc-plasma containing deuterium on glass substrate without any heat treatments exhibited gradual lowering in electrical resistivity with increasing the deuterium content [D2] in plasma gas by 1% and then demonstrated a jump in resistivity by further increase of [D2] than 1%. X-ray photoelectron spectroscopy revealed that hydroxyl-bonded oxygen in ITO grew continuingly with [D2]. Deuterium positioned at the interstitial site increased almost quantitatively with increasing [D2]. Rutherford backscattering spectroscopy showed gradual reduction in the oxygen content of ITO with increasing [D2] by 1% and then demonstrated an abrupt increase of the oxygen content with the increase of [D2] than 1%. The films with [D2] < 1% were oxygen deficient, but those with [D2] > 1% were excess of oxygen. The most oxygen deficient film of [D2] = 1% was the most conductive. Behavior in the resistivity with [D2] looks parallel to that in the oxygen content. A lower resistivity of the films corresponded well to oxygen vacancy rather than hydrogen interstitial., source:https://doi.org/10.1016/j.tsf.2011.01.249

Published
2017

57. Resonance near-field microwave diagnostics in dermatology

Author

Kostrov, A. V.; Institute of Applied Physics, Russian Academy of Sciences, Strikovskiy, A. V.; Institute of Applied Physics, Russian Academy of Sciences, Yanin, D. V.; Institute of Applied Physics, Russian Academy of Sciences, Smirnov, A. I.; Institute of Applied Physics, Russian Academy of Sciences, Pantileeva, G. A.; Research Institute of Dermatology and Venereology, Davoyan, Z. V.; Research Institute of Dermatology and Venereology, Kostrov, A. V.; Institute of Applied Physics, Russian Academy of Sciences, Strikovskiy, A. V.; Institute of Applied Physics, Russian Academy of Sciences, Yanin, D. V.; Institute of Applied Physics, Russian Academy of Sciences, Smirnov, A. I.; Institute of Applied Physics, Russian Academy of Sciences, Pantileeva, G. A.; Research Institute of Dermatology and Venereology, and Davoyan, Z. V.; Research Institute of Dermatology and Venereology

Abstract

Resonance sensors for noninvasive express diagnostics of biological tissues are developed. The sensor operation is based on the method of near-field microwave sounding. The state of a tissue is estimated by its electrodynamic parameters (dielectric permittivity and conductivity). The capabilities (sensitivity, resolution, etc.) of the measuring systems employed for investigation of skin and differential diagnostics of various dermatoses.

Published
2009

58. Bearing estimation of a source with complicated spectrum using a moving sparse antenna array

Author

The work is supported by the Russian Foundation for Basic Research (project 08-02-97025)., Korotin, P. I.; Institute of Applied Physics of the Russian Academy of Sciences, Rodionov, A. A.; Institute of Applied Physics of the Russian Academy of Sciences, Turchin, V. I.; Institute of Applied Physics of the Russian Academy of Sciences, The work is supported by the Russian Foundation for Basic Research (project 08-02-97025)., Korotin, P. I.; Institute of Applied Physics of the Russian Academy of Sciences, Rodionov, A. A.; Institute of Applied Physics of the Russian Academy of Sciences, and Turchin, V. I.; Institute of Applied Physics of the Russian Academy of Sciences

Abstract

Estimation of bearing of a narrowband source with the use of a sparse equidistant array usually turns out to be ambiguous. For a wideband source with smooth spectrum, this ambiguity can be overcome at the expense of decreasing the spatial resolution. At the same time, the ambiguity of bearing estimate of a narrowband source can be eliminated if the array is moving in respect to the source, and the well-known technique used in radars and sonars with synthetic aperture is used (in this case, a single receiver is enough). In the present article, a scenario is analyzed when the source spectrum has a smooth wideband component and several narrowband components; such a spectrum is typical, for example, for underwater noise of ships. It is shown that a procedure of aperture synthesis applied to such a signal gives, under some conditions, the same result as conventional beamforming using a motionless array. This fact allows for effective separation of discrete components of the spectrum from its continuous part. Estimates of aperture synthesis duration allowing one to perform such a separation, as well as output signal-to-noise ratios, are presented.

Published
2009

59. Optimizing the planar structure of (1 1 1) Au/Co/Au trilayers

Author

Applied Physics Program and FOCUS Center, University of Michigan, 450 Church St., Ann Arbor, MI 48109-1040, USA, Applied Physics Program and FOCUS Center, University of Michigan, 450 Church St., Ann Arbor, MI 48109-1040, USA; Instituto de Microelectrónica de Madrid-IMM (CNM-CSIC), Isaac Newton 8-PTM, 28760 Tres Cantos, Madrid, Spain, Instituto de Microelectrónica de Madrid-IMM (CNM-CSIC), Isaac Newton 8-PTM, 28760 Tres Cantos, Madrid, Spain, Physics and Astronomy Department, University of Toledo, 2801 W. Bancroft St., Mailstop 111, Toledo, OH 43606, USA, Ann Arbor, Kumah, D. P., Cebollada, A., Clavero, C., García-Martín, J. M., Skuza, J. R., Lukaszew, R. A., Clarke, R., Applied Physics Program and FOCUS Center, University of Michigan, 450 Church St., Ann Arbor, MI 48109-1040, USA, Applied Physics Program and FOCUS Center, University of Michigan, 450 Church St., Ann Arbor, MI 48109-1040, USA; Instituto de Microelectrónica de Madrid-IMM (CNM-CSIC), Isaac Newton 8-PTM, 28760 Tres Cantos, Madrid, Spain, Instituto de Microelectrónica de Madrid-IMM (CNM-CSIC), Isaac Newton 8-PTM, 28760 Tres Cantos, Madrid, Spain, Physics and Astronomy Department, University of Toledo, 2801 W. Bancroft St., Mailstop 111, Toledo, OH 43606, USA, Ann Arbor, Kumah, D. P., Cebollada, A., Clavero, C., García-Martín, J. M., Skuza, J. R., Lukaszew, R. A., and Clarke, R.

Abstract

Au/Co/Au trilayers are interesting for a range of applications which exploit their unusual optical and electronic transport behaviour in a magnetic field. Here we present a comprehensive structural and morphological study of a series of trilayers with 0–7 nm Co layer thickness fabricated on glass by ultrahigh vacuum vapour deposition. We use a combination of in situ electron diffraction, atomic force microscopy and x-ray scattering to determine the optimum deposition conditions for highly textured, flat and continuous layered structures. The 16 nm Au-on-glass buffer layer, deposited at ambient temperature, is found to develop a smooth (1 1 1) texture on annealing at 350 °C for 10 min. Subsequent growth of the Co layer at 150 °C produces a (1 1 1) textured film with lateral grain size of ∼150 nm in the 7 nm-thick Co layer. A simultaneous in-plane and out-of-plane Co lattice expansion is observed for the thinnest Co layers, converging to bulk values for the thickest films. The roughness of the Co layer is similar to that of the Au buffer layer, indicative of conformal growth. The 6 nm Au capping layer smoothens the trilayer surface, resulting in a surface roughness independent of the Co layer thickness.

Published
2008

60. Theoretical investigation of structural, energetic and electronic properties of titanate pyrochlores

Author

Department of Applied Physics, University of Electronic Science and Technology of China, Chengdu 610054, People’s Republic of China ; Department of Nuclear Engineering and Radiological Sciences, University of Michigan, Ann Arbor, MI 48109-2104, USA, Department of Nuclear Engineering and Radiological Sciences, University of Michigan, Ann Arbor, MI 48109-2104, USA, Departments of Geological Science and Materials Sciences and Engineering, University of Michigan, Ann Arbor, MI 48109-1005, USA, Department of Applied Physics, University of Electronic Science and Technology of China, Chengdu 610054, People’s Republic of China, Ann Arbor, Xiao, H. Y., Wang, L. M., Zu, X. T., Lian, Jie, Ewing, Rodney C., Department of Applied Physics, University of Electronic Science and Technology of China, Chengdu 610054, People’s Republic of China ; Department of Nuclear Engineering and Radiological Sciences, University of Michigan, Ann Arbor, MI 48109-2104, USA, Department of Nuclear Engineering and Radiological Sciences, University of Michigan, Ann Arbor, MI 48109-2104, USA, Departments of Geological Science and Materials Sciences and Engineering, University of Michigan, Ann Arbor, MI 48109-1005, USA, Department of Applied Physics, University of Electronic Science and Technology of China, Chengdu 610054, People’s Republic of China, Ann Arbor, Xiao, H. Y., Wang, L. M., Zu, X. T., Lian, Jie, and Ewing, Rodney C.

Abstract

Ab initio total energy calculations using the plane-wave pseudopotential method based on density functional theory were carried out to investigate the structural, energetic and electronic properties of A2Ti2O7 (A = La, Gd and Yb) pyrochlores. It turned out that the formation energies of antisite defects are not linearly dependent on the ratio of the cation radii, and, for the three compositions, the cation antisite formation energy is largest for Gd2Ti2O7 pyrochlore. It was indicated that Gd2Ti2O7 compound is the least likely to form defect fluorite structure, which gives rise to the least resistance to radiation-induced amorphization. DOS analysis showed that stronger interaction exists in the Gd2Ti2O7 compound, and its electronic structure is very different from that of La2Ti2O7 and Yb2Ti2O7. Our calculations suggested that the electronic structure of the A cation and bond type should be taken into account when explaining the response behavior of A2Ti2O7 (A = La, Gd, Yb) pyrochlores to ion irradiation-induced amorphization.

Published
2008

61. Adaptive techniques of the wavefield formation in random-inhomogeneous multimode propagation channels by the use of large arrays

Author

This research was supported in part by the Russian Federal Agency for Science and Innovations (Project No. NSh-6043.2006.2)., Gorodetskaya, Elena Yu.; Institute of Applied Physics, Russian Academy of Sciences, Malekhanov, Alexander I.; Institute of Applied Physics, Russian Academy of Sciences, Sazontov, A. G.; Institute of Applied Physics, Russian Academy of Sciences, Vdovicheva, N. K.; Institute for Physics of Microstructures, Russian Academy of Sciences, This research was supported in part by the Russian Federal Agency for Science and Innovations (Project No. NSh-6043.2006.2)., Gorodetskaya, Elena Yu.; Institute of Applied Physics, Russian Academy of Sciences, Malekhanov, Alexander I.; Institute of Applied Physics, Russian Academy of Sciences, Sazontov, A. G.; Institute of Applied Physics, Russian Academy of Sciences, and Vdovicheva, N. K.; Institute for Physics of Microstructures, Russian Academy of Sciences

Abstract

We address the source array synthesis problem in a random propagation channel under the different optimization criteria specified for the remote receiving array, namely, the criteria of (i) the output SNR and (ii) the array gain. For the first step, we discuss the optimal schemes for the source excitation and array beamforming by using a general technique of the eigenvalue-eigenvector expansion associated with the normal-mode model of long-range signal propagation in a channel. Then, we develop an adaptive approach to the source array synthesis which is shown to be an iterative correction of the sources excitation coefficients depending on the signal coherence, the receiving array arrangement in a channel, and also on the modal spectrum of the ambient noise interference. Computer simulation is performed for the vertical source and receiving arrays in random-inhomogeneous environments typical for sound propagation in shallow-water channels from the Barents Sea. The results exhibit distinctly a rather high efficiency of the adaptive synthesis algorithms for various sets of the source and environmental parameters including the signal frequency, distance, vertical locations of the sources and receivers.

