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Secondary Component (secondary + component)

Distribution by Scientific Domains

Physics and Astronomy	69%

Selected Abstracts

Progressive edge detection compression for fingerprint images

INTERNATIONAL JOURNAL OF IMAGING SYSTEMS AND TECHNOLOGY, Issue 5 2002
Awad K. Al-Asmari
In this article, a progressive fingerprint image compression (for storage or transmission) that uses an edge detection scheme is developed. First, the image is decomposed into two components: the primary component, which contains the edges, and the secondary component, which contains the textures and the features. Then, a general grasp for the image is reconstructed in the first stage at bit rates of 0.0223 and 0.0245 bpp for the tested fingerprints images (samples 1 and 2), respectively. The quality of the reconstructed images is competitive with the 0.75-bpp target bit set by the FBI standard. Also, the compression ratio and the image quality of this algorithm are competitive with other methods reported in the literature. The compression ratio for our algorithm is about 45:1 (0.180 bpp). © 2003 Wiley Periodicals, Inc. Int J Imaging Syst Technol 12, 211,216, 2002; Published online in Wiley InterScience (www.interscience.wiley.com). DOI 10.1002/ima.10025 [source]

H, long-term monitoring of the Be star , Cephei Aa

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Issue 2 2008
G. Catanzaro
ABSTRACT Papers published in recent years have contributed to resolve the enigma of the hypothetical Be nature of the hot pulsating star , Cephei. This star shows variable emission in the H, line, typical for Be stars, but its projected rotational velocity is very much lower than the critical limit, contrary to what is expected for a typical Be star. The emission has been attributed to the secondary component of the , Cephei spectroscopic binary system. In this paper, using both our and archived spectra, we attempt to recover the H, profile of the secondary component and to analyse its behaviour with time for a long period. To accomplish this task, we first derive the atmospheric parameters of the primary, Teff= 24 000 ± 250 K and log g= 3.91 ± 0.10, and then we use these values to compute its synthetic H, profile, and finally we reconstruct the secondary's profile disentangling the observed one. The secondary's H, profile shows the typical two-peak emission of a Be star with a strong variability. We also analysed the behaviour versus time of some linewidth parameters: equivalent width, ratio of blue to red peak intensities, full width at half-maximum, peak separation and radial velocity of the central depression. The projected rotational velocity (v sin i) of the secondary and the dimension of the equatorial surrounding disc have also been estimated. [source]

Physical parameters of the O6.5V+B1V eclipsing binary system LS 1135

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Issue 4 2006
E. Fernández Lajús
ABSTRACT The ,All Sky Automated Survey' (ASAS) photometric observations of LS 1135, an O-type single-lined binary (SB1) system with an orbital period of 2.7 d, show that the system is also eclipsing performing a numerical model of this binary based on the Wilson,Devinney method. We obtained an orbital inclination . With this value of the inclination, we deduced masses M1, 30 ± 1 M, and M2, 9 ± 1 M,, and radii R1, 12 ± 1 R, and R2, 5 ± 1 R, for primary and secondary components, respectively. Both the components are well inside their respective Roche lobes. Fixing the Teff of the primary to the value corresponding to its spectral type (O6.5V), the Teff obtained for the secondary component corresponds approximately to a spectral type of B1V. The mass ratio M2/M1, 0.3 is among the lowest known values for spectroscopic binaries with O-type components. [source]

