Flickering in the Magnetic Cv Star Am Herculis     

Belinda Kalomeni  E. Rennan PekÜnlÜ  Kadri Yakut 《Astrophysics and Space Science》2005,296(1-4):477-480

In this study, we present a photometric study of AM Her, a prototype of a class of magnetic CVs. Optical photometry of AM Her was obtained using the Russian–Turkish 1.5 m telescope at TüBİTAK National Observatory (TUG) in August 2003. The R band light curve of the system shows two maxima and two minima during one orbital cycle. In both observing nights the star showed flickering at a significant level. The measured flickering time scale is about 5 min.  相似文献   

Series approximation of the Kirchhoff method for wavefield computation on a rough subsurface     

Selma Kadio&#;lu  Turan Kayiran 《Geophysical Prospecting》2002,50(2):239-257

ABSTRACT Computation of the wavefield due to reflection from an irregular surface is carried out for subsurfaces with large radii of curvature. The Kirchhoff approximation is proved to be sufficiently accurate provided that the acoustic wavelength is sufficiently small with respect to the asperities of the rough surface. For cases where the irregular surface does not fulfil this condition, a series solution is proposed. The first term of this series appears to be the result obtained by conventional Kirchhoff approximation. The series, initially developed in the space–wavenumber domain by Meecham, is transformed into the space–time domain, and the general expression for the series is obtained by calculation of the normal derivative of the field function. The series solution, restricted to the first two terms, is illustrated by application to three synthetic examples. Applications show that the series approximation obtained by the Kirchhoff method contributes significantly to the modelling of narrow, steep and deep structures and consequently it appears that the second term in the series cannot be ignored in the computation of the wavefields arising from a rough surface.  相似文献   

Late Cretaceous–Cenozoic subduction–collision history of the Southern Neotethys: new evidence from the Çağlayancerit area,SE Turkey     

Ahmet Can Akıncı  Alastair H. F. Robertson  Ulvi Can Ünlügenç 《International Journal of Earth Sciences》2016,105(1):315-337

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Comparison Of Three Uncertainty-Analysis Methods To Assess Impacts On Groundwater Of Constituents Leached From Land-Disposed Waste     