Published
2007

62. ZnO nanoparticles embedded in sapphire fabricated by ion implantation and annealing

Author

Department of Nuclear Engineering and Radiological Sciences, University of Michigan, Ann Arbor, MI 48109-2104, USA, Department of Applied Physics, University of Electronic Science and Technology of China, Chengdu, 610054, People???s Republic of China, Department of Applied Physics, University of Electronic Science and Technology of China, Chengdu, 610054, People???s Republic of China ; International Center for Material Physics, Chinese Academy of Sciences, Shenyang 110015, People???s Republic of China, Ann Arbor, Xiang, X., Zu, X. T., Zhu, S., Wei, Q. M., Zhang, C. F., Sun, K., Wang, L. M., Department of Nuclear Engineering and Radiological Sciences, University of Michigan, Ann Arbor, MI 48109-2104, USA, Department of Applied Physics, University of Electronic Science and Technology of China, Chengdu, 610054, People???s Republic of China, Department of Applied Physics, University of Electronic Science and Technology of China, Chengdu, 610054, People???s Republic of China ; International Center for Material Physics, Chinese Academy of Sciences, Shenyang 110015, People???s Republic of China, Ann Arbor, Xiang, X., Zu, X. T., Zhu, S., Wei, Q. M., Zhang, C. F., Sun, K., and Wang, L. M.

Abstract

ZnO nanoparticles were fabricated in sapphire (??-Al2O3 single crystal) by Zn ion implantation (48??keV) at an ion fluence of 1 ?? 1017??cm???2 and subsequent thermal annealing in a flowing oxygen atmosphere. Transmission electron microscopy (TEM) analysis revealed that metallic Zn nanoparticles of 3???10??nm in dimensions formed in the as-implanted sample and that ZnO nanoparticles of 10???12??nm in dimensions formed after annealing at 600?????C. A broad absorption band, peaked at 280??nm, appeared in the as-implanted crystal, due to surface plasma resonance (SPR) absorption of metallic Zn nanoparticles. After annealing at 600?????C, ZnO nanoparticles resulted in an exciton absorption peak at 360??nm. The photoluminescence (PL) of the as-implanted sample was very weak when using a He???Cd 325??nm line as the excitation source. However, two emission peaks appeared in the PL spectrum of ZnO nanopraticles, i.e., one ultraviolet (UV) peak at 370??nm and the other a green peak at 500??nm. The emission at 500??nm is stronger and has potential applications in green/blue light-emitting devices.

Published
2006

63. Multiwavelength observations of Mrk 501 in 2008

Author

MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Ansoldi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), L. A. Antonelli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), A. Babic(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), P. Bangale(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, D-80805 München, Germany), J. A. Barrio(Universidad Complutense, E-28040 Madrid, Spain), J. Becerra González(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), W. Bednarek(University of Lodz, PL-90236 Lodz, Poland), K. Berger(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, CH-8093 Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), R. K. Bock(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Bonnefoy(Universidad Complutense, E-28040 Madrid, Spain), G. Bonnoli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), F. Borracci(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Bretz(Universität Würzburg, D-97074 Würzburg, Germany), E. Carmona(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), A. Carosi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Carreto Fidalgo(Universität Würzburg, D-97074 Würzburg, Germany), P. Colin(Max-Planck-Institut für Physik, D-80805 München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), J. L. Contreras(Universidad Complutense, E-28040 Madrid, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Covino(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), F. Dazzi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), A. De Angelis(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), B. De Lotto(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), C. Delgado Mendez(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), M. Doert(Technische Universität Dortmund, D-44221 Dortmund, Germany), A. Domínguez(Inst. de Astrofísica de Andalucía), D. Dominis Prester(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Dorner(Universität Würzburg, D-97074 Würzburg, Germany), M. Doro(Università di Padova and INFN, I-35131 Padova, Italy), S. Einecke(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Eisenacher(Universität Würzburg, D-97074 Würzburg, Germany), D. Elsaesser(Universität Würzburg, D-97074 Würzburg, Germany), E. Farina(Università dell'Insubria, Como, I-22100 Como, Italy), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), M. V. Fonseca(Universidad Complutense, E-28040 Madrid, Spain), L. Font(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), K. Frantzen(Technische Universität Dortmund, D-44221 Dortmund, Germany), C. Fruck(Max-Planck-Institut für Physik, D-80805 München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Garczarczyk(Deutsches Elektronen-Synchrotron), D. Garrido Terrats(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), M. Gaug(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), A. González Muñoz(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), A. Hadamek(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Hadasch(Institut de Ciències de l'Espai), A. Herrero(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), D. Hildebrand(ETH Zurich, CH-8093 Zurich, Switzerland), J. Hose(Max-Planck-Institut für Physik, D-80805 München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), W. Idec(University of Lodz, PL-90236 Lodz, Poland), V. Kadenius(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), H. Kellermann(Max-Planck-Institut für Physik, D-80805 München, Germany), M. L. Knoetig(ETH Zurich, CH-8093 Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Kushida(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. La Barbera(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), N. Lewandowska(Universität Würzburg, D-97074 Würzburg, Germany), E. Lindfors(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), S. Lombardi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), M. López(Universidad Complutense, E-28040 Madrid, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), E. Lorenz(Max-Planck-Institut für Physik, D-80805 München, Germany), I. Lozano(Universidad Complutense, E-28040 Madrid, Spain), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), K. Mallot(Deutsches Elektronen-Synchrotron), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), N. Mankuzhiyil(2,*), K. Mannheim(Universität Würzburg, D-97074 Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), B. Marcote(Universitat de Barcelona), M. Mariotti(Università di Padova and INFN, I-35131 Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), D. Mazin(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Menzel(Max-Planck-Institut für Physik, D-80805 München, Germany), M. Meucci(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Moralejo(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), P. Munar-Adrover(Universitat de Barcelona), D. Nakajima(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Niedzwiecki(University of Lodz, PL-90236 Lodz, Poland), K. Nilsson(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), N. Nowak(Max-Planck-Institut für Physik, D-80805 München, Germany), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Overkemping(Technische Universität Dortmund, D-44221 Dortmund, Germany), S. Paiano(Università di Padova and INFN, I-35131 Padova, Italy), M. Palatiello(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), D. Paneque(6,*), R. Paoletti(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Paredes(Universitat de Barcelona), X. Paredes-Fortuny(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), M. Persic(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), E. Prandini(Università di Padova and INFN, I-35131 Padova, Italy), S. Preziuso(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), R. Reinthal(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), W. Rhode(Technische Universität Dortmund, D-44221 Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), J. Rodriguez Garcia(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Rügamer(Universität Würzburg, D-97074 Würzburg, Germany), A. Saggion(Università di Padova and INFN, I-35131 Padova, Italy), T. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), K. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), M. Salvati(INAF National Institute for Astrophysics, I-00136 Rome, Italy), K. Satalecka(7,*), V. Scalzotto(Università di Padova and INFN, I-35131 Padova, Italy), V. Scapin(Universidad Complutense, E-28040 Madrid, Spain), C. Schultz(Università di Padova and INFN, I-35131 Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, D-80805 München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), A. Sillanpää(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Sobczynska(University of Lodz, PL-90236 Lodz, Poland), F. Spanier(Universität Würzburg, D-97074 Würzburg, Germany), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. Stamerra(INAF National Institute for Astrophysics, I-00136 Rome, Italy), T. Steinbring(Universität Würzburg, D-97074 Würzburg, Germany), J. Storz(Universität Würzburg, D-97074 Würzburg, Germany), S. Sun(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), L. Takalo(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), F. Tavecchio(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Thaele(Technische Universität Dortmund, D-44221 Dortmund, Germany), O. Tibolla(Universität Würzburg, D-97074 Würzburg, Germany), D. F. Torres(Institut de Ciències de l'Espai), T. Toyama(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Treves(Università dell'Insubria, Como, I-22100 Como, Italy), M. Uellenbeck(Technische Universität Dortmund, D-44221 Dortmund, Germany), P. Vogler(ETH Zurich, CH-8093 Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, D-80805 München, Germany), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), VERITAS Collaboration(Deutsches Elektronen-Synchrotron), (Deutsches Elektronen-Synchrotron), B. Behera(Deutsches Elektronen-Synchrotron), M. Beilicke(Department of Physics, Washington University, St. Louis, MO 63130, USA), W. Benbow(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), R. Bird(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), A. Bouvier(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), V. Bugaev(Department of Physics, Washington University, St. Louis, MO 63130, USA), M. Cerruti(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), X. Chen(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), L. Ciupik(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), E. Collins-Hughes(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), W. Cui(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), C. Duke(Department of Physics, Grinnell College, Grinnell, IA 50112-1690, USA), J. Dumm(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), A. Falcone(Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802, USA), S. Federici(now at GRAPPA Institute, University of Amsterdam, 1098XH), Q. Feng(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), J. P. Finley(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), L. Fortson(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), A. Furniss(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), N. Galante(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), G. H. Gillanders(School of Physics, National University of Ireland Galway, University Road, Galway, Ireland), S. Griffin(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), S. T. Griffiths(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), J. Grube(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), G. Gyuk(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), D. Hanna(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), J. Holder(Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), C. A. Johnson(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), P. Kaaret(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), M. Kertzman(Department of Physics and Astronomy, DePauw University, Greencastle, IN 46135-0037, USA), D. Kieda(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), H. Krawczynski(Department of Physics, Washington University, St. Louis, MO 63130, USA), M. J. Lang(School of Physics, National University of Ireland Galway, University Road, Galway, Ireland), A. S Madhavan(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), G. Maier(Deutsches Elektronen-Synchrotron), P. Majumdar(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), K. Meagher(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), P. Moriarty(Department of Life and Physical Sciences, Galway-Mayo Institute of Technology, Dublin Road, Galway, Ireland), R. Mukherjee(Department of Physics and Astronomy, Barnard College, Columbia University, NY 10027, USA), D. Nieto(Physics Department, Columbia University, New York, NY 10027, USA), A. O'Faoláin de Bhróithe(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), R. A. Ong(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), A. N. Otte(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), A. Pichel(Instituto de Astronomia y Fisica del Espacio, Casilla de Correo 67 - Sucursal 28), M. Pohl(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), A. Popkow(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), H. Prokoph(Deutsches Elektronen-Synchrotron), J. Quinn(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), J. Rajotte(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), G. Ratliff(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), L. C. Reyes(Physics Department, California Polytechnic State University, San Luis Obispo, CA 94307, USA), P. T. Reynolds(Department of Applied Physics and Instrumentation, Cork Institute of Technology, Bishopstown, Cork, Ireland), G. T. Richards(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), E. Roache(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), G. H. Sembroski(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), K. Shahinyan(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), F. Sheidaei(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), A. W. Smith(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), D. Staszak(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), I. Telezhinsky(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), M. Theiling(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), J. Tyler(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), A. Varlotta(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), S. Vincent(Deutsches Elektronen-Synchrotron), S. P. Wakely(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), T. C. Weekes(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), R. Welsing(Deutsches Elektronen-Synchrotron), D. A. Williams(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), A. Zajczyk(Department of Physics, Washington University, St. Louis, MO 63130, USA), B. Zitzer(Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA), External Collaborators(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), (INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), M. Villata(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), C. M. Raiteri(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), M. Ajello(Space Sciences Laboratory, 7 Gauss Way, University of California, Berkeley, CA 94720-7450, USA), M. Perri(ASI-Science Data Center, Via del Politecnico, I-00133 Rome, Italy), H. D. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), M. F. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), V. M. Larionov(Astron. Inst., St.-Petersburg State Univ., Russia), N. V. Efimova(Astron. Inst., St.-Petersburg State Univ., Russia), T. S. Konstantinova(Astron. Inst., St.-Petersburg State Univ., Russia), E. N. Kopatskaya(Astron. Inst., St.-Petersburg State Univ., Russia), W. P. Chen(Graduate Institute of Astronomy, National Central University, 300 Jhongda Rd., Jhongli 32001, Taiwan), E. Koptelova(Graduate Institute of Astronomy, National Central University, 300 Jhongda Rd., Jhongli 32001, Taiwan), H. Y. Hsiao(Graduate Institute of Astronomy, National Central University, 300 Jhongda Rd., Jhongli 32001, Taiwan), O. M. Kurtanidze(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), M. G. Nikolashvili(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), G. N. Kimeridze(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), B. Jordan(School of Cosmic Physics, Dublin Institute For Advanced Studies, Ireland), P. Leto(INAF - Osservatorio Astrofisico di Catania, Italy), C. S. Buemi(INAF - Osservatorio Astrofisico di Catania, Italy), C. Trigilio(INAF - Osservatorio Astrofisico di Catania, Italy), G. Umana(INAF - Osservatorio Astrofisico di Catania, Italy), A. Lahtenmaki(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), E. Nieppola(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), M. Tornikoski(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), J. Sainio(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), M. Giroletti(INAF Istituto di Radioastronomia, 40129 Bologna, Italy), A. Cesarini(University of Trento, Department of Physics, I38050 Povo, Trento, Italy), L. Fuhrmann(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), Yu. A. Kovalev(Astro Space Center of the Lebedev Physical Institute, 117997), Y. Y. Kovalev(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), Anne Lähteenmäki Group, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, Universitat de Barcelona, School services, ELEC, and ~