On the orbital period modulation of RS CVn binary systems

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Issue 1 2005
Antonino F. Lanza
ABSTRACT The Applegate hypothesis proposed to explain the orbital period modulation of RS Canum Venaticorum (RS CVn) close binaries (Applegate 1992) is considered in the framework of a general model to treat the angular momentum exchanges within the convective envelope of a magnetically active star. This model assumes that the convection zone is strictly adiabatic and that the Taylor,Proudman balance holds, leading to an internal angular velocity constant over cylindrical surfaces co-axial with the rotation axis. It turns out that the angular velocity perturbations, whatever their origin, can be expressed in terms of the eigenfunctions of the equation of angular momentum conservation with stress-free boundary conditions. Moreover, a lower limit for the energy dissipation rate in a turbulent convection zone can be set, thanks to the extremal properties of the eigenfunctions. This approach allows to apply precise constraints on the amplitude and the radial profile of the angular velocity variations that are required to explain the observed orbital period changes in classical RS CVn binaries (i.e. with orbital period longer than 1,2 d and a subgiant secondary component). It is found that an angular velocity change as large as 10 per cent of the unperturbed angular velocity at the base of the stellar convection zone is needed. Such a large change is not compatible with the observations. Moreover, it would produce an energy dissipation rate much larger than the typical luminosities of the active components of RS CVn systems, except in the case that fast rotation and internal magnetic fields reduce the turbulent viscosity by at least 2 orders of magnitude with respect to the value given by the mixing-length theory. Therefore, the model proposed by Applegate should be rejected, at least in the case of classical RS CVn close binaries. Possible alternative models are briefly discussed, emphasizing the effects of intense magnetic fields (, 10 T) on the internal structure of magnetically active stars and the dynamics of close binary systems. [source]

Eclipsing binaries in open clusters , III.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Issue 3 2004
Persei, V621 Per in
ABSTRACT V621 Persei is a detached eclipsing binary in the open cluster , Persei, which is composed of an early B-type giant star and a main-sequence secondary component. From high-resolution spectroscopic observations and radial velocities from the literature, we determine the orbital period to be 25.5 d and the primary velocity semi-amplitude to be K= 64.5 ± 0.4 km s,1. No trace of the secondary star has been found in the spectrum. We solve the discovery light curves of this totally eclipsing binary and find that the surface gravity of the secondary star is log gB= 4.244 ± 0.054. We compare the absolute masses and radii of the two stars in the mass,radius diagram, for different possible values of the primary surface gravity, with the predictions of stellar models. We find that log gA, 3.55, in agreement with values found from fitting Balmer lines with synthetic profiles. The expected masses of the two stars are 12 and 6 M, and the expected radii are 10 and 3 R,. The primary component is near the blue loop stage in its evolution. [source]

A photometric,spectroscopic analysis and the evolutionary status of the Algol-type binary U Coronae Borealis

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Issue 4 2003
S. K. Yerli
ABSTRACT The prime purposes of this study are to obtain reliable orbital parameters for the Algol-type binary U Coronae Borealis (U CrB) and to explain the evolutionary status of this system. All observations of the primary star's radial velocity are consistent with the value K1= 58.6 ± 2.0 km s,1. Measurements of the radial velocity of the secondary component give K2 = 185.2 ± 5.0 km s,1. Using the photometrically determined inclination of 78.7 ± 0.3, the masses of the two stars are therefore deduced to be 4.74 ± 0.28 and 1.46 ± 0.06 M, for the primary and secondary components, respectively. Using all available observations, we discuss the origin and evolution of the close binary system U CrB. We derive the restrictions concerning masses and period from a general network of calculations of medium mass close binary evolution. Detailed models are calculated within the derived ranges, giving the most likely initial system parameters as and Pi= 1.4 d. It turns out that the interactive evolution up to the present stage has been non-conservative. During its evolution, U CrB has lost about 14 per cent of its initial total mass (,M, 1 M,) and around 18 per cent of its initial total angular momentum. We also examine the possibility of probing dynamo action in the mass-losing component of U CrB. We point out that, in order to maintain the evolution of U CrB in its later stages, which is presumably driven by stellar ,magnetic braking', an efficient mechanism for producing large-scale surface magnetic fields in the donor star is required. We suggest that observed X-ray activity in U CrB may be a good indicator of its evolutionary status and the internal structure of the mass-losing component. [source]

Influence of boron concentration on the XPS spectra of the (100) surface of homoepitaxial boron-doped diamond films