K. Ünlü  J. C. Parker  P. K. Chong 《Hydrogeology Journal》1995,3(2):4-18

Assessment of the environmental fate and behavior of constituents that have the potential to leach from waste-disposal pits that are associated with petroleum exploration and production activities is a problem of interest to industry and regulatory agencies. A stochastic modeling approach for the migration of constituents in soil and groundwater was developed to assess the impact on groundwater at receptors that are downgradient from a waste pit. The model evaluates uncertainties in constituent concentrations in groundwater due to uncertainties in waste-composition and hydrogeologic properties of waste sites, and it determines the probability distributions of constituent concentration at receptor points by using Monte Carlo (MC), First-Order (FO), and Point-Estimate (PE) methods. Application of the FO and PE methods to assess probability distributions requires an assumption of the form of the probability density function for concentration at a receptor point. A log-normal distribution is employed here. A comparison of the three uncertainty-analysis methods is performed to evaluate the efficiency and accuracy of the FO and PE methods relative to the MC method. Results suggest that for non-reactive and conservative constituents the level of accuracy provided by FO method is similar to that of the MC method. The computational effort for the FO method is about 1 percent of that for the MC method. For nonconservative constituents, the FO method compared less favorably with the MC results. Thus, the use of the MC method is warranted, for nonconservative constituents or for cases where a higher degree of precision in the probability distribution is needed. RÉSUMÉ: L'industrie et les organismes de contrôle s'intéressent particulièrement au problème de la prédiction du devenir et du comportement environnemental de composés susceptibles de lixivier des pollutants à partir de puits de stockage de déchets associés à des zones d'exploration et de production pétrolières. Une modélisation stochastique de la migration de composées dans le sol et les eaux souterraines est proposée en vue de prédire l'impact sur les eaux souterraines en des points de prélèvement situés en aval-gradient d'un puits de stockage. Le modèle fournit une estimation des incertitudes sur les teneurs des composés dans les eaux souterraines en fonction de la composition des déchets et des propriétés hydrogéologiques des sites de stockage; il détermine les distributions de probabilité de la concentration des composés à des points de prélèvement au moyen des méthodes de Monte-Carlo (MC), du Premier Ordre (PO) et de l'Estimation Ponctuelle (EP). Le recours aux méthodes PO et EP pour prédire les distributions de probabilité impose une hypothèse sur la forme de la fonction de densité de probabilité pour la concentration en un point de prélèvement. Une distrubution log-normale est utilisée ici. Une comparaison des trois méthodes d'analyse de l'incertude a été réalisée afin d'estimer l'efficacité et la précision des méthodes PO et EP par rapport à la méthode MC. Les résultats indiquent que, pour des composés conservatifs, le degré de précision atteint par la méthode PO est comparable à celle de la méthode MC. La puissance de calcul requise par la méthode PO est 1% environ de celle nécessaire pour la méthode MC. Pour des composés non conservatifs, la comparaison avec la méthode MC est moins favorable à la méthode PO. Par conséquent, la méthode MC est préférable pour les composés non conservatifs ou dans les cas où un meilleur degré de précision de la distribution de probabilité est nécessaire. RESUMEN: La evaluación del comportamiento de constituyentes lixiviables desde vertidos de residuos asociados a actividades de exploración y producción petrolífera, así como su posible impacto ambiental, es un problema de interés para la industria y las agencias reguladoras. Se ha desarrollado una modelación estocástica para estudiar la migración de los constituyentes en el suelo y el agua subterránea, con el objetivo de evaluar su impacto en receptores situados aguas abajo de un vertido. El modelo evalúa las incertidumbres en las concentraciones de los constituyentes debidas a las incertidumbre en la composición de los residuos y de las propiedades hidrogeológicas de la zona de vertido y determina las distribuciones de probabilidad de dichas concentraciones en puntos de recepción mediante los métodos de Monte Carlo (MC), Primer-Orden (FO) y Estimación Puntual (PE). La aplicación de los métodos FO y PE para evaluar las distribuciones de probabilidad reqiere suponer conocida la forma de la función de densidad de probabilidad para la concentración en el punto receptor. En este caso, se emplea una distribución log-normal. Se lleva a cabo una comparación entre los tres métodos de análisis de errores para evaluar la eficiencia y exactitud de los métodos FO y PE respecto al MC. Los resultados sugieren que para constituyentes conservativos no-reactivos, el nivel de exactitud suministrado por el método FO es comparable con el del MC. El esfuerzo computacional para el método FO, en cambio, es alrededor del 1% del método MC. Para constituyentes no conservativos, es método FO no compara tan favorablemente frente a los resultados del MC. Por tanto, el uso del método MC está obligado para constituyentes no conservativos y para casos en los que se requiere un alto nivel de precisión en la distribución de probabilidad.  相似文献   

Circulating subbeam systemsand the physics of pulsar emission     

Joanna?M.?RankinEmail author  Geoffrey?A.?E.?Wright 《Astronomy and Astrophysics Review》2003,12(1):43-69

The purpose of this paper is to suggest how detailed single-pulse observations of slow radio pulsars may be utilized to construct an empirical model for their emission. It links the observational synthesis developed in a series of papers by Rankin in the 1980s and 90s to the more recent empirical feedback model of Wright (2003a) by regarding the entire pulsar magnetosphere as a non-steady, non-linear interactive system with a natural built-in delay. It is argued that the enhanced role of the outer gap in such a system indicates an evolutionary link to younger pulsars, in which this region is thought to be highly active, and that pulsar magnetospheres should no longer be seen as being driven by events on the neutron stars polar cap, but as having more in common with planetary magnetospheres and auroral phenomena.Received: 8 May 2003, Published online: 14 November 2003 Correspondence to: Joanna M. Rankin. On leave from: Physics Department, University of Vermont, Burlington, VT 05405, USA  相似文献   

Fundamental physics and absolute positioning metrology with the MAGIA lunar orbiter     