Subjects
extragalactic background light, Ciencias Físicas, Flux, Electron, Astrophysics, 7. Clean energy, law.invention, purl.org/becyt/ford/1 [https], Raigs gamma, bl lacertae objects, law, individual: Mrk 501 [BL Lacertae objects], Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, 213 Electronic, automation and communications engineering, electronics, Astroparticle physics, BL Lacertae objects: individual: Mrk 501, Gamma rays: general, Astronomy and Astrophysics, Space and Planetary Science, Synchrotron, individual: Mrk 50 [BL Lacertae objects], Homogeneous, astroparticle physics, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, 1171 Geosciences, Astrophysics::High Energy Astrophysical Phenomena, emitting electrons, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 114 Physical sciences, bl lacertae objects: individual: mrk 501, crab-nebula, Blazar, Astrophysics::Galaxy Astrophysics, tev blazars, variability, 221 Nanotechnology, Gamma rays, Individual: Mrk 501, Institut für Physik und Astronomie, purl.org/becyt/ford/1.3 [https], gamma rays: general, Galaxies, gamma-ray emission, telescope system, Galàxies, Active Galaxies, blazars, gamma-rays, Mrk 501, Astronomía, Crab Nebula, x-ray, 115 Astronomy and space science, Low emission, 216 Materials engineering, Galàxies actives, active galactic nuclei, Active galaxies, ddc:520, general [gamma rays]
Abstract

Mrk 501 is one of the brightest blazars at TeV energies and has been extensively studied since its first VHE detection in 1996. Our goal is to characterize in detail the source gamma-ray emission, together with the radio-to-X-ray emission, during the non-flaring (low) activity, which is less often studied than the occasional flaring (high) activity. We organized a multiwavelength (MW) campaign on Mrk 501 between March and May 2008. This multi-instrument effort included the most sensitive VHE gamma-ray instruments in the northern hemisphere, namely the imaging atmospheric Cherenkov telescopes MAGIC and VERITAS, as well as Swift, RXTE, the F-GAMMA, GASP-WEBT, and other collaborations and instruments. Mrk 501 was found to be in a low state of activity during the campaign, with a VHE flux in the range of 10%-20% of the Crab nebula flux. Nevertheless, significant flux variations were detected with various instruments, with a trend of increasing variability with energy. The broadband spectral energy distribution during the two different emission states of the campaign can be adequately described within the homogeneous one-zone synchrotron self-Compton model, with the (slightly) higher state described by an increase in the electron number density. This agrees with previous studies of the broadband emission of this source during flaring and non-flaring states. We report for the first time a tentative X-ray-to-VHE correlation during a low VHE activity. Although marginally significant, this positive correlation between X-ray and VHE, which has been reported many times during flaring activity, suggests that the mechanisms that dominate the X-ray/VHE emission during non-flaring-activity are not substantially different from those that are responsible for the emission during flaring activity., Comment: Accepted for publication in A&A

Published
2015
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64. The 2009 multiwavelength campaign on Mrk 421: Variability and correlation studies