PHYSICA STATUS SOLIDI (A) APPLICATIONS AND MATERIALS SCIENCE, Issue 12 2006
S. Ghodbane
Abstract As-grown (100) homoepitaxial diamond films with boron concentrations [B] from 4.6 × 1016 to 1.5 × 1021 cm,3 have been analysed using X-ray photoelectron spectroscopy (XPS). Their C 1s core levels contain a dominant component around 284.17 ± 0.2 eV ascribed to sp3 C and a main secondary component around 284.88 ± 0.2 eV ascribed to CHx (x , 2) on surface defects. Their relative concentration decreases and increases, respectively, as [B] increases. A significant component around 286.4 ± 0.2 eV ascribed to ether group (C,O,C) remains nearly constant up to [B] , 3 × 1020 cm,3, then increases for greater boron concentrations. Other components around 283.0 ± 0.2, 287.69 ± 0.2 and 288.76 ± 0.2 eV ascribed, respectively, to sp2 C, carbonyl (C=O) and carboxyl (HO,C=O) on surface defects remain with low concentrations. The occurrence of these XPS components, their assignments and their relative concentrations are satisfactorily compared to those previously found for IIb crystals with (100) surface and for polycrystalline films with [B] around 1019 and 7 × 1020 cm,3. (© 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) [source]

Radial velocity and light curves analysis of the eclipsing binary NN Vir

ASTRONOMISCHE NACHRICHTEN, Issue 9 2004
R. Pazhouhesh
Abstract The eclipsing binary NN Vir is a short period system showing an EW-type light curve. Photometric observations of NN Vir were done by Gomez-Ferrellad & Garcia-Melendo (1997) at Esteve Duran Observatory. We used photometric data of NN Vir for light curve analysis. The available spectroscopic data of NN Vir is new and we also used the first radial velocity data of this system obtained by Rusinski & Lu (1999) for analysis. The radial velocity and light curves analysis was made with the latest version ofWilson program(1998) and the geometric and physical elements of the system are derived. By searching the simultaneous solutions of the system, we have determined the masses and radii of the components : 1.89(M,) and 1.65(R,) for the primary component; 0.93(M,) and 1.23(R,) for the secondary component. We estimated effective temperatures of 7030(K) for the primary and 6977(K) for the secondary component. (© 2004 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) [source]

Data Mining for Bioprocess Optimization

ENGINEERING IN LIFE SCIENCES (ELECTRONIC), Issue 3 2004
S. Rommel
Abstract Although developed for completely different applications, the great technological potential of data analysis methods called "data mining" has increasingly been realized as a method for efficiently analyzing potentials for optimization and for troubleshooting within many application areas of process, technology. This paper presents the successful application of data mining methods for the optimization of a fermentation process, and discusses diverse characteristics of data mining for biological processes. For the optimization of biological processes a huge amount of possibly relevant process parameters exist. Those input variables can be parameters from devices as well as process control parameters. The main challenge of such optimizations is to robustly identify relevant combinations of parameters among a huge amount of process parameters. For the underlying process we found with the application of data mining methods, that the moment a special carbohydrate component is added has a strong impact on the formation of secondary components. The yield could also be increased by using 2 m3 fermentors instead of 1 m3 fermentors. [source]

Membrane Photolithography: Direct Micropatterning and Manipulation of Fluid Phospholipid Membranes in the Aqueous Phase Using Deep-UV Light,

ADVANCED MATERIALS, Issue 14 2004
K. Yee
A wet photolithography approach using light-activated, localized, oxidative chemistry can directly pattern fluid phospholipid bilayers submerged in aqueous phases. Targeted incorporation of secondary components within pattern voids (see Figure) allows many membrane dynamical processes to be probed and optically defined arrays of holes, functional membrane microdomains, and proteins embedded in a lipidic background can be designed. [source]

The role of Raman microspectroscopy in the study of black gloss coatings on Roman pottery

JOURNAL OF RAMAN SPECTROSCOPY, Issue 1 2005
Francesca Ospitali
Abstract Raman microspectroscopy was adopted for the study of black gloss coatings on Roman pottery, found in Rimini (northern Italy) and in Suasa, near Ancona (central Italy), dated second century B.C. This non-destructive technique allowed a very accurate analysis of the crystalline and amorphous components of thin surface layers. The investigated coating is black, homogeneous and glazed, without any crystals, becoming red on approaching to the ceramic body. Magnetite and carbon are the main phases of the black zones, whereas hercynite, quartz, silicates and haematite are the secondary components. In the red zones, approaching the ceramic body, the amount of haematite increases and the amount of magnetite decreases. The presence of carbon, on the surface only, confirms the hypothesis of a firing cycle in a partial reducing atmosphere. Copyright © 2004 John Wiley & Sons, Ltd. [source]