Author

MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Ansoldi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), L. A. Antonelli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), A. Babic(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), P. Bangale(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, D-80805 München, Germany), J. A. Barrio(Universidad Complutense, E-28040 Madrid, Spain), J. Becerra González(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), W. Bednarek(University of Lodz, PL-90236 Lodz, Poland), K. Berger(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, CH-8093 Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), R. K. Bock(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Bonnefoy(Universidad Complutense, E-28040 Madrid, Spain), G. Bonnoli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), F. Borracci(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Bretz(Universität Würzburg, D-97074 Würzburg, Germany), E. Carmona(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), A. Carosi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Carreto Fidalgo(Universität Würzburg, D-97074 Würzburg, Germany), P. Colin(Max-Planck-Institut für Physik, D-80805 München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), J. L. Contreras(Universidad Complutense, E-28040 Madrid, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Covino(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), F. Dazzi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), A. De Angelis(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), B. De Lotto(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), C. Delgado Mendez(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), M. Doert(Technische Universität Dortmund, D-44221 Dortmund, Germany), A. Domínguez(Inst. de Astrofísica de Andalucía), D. Dominis Prester(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Dorner(Universität Würzburg, D-97074 Würzburg, Germany), M. Doro(Università di Padova and INFN, I-35131 Padova, Italy), S. Einecke(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Eisenacher(Universität Würzburg, D-97074 Würzburg, Germany), D. Elsaesser(Universität Würzburg, D-97074 Würzburg, Germany), E. Farina(Università dell'Insubria, Como, I-22100 Como, Italy), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), M. V. Fonseca(Universidad Complutense, E-28040 Madrid, Spain), L. Font(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), K. Frantzen(Technische Universität Dortmund, D-44221 Dortmund, Germany), C. Fruck(Max-Planck-Institut für Physik, D-80805 München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Garczarczyk(Deutsches Elektronen-Synchrotron), D. Garrido Terrats(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), M. Gaug(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), A. González Mu\ noz(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), A. Hadamek(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Hadasch(Institut de Ciències de l'Espai), A. Herrero(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), D. Hildebrand(ETH Zurich, CH-8093 Zurich, Switzerland), J. Hose(Max-Planck-Institut für Physik, D-80805 München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), W. Idec(University of Lodz, PL-90236 Lodz, Poland), V. Kadenius(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), H. Kellermann(Max-Planck-Institut für Physik, D-80805 München, Germany), M. L. Knoetig(ETH Zurich, CH-8093 Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Kushida(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. La Barbera(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), N. Lewandowska(Universität Würzburg, D-97074 Würzburg, Germany), E. Lindfors(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), F. Longo(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), S. Lombardi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), M. López(Universidad Complutense, E-28040 Madrid, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), E. Lorenz(Max-Planck-Institut für Physik, D-80805 München, Germany), I. Lozano(Universidad Complutense, E-28040 Madrid, Spain), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), K. Mallot(Deutsches Elektronen-Synchrotron), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), N. Mankuzhiyil(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), K. Mannheim(Universität Würzburg, D-97074 Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), B. Marcote(Universitat de Barcelona), M. Mariotti(Università di Padova and INFN, I-35131 Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), D. Mazin(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Menzel(Max-Planck-Institut für Physik, D-80805 München, Germany), M. Meucci(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Moralejo(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), P. Munar-Adrover(Universitat de Barcelona), D. Nakajima(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Niedzwiecki(University of Lodz, PL-90236 Lodz, Poland), K. Nilsson(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), N. Nowak(6,32,*), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Overkemping(Technische Universität Dortmund, D-44221 Dortmund, Germany), S. Paiano(Università di Padova and INFN, I-35131 Padova, Italy), M. Palatiello(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), D. Paneque(6,*), R. Paoletti(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Paredes(Universitat de Barcelona), X. Paredes-Fortuny(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), M. Persic(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), E. Prandini(Università di Padova and INFN, I-35131 Padova, Italy), S. Preziuso(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), R. Reinthal(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), W. Rhode(Technische Universität Dortmund, D-44221 Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), J. Rodriguez Garcia(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Rügamer(Universität Würzburg, D-97074 Würzburg, Germany), A. Saggion(Università di Padova and INFN, I-35131 Padova, Italy), K. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), M. Salvati(INAF National Institute for Astrophysics, I-00136 Rome, Italy), K. Satalecka(Universidad Complutense, E-28040 Madrid, Spain), V. Scalzotto(Università di Padova and INFN, I-35131 Padova, Italy), V. Scapin(Universidad Complutense, E-28040 Madrid, Spain), C. Schultz(Università di Padova and INFN, I-35131 Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, D-80805 München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), A. Sillanpää(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Sobczynska(University of Lodz, PL-90236 Lodz, Poland), F. Spanier(Universität Würzburg, D-97074 Würzburg, Germany), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. Stamerra(INAF National Institute for Astrophysics, I-00136 Rome, Italy), T. Steinbring(Universität Würzburg, D-97074 Würzburg, Germany), J. Storz(Universität Würzburg, D-97074 Würzburg, Germany), S. Sun(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), L. Takalo(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), F. Tavecchio(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Thaele(Technische Universität Dortmund, D-44221 Dortmund, Germany), O. Tibolla(Universität Würzburg, D-97074 Würzburg, Germany), D. F. Torres(Institut de Ciències de l'Espai), T. Toyama(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Treves(Università dell'Insubria, Como, I-22100 Como, Italy), M. Uellenbeck(Technische Universität Dortmund, D-44221 Dortmund, Germany), P. Vogler(ETH Zurich, CH-8093 Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, D-80805 München, Germany), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), VERITAS collaboration(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), (Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), S. Archambault(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), B. Behera(Deutsches Elektronen-Synchrotron), M. Beilicke(Department of Physics, Washington University, St. Louis, MO 63130, USA), W. Benbow(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), R. Bird(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), J. H. Buckley(Department of Physics, Washington University, St. Louis, MO 63130, USA), V. Bugaev(Department of Physics, Washington University, St. Louis, MO 63130, USA), M. Cerruti(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), X. Chen(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), L. Ciupik(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), E. Collins-Hughes(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), W. Cui(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. Dumm(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), J. D. Eisch(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), A. Falcone(Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802, USA), S. Federici(DESY, Platanenallee 6, 15738 Zeuthen, Germany), Q. Feng(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. P. Finley(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), H. Fleischhack(Deutsches Elektronen-Synchrotron), P. Fortin(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA), L. Fortson(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), A. Furniss(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), S. Griffin(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), S. T. Griffiths(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), J. Grube(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), G. Gyuk(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), D. Hanna(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), J. Holder(Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), G. Hughes(Deutsches Elektronen-Synchrotron), T. B. Humensky(Physics Department, Columbia University, New York, NY 10027, USA), C. A. Johnson(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), P. Kaaret(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), M. Kertzman(Department of Physics and Astronomy, DePauw University, Greencastle, IN 46135-0037, USA), Y. Khassen(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), D. Kieda(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), H. Krawczynski(Department of Physics, Washington University, St. Louis, MO 63130, USA), F. Krennrich(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), S. Kumar(Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), M. J. Lang(School of Physics, National University of Ireland Galway, University Road, Galway, Ireland), G. Maier(Deutsches Elektronen-Synchrotron), S. McArthur(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), K. Meagher(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), P. Moriarty(Department of Life and Physical Sciences, Galway-Mayo Institute of Technology, Dublin Road, Galway, Ireland), R. Mukherjee(Department of Physics and Astronomy, Barnard College, Columbia University, NY 10027, USA), R. A. Ong(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), A. N. Otte(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), N. Park(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), A. Pichel(Instituto de Astronomia y Fisica del Espacio, Casilla de Correo 67 - Sucursal 28), M. Pohl(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), A. Popkow(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), H. Prokoph(Deutsches Elektronen-Synchrotron), J. Quinn(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), K. Ragan(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), J. Rajotte(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), P. T. Reynolds(Department of Applied Physics and Instrumentation, Cork Institute of Technology, Bishopstown, Cork, Ireland), G. T. Richards(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), E. Roache(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), A. C. Rovero(Instituto de Astronomia y Fisica del Espacio, Casilla de Correo 67 - Sucursal 28), G. H. Sembroski(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), K. Shahinyan(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), D. Staszak(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), I. Telezhinsky(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), M. Theiling(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. V. Tucci(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. Tyler(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), A. Varlotta(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), S. P. Wakely(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), T. C. Weekes(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), A. Weinstein(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), R. Welsing(Deutsches Elektronen-Synchrotron), A. Wilhelm(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), D. A. Williams(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), B. Zitzer(Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA), External collaborators(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), (INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), M. Villata(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), C. Raiteri(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), H. D. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), M. F. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), W. P. Chen(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), B. Jordan(School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin, 2, Ireland), E. Koptelova(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), O. M. Kurtanidze(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), A. Lähteenmäki(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), B. McBreen(University College Dublin, Belfield, Dublin 4, Ireland), V. M. Larionov(Isaac Newton Institute of Chile, St. Petersburg Branch, St. Petersburg, Russia), C. S. Lin(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), M. G. Nikolashvili(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), E. Angelakis(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), M. Capalbi(ASI-Science Data Center, Via del Politecnico, I-00133 Rome, Italy), A. Carrami\ nana(Instituto Nacional de Astrofísica, Óptica y Electrónica, Tonantzintla, Puebla 72840, Mexico), L. Carrasco(Instituto Nacional de Astrofísica, Óptica y Electrónica, Tonantzintla, Puebla 72840, Mexico), P. Cassaro(INAF Istituto di Radioastronomia, Sezione di Noto, Contrada Renna Bassa, 96017 Noto), A. Cesarini(Department of Physics, University of Trento, I38050, Povo, Trento, Italy), L. Fuhrmann(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), M. Giroletti(INAF Istituto di Radioastronomia, 40129 Bologna, Italy), T. Hovatta(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), T. P. Krichbaum(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), H. A. Krimm(Astro Space Center of the Lebedev Physical Institute, 117997 Moscow, Russia), W. Max-Moerbeck(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), J. W. Moody(Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA), G. Maccaferri(INAF Istituto di Radioastronomia, Stazione Radioastronomica di Medicina, I-40059 Medicina), Y. Mori(Department of Physics, Tokyo Institute of Technology, Meguro City, Tokyo 152-8551, Japan), I. Nestoras(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), A. Orlati(INAF Istituto di Radioastronomia, Stazione Radioastronomica di Medicina, I-40059 Medicina), C. Pace(Indiana University, Department of Astronomy, Swain Hall West 319, Bloomington, IN 47405-7105, USA), R. Pearson(Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA), M. Perri(INAF National Institute for Astrophysics, I-00136 Rome, Italy), A. C. S. Readhead(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), J. L. Richards(Department of Physics, Purdue University, 525 Northwestern Ave, West Lafayette, IN 47907), A. C. Sadun(Department of Physics, University of Colorado, Denver, CO 80220, USA), T. Sakamoto(Department of Physics and Mathematics, College of Science and 952 Engineering, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuoku, Sagamihara-shi Kanagawa 252-5258, Japan), J. Tammi(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), M. Tornikoski(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), Y. Yatsu(Department of Physics, Tokyo Institute of Technology, Meguro City, Tokyo 152-8551, Japan), A. Zook(Department of Physics and Astronomy, Pomona College, Claremont CA 91711-6312, USA), Aleksić, J, Ansoldi, Stefano, Antonelli, L. A., Antoranz, P., Babic, A., Bangale, P., Barres De Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Berger, K., Bernardini, E., Biland, A., Blanch, O., Bock, R. K., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Carreto Fidalgo, D., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Caneva, G., De Lotto, B., Delgado Mendez, C., Doert, M., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher, D., Elsaesser, D., Farina, E., Ferenc, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., García López, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giavitto, G., Godinović, N., González Muñoz, A., Gozzini, S. R., Hadamek, A., Hadasch, D., Herrero, A., Hildebrand, D., Hose, J., Hrupec, D., Idec, W., Kadenius, V., Kellermann, H., Knoetig, M. L., Krause, J., Kushida, J., La Barbera, A., Lelas, D., Lewandowska, N., Lindfors, E., Longo, Francesco, Lombardi, S., López, M., López Coto, R., López Oramas, A., Lorenz, E., Lozano, I., Makariev, M., Mallot, K., Maneva, G., Mankuzhiyil, N., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Meucci, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Munar Adrover, P., Nakajima, D., Niedzwiecki, A., Nilsson, K., Nowak, N., Orito, R., Overkemping, A., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Partini, S., Persic, M., Prada, F., Prada Moroni, P. G., Prandini, E., Preziuso, S., Puljak, I., Reinthal, R., Rhode, W., Ribó, M., Rico, J., Rodriguezgarcia, J., Rügamer, S., Saggion, A., Saito, K., Salvati, M., Satalecka, K., Scalzotto, V., Scapin, V., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Spanier, F., Stamatescu, V., Stamerra, A., Steinbring, T., Storz, J., Sun, S., Surić, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Tibolla, O., Torres, D. F., Toyama, T., Treves, A., Uellenbeck, M., Vogler, P., Wagner, R. M., Zandanel, F., Zanin, R., Archambault, S., Behera, B., Beilicke, M., Benbow, W., Bird, R., Buckley, J. H., Bugaev, V., Cerruti, M., Chen, X., Ciupik, L., Collins Hughes, E., Cui, W., Dumm, J., Eisch, J. D., Falcone, A., Federici, S., Feng, Q., Finley, J. P., Fleischhack, H., Fortin, P., Fortson, L., Furniss, A., Griffin, S., Griffiths, S. T., Grube, J., Gyuk, G., Hanna, D., Holder, J., Hughes, G., Humensky, T. B., Johnson, C. A., Kaaret, P., Kertzman, M., Khassen, Y., Kieda, D., Krawczynski, H., Krennrich, F., Kumar, S., Lang, M. J., Maier, G., Mcarthur, S., Meagher, K., Moriarty, P., Mukherjee, R., Ong, R. A., Otte, A. N., Park, N., Pichel, A., Pohl, M., Popkow, A., Prokoph, H., Quinn, J., Ragan, K., Rajotte, J., Reynolds, P. T., Richards, G. T., Roache, E., Rovero, A. C., Sembroski, G. H., Shahinyan, K., Staszak, D., Telezhinsky, I., Theiling, M., Tucci, J. V., Tyler, J., Varlotta, A., Wakely, S. P., Weekes, T. C., Weinstein, A., Welsing, R., Wilhelm, A., Williams, D. A., Zitzer, B., Villata, M., Raiteri, C., Aller, H. D., Aller, M. F., Chen, W. P., Jordan, B., Koptelova, E., Kurtanidze, O. M., Lähteenmäki, A., Mcbreen, B., Larionov, V. M., Lin, C. S., Nikolashvili, M. G., Angelakis, E., Capalbi, M., Carramiñana, A., Carrasco, L., Cassaro, P., Cesarini, A., Fuhrmann, L., Giroletti, M., Hovatta, T., Krichbaum, T. P., Krimm, H. A., Max Moerbeck, W., Moody, J. W., Maccaferri, G., Mori, Y., Nestoras, I., Orlati, A., Pace, C., Pearson, R., Perri, M., Readhead, A. C. S., Richards, J. L., Sadun, A. C., Sakamoto, T., Tammi, J., Tornikoski, M., Yatsu, Y., Zook, A., Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, and Universitat de Barcelona

Subjects
Astrofísica, Brightness, Ciencias Físicas, blazars, Astrophysics, telescope, x-ray variability, 01 natural sciences, Spectral line, BL Lacertae objects, individual, Mrk 421, purl.org/becyt/ford/1 [https], Raigs gamma, emission, MAGIC (telescope), 010303 astronomy & astrophysics, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), individual: Mrk 421 [BL Lacertae objects], Galaxies: BL Lacertae objects: individual: Markarian 421, Spectral energy distribution, Electrónica, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, power spectra, BL Lacertae object, tev photons, 0103 physical sciences, Nucli galàctic actiu, bl lacertae objects: individual: mrk 421, Blazar, Astronomy and Astrophysics, Space and Planetary Science, Active galactic nuclei, 010308 nuclear & particles physics, light curves, Gamma rays, Institut für Physik und Astronomie, purl.org/becyt/ford/1.3 [https], Light curve, Galaxies, Galàxies, Astronomía, Crab Nebula, optical variability, active galactic nuclei, Galàxies actives, Active galaxies, markarian-421, ddc:520
Abstract

We performed a 4.5-month multi-instrument campaign (from radio to VHE gamma rays) on Mrk421 between January 2009 and June 2009, which included VLBA, F-GAMMA, GASP-WEBT, Swift, RXTE, Fermi-LAT, MAGIC, and Whipple, among other instruments and collaborations. Mrk421 was found in its typical (non-flaring) activity state, with a VHE flux of about half that of the Crab Nebula, yet the light curves show significant variability at all wavelengths, the highest variability being in the X-rays. We determined the power spectral densities (PSD) at most wavelengths and found that all PSDs can be described by power-laws without a break, and with indices consistent with pink/red-noise behavior. We observed a harder-when-brighter behavior in the X-ray spectra and measured a positive correlation between VHE and X-ray fluxes with zero time lag. Such characteristics have been reported many times during flaring activity, but here they are reported for the first time in the non-flaring state. We also observed an overall anti-correlation between optical/UV and X-rays extending over the duration of the campaign. The harder-when-brighter behavior in the X-ray spectra and the measured positive X-ray/VHE correlation during the 2009 multi-wavelength campaign suggests that the physical processes dominating the emission during non-flaring states have similarities with those occurring during flaring activity. In particular, this observation supports leptonic scenarios as being responsible for the emission of Mrk421 during non-flaring activity. Such a temporally extended X-ray/VHE correlation is not driven by any single flaring event, and hence is difficult to explain within the standard hadronic scenarios. The highest variability is observed in the X-ray band, which, within the one-zone synchrotron self-Compton scenario, indicates that the electron energy distribution is most variable at the highest energies., Comment: Accepted for publication in A&A, 18 pages, 14 figures (v2 has a small modification in the acknowledgments, and also corrects a typo in the field "author" in the metadata)

Published
2015
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65. Blind estimation of target parameters in the presence of unknown Gaussian space-time interference

Author

This work was supported by Russian Foundation of Basic Research, Grant 03-02-17035, and by the Grant of Russian Ministry of Industry and Science NSh-1641.2003.2., Rodionov, A. A.; Institute of Applied Physics of the Russian Academy of Sciences, Turchin, V. I.; Institute of Applied Physics of the Russian Academy of Sciences, This work was supported by Russian Foundation of Basic Research, Grant 03-02-17035, and by the Grant of Russian Ministry of Industry and Science NSh-1641.2003.2., Rodionov, A. A.; Institute of Applied Physics of the Russian Academy of Sciences, and Turchin, V. I.; Institute of Applied Physics of the Russian Academy of Sciences

Abstract

Parametric estimation technique for deterministic space-time signals on the output of linear sensor array in the presence of Gaussian noise with unknown second moment is considered. For this scenario, the derived maximum-likelihood statistics becomes invariant with respect to the second moment of noise and can be termed as blind estimator. Proposed technique was experimentally examined via estimation of track parameters for moving scatterer. It was shown for numerous records that the blind and model-based estimation techniques have close performance, however, blind estimator does not require preliminary investigation of interference and designing of its statistical model.

Published
2005

66. An adaptive parametric estimation of space-time deterministic signal against unknown Gaussian noise background

Author

This work was supported by the Office of Naval Research., Rodionov, A. A.; Institute of Applied Physics of the Russian Academy of Sciences, Turchin, V. I.; Institute of Applied Physics of the Russian Academy of Sciences, This work was supported by the Office of Naval Research., Rodionov, A. A.; Institute of Applied Physics of the Russian Academy of Sciences, and Turchin, V. I.; Institute of Applied Physics of the Russian Academy of Sciences

Abstract

Parametric estimation technique for deterministic space-time signals on the output of linear sensor array in the presence of white Gaussian noise with unknown covariance matrix is considered. For this scenario, the derived maximum likelihood statistics become invariant with respect to the structure of noise covariance matrix, i.e., using of derived statistics corresponds exactly to adaptive array processing. It was found that in the simplest case of one source and factorized spatial and time components of deterministic signal, the statistic can be represented exactly as the combination of two trivial statistics: the first one corresponds to conventional time matched filtering and adaptive beamforming with the weight vector obtained from empirical covariance matrix of snapshots (i.e., from observed mixture of noise and deterministic component), and the second is the same statistic derived for unknown shape of steering vector. A stochastic numerical simulation showed that the statistic proposed eliminates some estimate bias appearing for the adaptive beamformer with inverse covariance matrix of snapshots.

Published
2003

67. Reflectivity of antenna and mirrors reflectors at 110 and 200 GHz

Author

The studies described were supported partly by INTAS program (project No. 01-2173) and by Russian State Programs: "Quantum and non-linear processes (project 1160)., Myasnikova, Svetlana E.; Applied Physics Institute, Russian Academy of Sciences, Nizhny Novgorod, Parshin, Vladimir V.; Applied Physics Institute, Russian Academy of Sciences, Nizhny Novgorod, Klooster, Kees van’t; European Space Agency, Valsecchi, Giuseppe; Media-Lario, The studies described were supported partly by INTAS program (project No. 01-2173) and by Russian State Programs: "Quantum and non-linear processes (project 1160)., Myasnikova, Svetlana E.; Applied Physics Institute, Russian Academy of Sciences, Nizhny Novgorod, Parshin, Vladimir V.; Applied Physics Institute, Russian Academy of Sciences, Nizhny Novgorod, Klooster, Kees van’t; European Space Agency, and Valsecchi, Giuseppe; Media-Lario

Abstract

Reflectivity (reflection loss) investigations of nickel samples with different types of surface finish, with and without rhodium coating, have been carried out in the 110-200 GHz frequency range on an installation developed in the Applied Physics Institute of Russia. The reflectivity measurements of high quality silver coated and gold coated mirrors are also presented. The reflectivity (reflection loss) investigations of some carbon fibre samples with and without aluminium coating have been made. Results are interesting, in view of the anisotropy of the carbon fibre material.

Published
2003

68. Оптимизация темпа роста тонких пленок сульфида кадмия электрохимических осаждений

Author

Демиденко Иван Владимирович, ГОУ ВПО «Приднестровский государственный университет им. Т.Г. Шевченко», Demidenko Ivan, The Department of solid-state electronics and microelectronics of Dniester State University, Tiraspol, Moldova., Вербина Анастасия, Verbina Anastasia, Ишимов Виктор, Ishimov Viktor, Белевский Станислав, Институт прикладной физики АНМ, Belevskii Stanislav, Institute of Applied Physics ASM, Демиденко Иван Владимирович, ГОУ ВПО «Приднестровский государственный университет им. Т.Г. Шевченко», Demidenko Ivan, The Department of solid-state electronics and microelectronics of Dniester State University, Tiraspol, Moldova., Вербина Анастасия, Verbina Anastasia, Ишимов Виктор, Ishimov Viktor, Белевский Станислав, Институт прикладной физики АНМ, Belevskii Stanislav, and Institute of Applied Physics ASM

Abstract

в данной работе показаны результаты исследования процесса осаждения сульфида кадмия из Aque-ОЕ электролита. В рамках полного факторного эксперимента (FFE) математическая модель зависимости между средним катодным ростом скорости CdS пленок и условий осаждения был построен. Была продемонстрирована взаимосвязь между эффективностью тока и осаждения таких факторов, как рН, температуры и концентрации электролита., the results of a study of the process of deposition of cadmium sulfide from an aqueous electrolyte were shown in this work. As part of the full factorial experiment (FFE), a mathematical modelof dependence between theaveragespeed growth cathode CdS films, and the deposition conditions was built. A relationshipbetween current efficiency and deposition factors such as pH, temperature and electrolyte concentration was demonstrated.

Published
2016

69. Identification of corrosion resistance different batches of the same brand austenitic fe- cr-ni alloys

Author

Snizhnoi, G. V.; Department of micro- and nanoelectronics, State Higher Education Establishment “Zaporizhzhya National Technical University”, 64, Zhukovskogo str., Zaporizhzhya, 69063, Ukraine, Snizhnoi, V. L.; Department of Applied Physics, State Higher Education Establishment “Zaporizhzhya National University”, 66, Zhukovskogo str., Zaporizhzhya, Snizhnoi, G. V.; Department of micro- and nanoelectronics, State Higher Education Establishment “Zaporizhzhya National Technical University”, 64, Zhukovskogo str., Zaporizhzhya, 69063, Ukraine, and Snizhnoi, V. L.; Department of Applied Physics, State Higher Education Establishment “Zaporizhzhya National University”, 66, Zhukovskogo str., Zaporizhzhya

Abstract

Purpose. Corrosion rate of different smelting of the one grade of austenite Fe-Cr-Ni alloy from the specific magnetic susceptibility of austenite experimentally determine. Austenitic Fe-Cr-Ni alloy of ferrite did not contain. The magnetic state of austenite specific magnetic susceptibility is determined. Methodology. Scales with unipolar astatic magnetic system and the prism engagement to locate the specific magnetic susceptibility used. The corrosion rate was determined of the relative weight lossK=m/(S). Aggressive solution "aqua regia" to accelerate the chemical corrosion of samples used. Findings. Corrosion rate alloys 06HN28MDT (EI943) by the magnetic state of the austenite (specific magnetic susceptibility) is defined. The corrosion rate isreduced if a specific magnetic susceptibility of austenite decreases, and vice versa. Originality. Correlation dependence of the corrosion rate and the specific magnetic susceptibility (magnetic state) austenite of different smelting of the one grade alloy EI943 revealed.. Practical value. The results for identification of the corrosion rate in the austenitic Fe-Cr-Ni alloys can be used., Цель. Экспериментально определить скорость коррозии разных плавок, но одной марки аустенитныхFe-Cr-Ni сплавов, не содержащих -феррит, по удельной магнитной восприимчивости аустенита, которая определяет магнитное состояние аустенита. Методика. Для нахождения удельной магнитной восприимчивости использовали весы с униполярной астатической системой и магнитным зацеплением призмы. Для выявления скорости коррозии использовали коэффициент интенсивности коррозии К, который определяли как относительную потерю массы K=m/(S). С целью ускорения химической коррозии исследуемые образцы помещали в агрессивный раствор "царская водка". Результаты.Установлено, что в пяти плавках сплава 06ХН28МДТ (ЭИ943) скорость коррозии определяется магнитным состоянием аустенита, т.е. удельной магнитной восприимчивостью: чем меньше удельная магнитная восприимчивость аустенита, тем меньше скорость коррозии и наоборот. Научная новизна. Выявлена корреляционная зависимость скорости коррозии от удельной магнитной восприимчивости, т.е. магнитного состояния аустенита разных плавок, но одной марки сплава ЭИ943. Практическая значимость. Полученные результаты могут быть использованы для идентификации скорости коррозии в аустеннитных Fe-Cr-Ni сплавах., Мета. Експериментально визначити швидкість корозії різних плавок, але однієї марки аустенітних Fe-Cr-Niсплавів, що не містять -ферит, за питомою магнітної сприйнятливістю аустеніту, яка визначає магнітний стан аустеніту. Методика. Для знаходження питомої магнітної сприйнятливості використовували терези з уніполярною астатичноюсистемою і магнітним зчепленням призми. Для виявлення швидкості корозії використовували коефіцієнт інтенсивності корозії К, який визначали як відносну втрату маси K=m/(S). З метою прискорення хімічної корозії досліджувані зразки поміщали в агресивний розчин "царська горілка". Результати. Встановлено, що в п'яти плавках сплаву 06ХН28МДТ (ЭИ943) швидкість корозії визначається магнітним станом аустеніту, тобто питомої магнітною сприйнятливістю: чим менше питома магнітна сприйнятливість аустеніту, тим менше швидкість корозії і навпаки. Наукова новизна. Виявлено кореляційну залежність швидкості корозії від питомої магнітної сприйнятливості, тобто магнітного стану аустеніту різних плавок, але однієї марки сплаву ЕІ943. Практична значимість. Отримані результати можуть бути використані для ідентифікації швидкості корозії в аустеннітних Fe-Cr-Ni сплавах.

Published
2016

70. PHOTOINDUCED IRREVERSIBLE EFFECTS ON MAGNETIC PROPERTIES AND ALLIED PHENOMENA IN MAGNETIC OXIDES X

Author

K., HISATAKE, I., MATSUBARA, K., MAEDA, T., MIYAZAKI, S., KAINUMA, K., UEMATSU, Department of Physics, Kanagawa Dental College, Department of Applied Physics, Tohoku University, Department of Electrical Engineering, Ashikaga Institute of Technplogy, and Advanced Research Institute for Science and Engineering, Waseda University Shinjyukuku

Abstract

This is a review which concerns with mainly the relaxation phenomena in permeability of magnetic oxides. In addition the study is, however, reported in our laboratory in 1997,which was in press. In single crystals of yttrium iron garnet irradiated with an intense visible light at 77K, a remarkable change of the temperature dependence of complex permeabilities μ' and μ" is observed. Simultaneously, conspicuous double peaks of photoinduced disaccommodation, DA around 130 K(DA(I)) and 200 K(DA(II)) were found, with correlative onset of the irreversible decrease of μ' at low temperature. Activation energies of these peaks are estimated 0.46eV for DA(I) and 0.7 eV for DA(II). In addition, we observed the third peak (DAIII, 0.88 eV), independent of irradiation around the room temperature. For an explanation of these results, a simple model is presented here for explaining these results. This review proposes also a new approach to studying the role of vacancy migration of YIG by the simple magnetic technique.

Published
1997

71. Diagnostics of receiving hydroacoustic antenna arrays

Author

The work was supported by Russian Foundation of Basic Research under Grant 96-15-96603., Orlov, Denis A.; Institute of Applied Physics of the Russian Academy of Sciences, Turchin, V. I.; Institute of Applied Physics of the Russian Academy of Sciences, The work was supported by Russian Foundation of Basic Research under Grant 96-15-96603., Orlov, Denis A.; Institute of Applied Physics of the Russian Academy of Sciences, and Turchin, V. I.; Institute of Applied Physics of the Russian Academy of Sciences

Abstract

Any experiment performed with the use of receiving hydroacoustic antenna arrays requires solving the important problem of determining their various characteristics after array deployment.Transfer coefficients of array hydrophones, that relate acoustic pressure at the hydrophone input with voltage at the output, are an example of such characteristics. After array deployment, these coefficients may differ considerably from the values measured under laboratory conditions (before array deployment). The problem of measurement of transfer coefficients of low-frequency arrays after array deployment has not been fully investigated. In the case of arrays with flexible or semi-rigid deployment, solution of the important problem of determining their profile in horizontal or vertical planes is needed. Besides for many applications in is necessary to estimate bottom parameters in the region of array deployment must be performed.To solve the problems mentioned, a complex method was developed. This method uses a source of tonal acoustic signal with changing frequency and a precise hydrophone with a known transfer coefficient. It is assumed that the transfer coefficients of array hydrophones are not considerably dependent on frequency, the source is monopole (its radiation level is the same in various directions) and the precise hydrophone has a uniform spatial beam pattern. The realization of the proposed method also enables to determine whether a multibeam substance model is suitable under natural conditions. In this model, an acoustic signal from a source of tonal signal is modeled as the sum of the direct signal and multiple reflections at the surface and bottom.

Published
1999

72. PHOTOINDUCED IRREVERSIBLE EFFECTS ON MAGNETIC PROPERTIES AND ALLIED PHENOMENA IN MAGNETIC OXIDES IX

Author

K., Hisatake, I., Matsubara, K., Maeda, T., Miyazaki, S., Kainuma, Department of Physics, Kanagawa Dental College, Department of Applied Physics, Tohoku University, and Ashikaga Institute of Technology

Abstract

In single crystals of yttrium iron garnet irradiated with laser (the most effective wavelength is 700nm) or white light at 77K, a remarkable change of the temperature dependence of complex permeabilities μ′ and μ″ is observed, which is peculiar to photoinduced magnetic effect. Simultaneously, conspicuous double peaks of DA around 125K and 200K below room temperature were found to be induced by light-irradiation, with correlative onset of the irreversible decrease of permeability insensitive to demagnetization at low temperature. The height of potential barrier around oxygen vacancy may be estimated 0.3eV. In order to explain these observations, we propose that oxygen defects provide a mechanism for occurrence of photomagnetic effects and discuss its validity; the review of these area of our laboratory in 1996 is given.

Published
1996

73. The optimization of chemical composition of heatproof basis of bimetallic purveyance

Author

Zolotarev, G. A.; Department of metal forming, Zaporizhia National Technical University, st. Zhukovskoho, 64, 69063, Zaporozhe, Ukraine., Sheyko, S. P.; Department of metal forming, Zaporizhia National Technical University, st. Zhukovskoho, 64, 69063, Zaporozhe, Ukraine., Mishchenko, V. G.; Department of applied physics, Zaporizhia National University, st. Zhukovskoho, 66, 69600, Zaporozhe, Ukraine., Zolotarev, G. A.; Department of metal forming, Zaporizhia National Technical University, st. Zhukovskoho, 64, 69063, Zaporozhe, Ukraine., Sheyko, S. P.; Department of metal forming, Zaporizhia National Technical University, st. Zhukovskoho, 64, 69063, Zaporozhe, Ukraine., and Mishchenko, V. G.; Department of applied physics, Zaporizhia National University, st. Zhukovskoho, 66, 69600, Zaporozhe, Ukraine.

Abstract

Purpose. Progressive material for the reactor can be a bimetal, consisting of a mild steel with an inner side of the tread and the reactor refractory basis - the outer. It is necessary to establish the influence of the degree of alloying patterns on the mechanical properties of experimental steel in the upper and lower limit of the content of alloying elements in the steel. Methodology. Analysis of the impact of carbon, chromium and nickel on mechanical properties of steel was studied using statistical method of planning of active experiment. As a response function took tensile strength ав and yield strength 00,2. Mathematical processing of the experimental data in order to construct a mathematical model of the influence of chemical composition on the properties of the steel was carried out by methods using regression analysis. To reduce the number of experiments and assuming the nonlinear nature of the response functions used in symmetric composite design of the second order. Findings. Reactor operating temperature of titanium sponge production with magnesium are 850...1020 ° C, and it is important to determine the effect of selected alloying complex on short-term strength at the maximum operating temperature with the aid of mathematical planning of the experiment. Intervals varying factors selected on the basis of preliminary information: experimental and literature data on the effect of alloying elements on the properties of chromium-nickel steel, mechanical properties in the initial state. As a result of mathematical planning of regression equations were obtained in full size to optimize the chemical composition of low-carbon steel. To assess the adequacy of the equations was calculated by regression equations obtained for the ground level of the chemical composition of the steel. The calculation results were compared with experimental studies. The error between the calculated and experimental values of the response function does not exceed 2%. To determine the, Цель. Прогрессивным материалом для изготовления реакторов может быть биметалл, состоящий из низкоуглеродистой стали в виде протектора с внутренней стороны реактора и жаропрочной основы - с наружной. Необходимо установить закономерности влияния степени легирования на механические свойства опытной стали на верхнем и нижнем пределе содержания легирующих элементов в стали. Методика. Анализ влияния углерода, хрома и никеля на механические свойства стали изучали с использованием статистического метода планирования активного эксперимента. В качестве функции отклика принимали предел прочности ав и предел текучести 00,2. Математическую обработку экспериментальных данных с целью построения математической модели влияния химического состава на свойства стали проводили по методикам с применением регрессионного анализа. Для сокращения числа опытов и предполагая нелинейный характер функций отклика в работе использовали симметричный композиционный план второго порядка. Результаты. Рабочие температуры реакторов магнийтермического производства губчатого титана составляют 850...1020 °С, и важно определить влияние выбранного легирующего комплекса на кратковременную прочность при максимальной рабочей температуре с помощью математического планирования эксперимента. Интервалы варьирования факторов выбирали на основании предварительной информации: экспериментальные и литературные данные о влиянии легирующих элементов на свойства хромоникелевых сталей, механические свойства в исходном состоянии. В результате математического планирования получены регрессионные уравнения в натуральных величинах для оптимизации химического состава низкоуглеродистой стали. Для оценки адекватности уравнений был проведен расчет по полученным уравнениям регрессии для основного уровня химического состава стали. Результаты расчетов были сопоставлены с экспериментальными исследованиями. Погрешность между расчетными и экспериментальными значениями функции отклика не превышает 2%. Для определения химического состава об, Мета. Прогресивним матеріалом для виготовлення реакторів може бути біметал, що складається з низьковуглецевої сталі у вигляді протектора з внутрішньої сторони реактора і жароміцної основи - із зовнішнього. Необхідно встановити закономірності впливу ступеня легування на механічні властивості дослідної сталі на верхньому і нижньому межі вмісту легуючих елементів в сталі. Методика. Аналіз впливу вуглецю, хрому і нікелю на механічні властивості сталі вивчали з використанням статистичного методу планування активного експерименту. Як функції відгуку брали межу міцності ав і межа плинності 00,2. Математичну обробку експериментальних даних з метою побудови математичної моделі впливу хімічного складу на властивості сталі проводили за методиками із застосуванням регресійного аналізу. Для скорочення числа дослідів і припускаючи нелінійний характер функцій відгуку в роботі використовували симетричний композиційний план другого порядку. Результати. Робочі температури реакторів магнійтермічного виробництва губчастого титану становлять 850...1020 °С, і важливо визначити вплив обраного легуючого комплексу на короткочасну міцність при максимальній робочій температурі за допомогою математичного планування експерименту. Інтервали варіювання факторів вибирали на підставі попередньої інформації: експериментальні та літературні дані про вплив легуючих елементів на властивості хромонікелевих сталей, механічні властивості в початковому стані. В результаті математичного планування отримані регресійні рівняння в натуральних величинах для оптимізації хімічного складу низьковуглецевої сталі. Для оцінки адекватності рівнянь було проведено розрахунок за отриманими рівняннями регресії для основного рівня хімічного складу сталі. Результати розрахунків були зіставлені з експериментальними дослідженнями. Похибка між розрахунковими і експериментальними значеннями функції відгуку не перевищує 2%. Для визначення хімічного складу забезпечує отримання оптимальних механічних властивостей ав і 00,2 сталі т

Published
2015

76. Increasing the healing rate of skin wounds

Author

Tipa, R.S., Kroesen, G.M.W., M. Hori, W.G. Graham, Japan Society of Applied Physics, xx, and Elementary Processes in Gas Discharges

Abstract

No abstract.

Published
2010

77. Feather-like structures in positive streamers

Author

Wormeester, G., Nijdam, S., Ebert, U.M., M. Hori, W.G. Graham, Japan Society of Applied Physics, xx, and Elementary Processes in Gas Discharges

Abstract

only.

Published
2010

79. Atomic hydrogen densities in expanding thermal plasmas

Author

Welzel, S., van Zon, P.A.C., van den Bos, R.A.J.M., Harskamp, van, W.E.N., Schram, D.C., Sanden, van de, M.C.M., Engeln, R.A.H., M. Hori, W.G. Graham, Japan Society of Applied Physics, xx, Plasma & Materials Processing, and Plasma-based gas conversion

Abstract

only.

Published
2010

80. A versatile method to grow localized arrays of nanowires for highly sensitive capacitive devices

Author

Antohe, Vlad, Radu, A., Yunus, Sami, Attout, Anne, Bertrand, Patrick, Mátéfi-Tempfli, Maria-Rita, Piraux, Luc, Mátéfi-Tempfli, Stefan, 9th International Balkan Workshop on Applied Physics, and UCL - FSA/MAPR - Département des sciences des matériaux et des procédés

Subjects
Alumina Templates, Nanowires, Polyaniline, Electrochemical Synthesis, Ph Sensors
Abstract

We propose a new approach to increase the detection efficiency of the capacitive sensing devices, by growing vertically aligned nanowires arrays, localized and confined on small interdigited electrodes structures. The metallic tracks are made using optical lithography, and the nanowires are realized by electrochemical synthesis in nanoporous materials (i.e. supported alumina templates). By controlling the preparation conditions, both their positions and pitches can be easily tuned, as well as their geometrical design (i.e. diameters between 5 - 350 nm and lengths between 150 nm - 10 mu m). Based on these considerations, a capacitive sensor structure with high active surface is sensitized with polyaniline, for pH detection. Reported data show that the sensitivity of the sensor is substantially improved by using nanowires arrays.

Published
2008

81. IAP Annual Report 2005

Author

ETH Zurich, Institute of Applied Physics (IAP)

Subjects
musculoskeletal diseases, body regions, viruses, biological phenomena, cell phenomena, and immunity
Abstract

IAP Annual Report

Published
2006

82. IAP Annual Report 2004

Author

ETH Zurich, Institute of Applied Physics (IAP)

Subjects
musculoskeletal diseases, body regions, viruses, biological phenomena, cell phenomena, and immunity
Abstract

IAP Annual Report

Published
2005
Full Text
View/download PDF

83. IAP Annual Report 2003

Author

ETH Zurich, Institute of Applied Physics (IAP)

Subjects
musculoskeletal diseases, body regions, viruses, biological phenomena, cell phenomena, and immunity
Abstract

IAP Annual Report

Published
2004

84. Polyfibroblast Phase 4: A Self-Healing and Galvanic Protection Additive

Author

JOHNS HOPKINS UNIV LAUREL MD APPLIED PHYSICS LAB, Benkoski, Jason J, JOHNS HOPKINS UNIV LAUREL MD APPLIED PHYSICS LAB, and Benkoski, Jason J

Abstract

The goal of this project is to develop a primer additive that mimics the self-healing ability of skin by forming a polymer scar across scratches. Designed to work with existing military grade primers, Polyfibroblast consists of microscopic, hollow zinc tubes filled with a moisture-cured polyurethane-urea (MCPU). When scratched, the foaming action of a propellant ejects the resin from the broken tubes and completely fills the crack. No catalysts or curing agents are needed since the polymerization is driven by ambient humidity.

Published
2014

85. Multijunction Solar Cell Efficiencies: Effect of Spectral Window, Optical Environment and Radiative Coupling

Author

CALIFORNIA INST OF TECH PASADENA T J WATSON LABS OF APPLIED PHYSICS, Eisler, Carissa N, Abrams, Ze'ev R, Sheldon, Matthew T, Zhang, Xiang, Atwater, Harry A, CALIFORNIA INST OF TECH PASADENA T J WATSON LABS OF APPLIED PHYSICS, Eisler, Carissa N, Abrams, Ze'ev R, Sheldon, Matthew T, Zhang, Xiang, and Atwater, Harry A

Abstract

Solar cell efficiency is maximized through multijunction architectures that minimize carrier thermalization and increase absorption. Previous proposals suggest that the maximum efficiency for a finite number of subcells is achieved for designs that optimize for light trapping over radiative coupling. We instead show that structures with radiative coupling and back reflectors for light trapping, e.g. spectrum-splitting cells, can achieve higher conversion efficiencies. We model a compatible geometry, the polyhedral specular reflector. We analyze and experimentally verify the effects of spectral window and radiative coupling on voltage and power. Our results indicate that radiative coupling with back reflectors leads to higher efficiencies than previously studied architectures for practical multijunction architectures (i.e., or = 20 subcells)., Published in Energy & Environmental Science, 10.1039/c4ee01060d, 2014.

Published
2014

86. Refining an Automated Transcranial Doppler System for the Detection of Vasospasm after Traumatic Brain Injury

Author

WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, Mourad, Pierre D, WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, and Mourad, Pierre D

Abstract

Traumatic brain injury (TBI) is a major contributor to morbidity and mortality experienced by those soldiers subjected to improvised explosive devices (IED) as well as in military and civilian high speed collisions. Traumatic cerebral vasospasm (TCV) is a major contributor to morbidity and mortality experienced by those TBI patients. Aggressive neurosurgical treatment motivated by early diagnosis appears to improve the clinical outcome for these patients. Early transcranial Doppler (TCD) measurements of blood flow speed within major cerebral arteries produces the initial diagnosis, hence motivates the rapid treatment of TCV. However, the skill necessary to deploy TCD limits its availability relative to its need. PhysioSonics, Inc, a local company in Seattle, created an automatic TCD system (called Presto or aTCD) that minimizes the skill necessary to perform TCD assays. Our long-term goal is to optimize Presto for patients in vasospasm, through optimization of its spectral Doppler envelope analyzer, its headset and supporting software so it can track blood flow in the internal carotid artery as well as middle cerebral artery., The original document contains color images.

Published
2014

87. Upper Ocean Stratification in the Bay of Bengal

Author

WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, D'Asaro, Eric, WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, and D'Asaro, Eric

Abstract

In collaboration with Indian oceanographers, we seek to measure and understand the processes controlling the stratification of the upper 100m of the Bay of Bengal and to educate a new generation of young Indian oceanographers in the methods used., The original document contains color images. Additional ONR contract N00014-10-1-0313.

Published
2014

88. Ocean Electric Field for Oceanography and Surveillance

Author

WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, Sanford, Thomas B, WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, and Sanford, Thomas B

Abstract

I have been an active member of the group of ONR SecNav/CNO Chairs in Oceanographic Sciences since being selected in 2008. The formal duration of the ONR Chairs grant was four years. For recent years, I have enjoyed no-cost extensions of this grant. I have continued to participate in Chairs meeting with the multiple Chiefs of Naval Research. These meetings are occasions for the Chairs to learn about ONR concerns and provide feedback on issues, such as opportunities and priorities for Arctic Ocean research. I will continue to participate at the pleasure of ONR. The accomplishments of this grant include support of two graduate students, Kevin Taylor and Nathan Lauffenburger, whom I supervised. Both were awarded MS degrees by the UW School of Oceanography and are currently employed in ocean studies at APL-JHU and NOAA, respectively. These students participated in and used data from ONR DRI projects, including QPEU for Taylor and OKMC for Lauffenburger.

Published
2014

89. The Importance of Neurogenic Inflammation in Blast-Induced Neurotrauma

Author

JOHNS HOPKINS UNIV LAUREL MD APPLIED PHYSICS LAB, Wester, Brock, Schaefer, Michele, Boggs, Nathan, Bradburne, Chris, JOHNS HOPKINS UNIV LAUREL MD APPLIED PHYSICS LAB, Wester, Brock, Schaefer, Michele, Boggs, Nathan, and Bradburne, Chris

Abstract

This study investigates the role of blood-borne immune cells as important mediators of damage and neuropathology resulting from blast-induced neurotrauma (BINT). We hypothesized that macrophages, along with their secreted cytokines and chemokines from the periphery, migrate via blood and infiltrate the CNS where they contribute to neuronal damage caused by activated microglia both in acute and chronic injury phases of BINT. We have used MRI and molecular techniques in mice with mild/moderate blast injury generated in a compressed helium-driven shock tube, as well as measurements of motor performance and behavioral assessment, observed temporally over 1 month. Groups of animals with mild/moderate BINT are imaged (MRI) and validated by immunocytochemistry, to visualize potential macrophage infiltration; blood-brain barrier (BBB) disturbance; reactive gliosis; or astrocyte activation. We show that a single exposure to mild/moderate blast induces both acute and chronic glial activation, levels of cytokines/chemokines, and motor impairment., The original document contains color images.

Published
2014

90. Verification-Based Model Tuning

Author

WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, Marzban, Caren, Jones, David W, Sandgathe, Scott A, WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, Marzban, Caren, Jones, David W, and Sandgathe, Scott A

Abstract

All numerical models (e.g., Numerical Weather Prediction models) have certain parameters within model algorithms which effect forecasts to a different degree, depending on the forecast quantity. The specific values of these model parameters are determined either theoretically using fundamental physics laws but incorporating necessary approximations to reduce computational cost, or empirically using observations from field experiments where observational error introduces uncertainty. In either case, the exact value of the parameter is often unknown a priori, and so their values are usually set to improve forecast quality through some form of forecast verification. Such an approach to model tuning, however, requires knowledge of the observations to which the forecasts must be compared, and therefore, a multitude of highly detailed experimental cases in order to fully resolve parameter values, a data set very difficult to obtain. A knowledge of the relationship between model parameters and forecast quantities, without reference to observations, can not only aid in such an observation-based approach to model tuning, it can also aid in tuning the model parameters according to other criteria that may not be based on observations directly, e.g., a desire to affect the forecasts according to some long-term experience of a forecaster. The main goal of our work has been to develop a framework for representing the complex relationship between model parameters and forecast quantities, without any reference to observations., The original document contains color images.

Published
2014

91. Influence of electric spark on hardness of carbon steel

Author

Vakulenko, I. O.; Dep. «Materials Technology», Dnipropetrovsk National University of Railway Transport named after Academician V. Lazaryan, Lazaryan St., 2, Dnipropetrovsk, Ukraine, 49010, tel. +38 (056) 373 15 56, e-mail dnyzt_texmat@ukr.net, Proydak, S. V.; Dep. «Materials Technology», Dnipropetrovsk National University of Railway Transport named after Academician V. Lazaryan, Lazaryan St., 2, Dnipropetrovsk, Ukraine, 49010, tel. +38 (056) 373 15 56, e-mail dnyzt_texmat@ukr.net, Stradomski, Z.; Fac. «Technology of Materials Processing and Applied Physics of Institute of Engineering Material Science», Czestochowa University of Technology, al. Armi Krajowej, 19, Czestochowa, Poland, 42-200, tel.+48 (34) 325 07 38, e-mail zbigniew@wip.pcz.pl, Diadko, V. A.; Dep. «Materials Technology», Dnipropetrovsk National University of Railway Transport named after Academician V. Lazaryan, Lazaryan St., 2, Dnipropetrovsk, Ukraine, 49010, tel. +38 (056) 373 15 56, e-mail dnyzt_texmat@ukr.net, Vakulenko, I. O.; Dep. «Materials Technology», Dnipropetrovsk National University of Railway Transport named after Academician V. Lazaryan, Lazaryan St., 2, Dnipropetrovsk, Ukraine, 49010, tel. +38 (056) 373 15 56, e-mail dnyzt_texmat@ukr.net, Proydak, S. V.; Dep. «Materials Technology», Dnipropetrovsk National University of Railway Transport named after Academician V. Lazaryan, Lazaryan St., 2, Dnipropetrovsk, Ukraine, 49010, tel. +38 (056) 373 15 56, e-mail dnyzt_texmat@ukr.net, Stradomski, Z.; Fac. «Technology of Materials Processing and Applied Physics of Institute of Engineering Material Science», Czestochowa University of Technology, al. Armi Krajowej, 19, Czestochowa, Poland, 42-200, tel.+48 (34) 325 07 38, e-mail zbigniew@wip.pcz.pl, and Diadko, V. A.; Dep. «Materials Technology», Dnipropetrovsk National University of Railway Transport named after Academician V. Lazaryan, Lazaryan St., 2, Dnipropetrovsk, Ukraine, 49010, tel. +38 (056) 373 15 56, e-mail dnyzt_texmat@ukr.net

Abstract

Purpose. The purpose of work is an estimation of influence of an electric spark treatment on the state of mouldable superficial coverage of carbon steel. Methodology. The steel of fragment of railway wheel rim served as material for research with chemical composition 0.65% С, 0.67% Mn, 0.3% Si, 0.027% P, 0.028% S. Structural researches were conducted with the use of light microscopy and methods of quantitative metallography. The structural state of the probed steel corresponded to the state after hot plastic deformation. The analysis of hardness distribution in the micro volumes of cathode metal was carried out with the use of microhardness tester of type of PMT-3. An electric spark treatment of carbon steel surface was executed with the use of equipment type of EFI-25M. Findings. After electric spark treatment of specimen surface from carbon steel the forming of multi-layered coverage was observed. The analysis of microstructure found out the existence of high-quality distinctions in the internal structure of coverage metal, depending on the probed area. The results obtained in the process are confirmed by the well-known theses, that forming of superficial coverage according to technology of electric spark is determined by the terms of transfer and crystallization of metal. The gradient of structures on the coverage thickness largely depends on development of structural transformation processes similar to the thermal character influence. Originality. As a result of electric spark treatment on the condition of identical metal of anode and cathode, the first formed layer of coverage corresponds to the monophase state according to external signs. In the volume of coverage metal, the appearance of carbide phase particles is accompanied by the decrease of microhardness values. Practical value. Forming of multi-layered superficial coverage during electric spark treatment is accompanied by the origin of structure gradient on a thickness. The effect of the superficial work, Цель. Целью работы является оценка влияния электрической искровой обработки на состояние формирующегося поверхностного покрытия углеродистой стали. Методика. Материалом для исследования служила сталь фрагмента обода железнодорожного колеса с химическим составом 0,65% С, 0,67% Mn, 0,3% Si, 0,027% P, 0,028% S. Структурные исследования проводились с использованием световой микроскопии и методик количественной металлографии. Структурное состояние исследуемой стали соответствовало состоянию после горячей пластической деформации. Анализ распределения твердости в микрообъемах металла катода осуществляли с использованием микротвердомера типа ПМТ-3. Электрическую искровую обработку поверхности углеродной стали выполняли с использованием оборудования типа ЭФИ-25М. Результаты. После электрической искровой обработки поверхности образца из углеродистой стали наблюдали формирование многослойного покрытия. Анализ микроструктуры показал существование качественных различий во внутреннем строении металла покрытия в зависимости от исследуемого участка. Полученные в работе результаты подтверждают известные положения, что формирование поверхностного покрытия по технологии электрического искрового разряда определяется условиями переноса и кристаллизации металла. Градиент структур по толщине покрытия в значительной степени зависит от развития процессов структурных превращений, подобных влиянию термического характера. Научная новизна. В результате электрической искровой обработки, при условии одинакового металла анода и катода, сформированная первая прослойка покрытия по внешним признакам соответствует однофазному состоянию. В объеме металла покрытия появление частиц карбидной фазы сопровождается снижением значений микротвердости. Практическая значимость. Формирование многослойного поверхностного покрытия при электрической искровой обработке сопровождается возникновением градиента структур по толщине. По уровню эффект поверхностного упрочнения от искрового разряда может быть альтернативой, Мета. Метою роботи є оцінка впливу електричної іскрової обробки на стан поверхневого нашарування вуглецевої сталі, що формується. Методика. Матеріалом для дослідження була сталь фрагменту ободу залізничного колеса з хімічним складом 0,65% С, 0,67% Mn, 0,3% Si, 0,027% P, 0,028% S. Структурні дослідження проводилися з використанням світлової мікроскопії й методик кількісної металографії. Структурний стан досліджуваної сталі відповідав стану після гарячої пластичної деформації. Аналіз розподілу мікротвердості в мікрооб’ємах металу катоду проводили з використанням мікротвердоміра типу ПМТ-3. Електричну іскрову обробку поверхні вуглецевої сталі виконували з використанням устаткування типу ЕФІ-25М. Результати. Після електричної іскрової обробки поверхні зразка вуглецевої сталі спостерігали формування багатошарового покриття. Аналіз мікроструктури показав існування якісних розбіжностей у внутрішній будові металу покриття в залежності від ділянки, яка досліджується. Отримані в роботі результати підтверджують відомі положення, що формування поверхневого покриття за технологією електричного іскрового розряду визначається умовами переносу й кристалізації металу. Градієнт структур по товщині покриття значною мірою обумовлений розвитком процесів структурних перетворень подібних впливові термічного характеру. Наукова новизна. У результаті електричної іскрової обробки, за умов однакового металу аноду і катоду, сформований перший прошарок покриття за зовнішніми ознаками відповідає однофазному стану. В об’ємі металу покриття поява часток карбідної фази супроводжується зниженням значень твердості. Практична значимість. Формування багатошарового поверхневого покриття при електричній іскровій обробці супроводжується виникненням градієнту структур за його товщиною. За досягненим рівнем ефект поверхневого зміцнення від іскрового розряду може бути конкурентоспроможним більшості термічних та хіміко-термічних технологій обробки поверхні металевих матеріалів.

Published
2014

92. IAP Annual Report 2002

Author

ETH Zurich, Institute of Applied Physics (IAP)

Subjects
musculoskeletal diseases, body regions, viruses, biological phenomena, cell phenomena, and immunity
Abstract

IAP Annual Report

Published
2003
Full Text
View/download PDF

93. IAP Annual Report 2001

Author

ETH Zurich, Institute of Applied Physics (IAP)

Subjects
musculoskeletal diseases, body regions, viruses, biological phenomena, cell phenomena, and immunity
Abstract

IAP Annual Report

Published
2002

94. IAP Annual Report

Author

ETH Zurich, Institute of Applied Physics (IAP)

Subjects
musculoskeletal diseases, body regions, viruses, Physics, biological phenomena, cell phenomena, and immunity, ELEKTRONISCHE ZEITSCHRIFTEN + ELEKTRONISCHE SCHRIFTENREIHEN (DOKUMENTENTYP), ELECTRONIC JOURNALS + ONLINE SERIALS (DOCUMENT TYPES)
Abstract

IAP Annual Report

Published
2002
Full Text
View/download PDF

95. ONR Progress Report: 2013 Contract

Author

WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, Wensnahan, Mark, WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, and Wensnahan, Mark

Abstract

This contract covers the processing and analysis of US Navy submarine measurements of sea-ice draft in the Arctic. Work in 2013 under this grant consisted of 4 basic tasks: (a) a regression analysis of the effect of ship depth and speed on mean draft and other statistics, (b) development of software to process both digital and analog data, (c) processing and analysis of data from two cruises in 2011 and (d) beginning processing of older analog data.

Published
2013

96. Wavefront Intensity Statistics for 284-Hz Broadband Transmissions to 107-km Range in the Philippine Sea: Observations and Modeling

Author

WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, White, Andrew W, Andrew, Rex K, Mercer, James A, Worcester, Peter F, Dzieciuch, Matthew A, Colosi, John A, WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, White, Andrew W, Andrew, Rex K, Mercer, James A, Worcester, Peter F, Dzieciuch, Matthew A, and Colosi, John A

Abstract

In the spring of 2009, broadband transmissions from a ship-suspended source with a 284-Hz center frequency were received on a moored and navigated vertical array of hydrophones over a range of 107 km in the Philippine Sea. During a 60-h period over 19 000 transmissions were carried out. The observed wavefront arrival structure reveals four distinct purely refracted acoustic paths: One with a single upper turning point near 80m depth, two with a pair of upper turning points at a depth of roughly 300 m, and one with three upper turning points at 420 m. Individual path intensity, defined as the absolute square of the center frequency Fourier component for that arrival, was estimated over the 60-h duration and used to compute scintillation index and log-intensity variance. Monte Carlo parabolic equation simulations using internal-wave induced sound speed perturbations obeying the Garrett-Munk internal-wave energy spectrum were in agreement with measured data for the three deeper-turning paths but differed by as much as a factor of four for the near surface-interacting path., The original document contains color images. Pub. in the Journal of Acoustical Society of America, v134 n4, p3347-3358, Oct 2013.

Published
2013

97. Flight Software Development for the Liberdade Flying Wing Glider

Author

WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, Brodsky, Peter, Luby, Jim, WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, Brodsky, Peter, and Luby, Jim

Abstract

This report covers work carried out under both the above ONR grant and a previous grant (N00014-05-1-0209) logically connected to the same program. This program concerned development of a computer control system for a very large underwater glider. In addition, APUUW partnered closely with the Scripps Institution of Oceanography who developed the vehicle hardware. A copy of the equivalent final report from Scripps is attached to this report as it covers work performed by both institutions in successful operation of the glider., The original document contains color images.

Published
2013

98. Understanding Chemical Sensitivity and Surface Response in Detecting Trace Levels of Explosives Using Vibrational Sum Frequency Spectroscopy

Author

WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, Asher, William E, WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, and Asher, William E

Abstract

Vibrational sum frequency spectroscopy (VSFS) can be used to detect trace quantities of high explosives (HEs) adsorbed on surfaces. As a trace detection method, VSFS has the advantages of being non-contact and non-destructive with sub-second detection times. Therefore, a HE-detection method for detecting IEDs or portal defense that was based on VSFS could provide stand-off trace detecting for IEDs and increase the throughput of package screening (in terms of objects scanned per minute) for portal defense. Furthermore, because VSFS does not degrade contaminants on surfaces, a positive detection result leaves any explosives detected in place for subsequent forensic analysis such as fingerprint identification. This research has shown that that VSFS provides high chemically selectivity for nitro-containing HEs in the presence of environmental chemical contamination., The original document contains color images.

Published
2013

99. Transport Theory for Propagation and Reverberation

Author

WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, Thorsos, Eric I, WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, and Thorsos, Eric I

Abstract

The main goals proposed for this project were to extend transport theory to range dependent environments and to develop reverberation modeling based on transport theory. The stochastic process emphasized was forward scattering from the sea surface, since it is the most important effect on reverberation modeling that is not being taken into account in reverberation modeling prediction for naval applications. The effect of sea surface forward scattering can affect predicted reverberation levels at mid frequencies by more than 10 dB, and therefore it is one of very few physical effects (if not the only one) not presently being taken into account that can lead to such large reverberation modeling uncertainties. The need to account for surface forward scattering with traditional reverberation modeling approaches readily accessable for naval applications is also being addressed with the development of an effective reflection loss model for the total field, referred to as TOTLOS. The original approach in developing TOTLOS was to base it on the results of Monte Carlo rough surface PE results, but as transport theory became available it became clear that results from it were much more suitable to support TOTLOS development, making it an important secondary goal of the present project., The original document contains color images.

Published
2013

100. Atmospheric Profiles, Clouds, and the Evolution of Sea Ice Cover in the Beaufort and Chukchi Seas Atmospheric Observations and Modeling as Part of the Seasonal Ice Zone Reconnaissance Surveys

Author

WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, Schweiger, Axel, Lindsay, Ron, Zhang, Jinlun, Liu, Zheng, Lawrence, Dale A, Maslanik, James, WASHINGTON UNIV SEATTLE APPLIED PHYSICS LAB, Schweiger, Axel, Lindsay, Ron, Zhang, Jinlun, Liu, Zheng, Lawrence, Dale A, and Maslanik, James

Abstract

The goal of this project is to examine the role of sea-ice and atmospheric interactions in the retreat of the SIZ. As sea ice retreats further, changes in lower atmospheric temperature, humidity, winds, and clouds are likely to result from changed sea ice concentrations and ocean temperatures. These changes in turn will affect the evolution of the SIZ. An appropriate representation of this feedback loop in models is critical if we want to advance prediction skill in the SIZ. To do so, we will conduct a combination of targeted measurements and modeling experiments as part of the atmospheric component of the Seasonal Ice Zone Reconnaissance Survey project (SIZRS). Objectives: * Determine the role of changing atmospheric properties in modifying the evolution of the SIZ in the Beaufort and Chukchi Seas from spring through fall. * Determine how changes in sea ice and sea surface conditions in the SIZ affect changes in cloud properties and cover. * Determine the role additional atmospheric profile observations may play in improving the quality of weather forecasts and ice predictions for the SIZ of the Beaufort and Chukchi Seas. * Adapt a low cost, expendable, air-deployed micro-aircraft to obtain temperature and humidity profiles and cloud top and base heights., Prepared in cooperation with Department of Aerospace Engineering, University of Colorado, Boulder, CO.

Published
2013

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