Simone Dell��Agnello  Caterina Lops  Giovanni O. Delle Monache  Douglas G. Currie  Manuele Martini  Roberto Vittori  Angioletta Coradini  Cesare Dionisio  Marco Garattini  Alessandro Boni  Claudio Cantone  Riccardo March  Giovanni Bellettini  Roberto Tauraso  Mauro Maiello  Luca Porcelli  Simone Berardi  Nicola Intaglietta 《Experimental Astronomy》2011,32(1):19-35

MAGIA is a mission approved by the Italian Space Agency (ASI) for Phase A study. Using a single large-diameter laser retroreflector, a large laser retroreflector array and an atomic clock onboard MAGIA we propose to perform several fundamental physics and absolute positioning metrology experiments: VESPUCCI, an improved test of the gravitational redshift in the Earth?CMoon system predicted by General Relativity; MoonLIGHT-P, a precursor test of a second generation Lunar Laser Ranging (LLR) payload for precision gravity and lunar science measurements under development for NASA, ASI and robotic missions of the proposed International Lunar Network (ILN); Selenocenter (the center of mass of the Moon), the determination of the position of the Moon center of mass with respect to the International Terrestrial Reference Frame/System (ITRF/ITRS); this will be compared to the one from Apollo and Lunokhod retroreflectors on the surface; MapRef, the absolute referencing of MAGIA??s lunar altimetry, gravity and geochemical maps with respect to the ITRF/ITRS. The absolute positioning of MAGIA will be achieved thanks to: (1) the laboratory characterization of the retroreflector performance at INFN-LNF; (2) the precision tracking by the International Laser Ranging Service (ILRS), which gives two fundamental contributions to the ITRF/ITRS, i.e. the metrological definition of the geocenter (the Earth center of mass) and of the scale of length; (3) the radio science and accelerometer payloads; (4) support by the ASI Space Geodesy Center in Matera, Italy. Future ILN geodetic nodes equipped with MoonLIGHT and the Apollo/Lunokhod retroreflectors will become the first realization of the International Moon Reference Frame (IMRF), the lunar analog of the ITRF.  相似文献   

Report of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2009   总被引：5，自引：0，他引：5  

B. A. Archinal  M. F. A��Hearn  E. Bowell  A. Conrad  G. J. Consolmagno  R. Courtin  T. Fukushima  D. Hestroffer  J. L. Hilton  G. A. Krasinsky  G. Neumann  J. Oberst  P. K. Seidelmann  P. Stooke  D. J. Tholen  P. C. Thomas  I. P. Williams 《Celestial Mechanics and Dynamical Astronomy》2011,109(2):101-135

Every three years the IAU Working Group on Cartographic Coordinates and Rotational Elements revises tables giving the directions of the poles of rotation and the prime meridians of the planets, satellites, minor planets, and comets. This report takes into account the IAU Working Group for Planetary System Nomenclature (WGPSN) and the IAU Committee on Small Body Nomenclature (CSBN) definition of dwarf planets, introduces improved values for the pole and rotation rate of Mercury, returns the rotation rate of Jupiter to a previous value, introduces improved values for the rotation of five satellites of Saturn, and adds the equatorial radius of the Sun for comparison. It also adds or updates size and shape information for the Earth, Mars?? satellites Deimos and Phobos, the four Galilean satellites of Jupiter, and 22 satellites of Saturn. Pole, rotation, and size information has been added for the asteroids (21) Lutetia, (511) Davida, and (2867) ?teins. Pole and rotation information has been added for (2) Pallas and (21) Lutetia. Pole and rotation and mean radius information has been added for (1) Ceres. Pole information has been updated for (4) Vesta. The high precision realization for the pole and rotation rate of the Moon is updated. Alternative orientation models for Mars, Jupiter, and Saturn are noted. The Working Group also reaffirms that once an observable feature at a defined longitude is chosen, a longitude definition origin should not change except under unusual circumstances. It is also noted that alternative coordinate systems may exist for various (e.g. dynamical) purposes, but specific cartographic coordinate system information continues to be recommended for each body. The Working Group elaborates on its purpose, and also announces its plans to occasionally provide limited updates to its recommendations via its website, in order to address community needs for some updates more often than every 3 years. Brief recommendations are also made to the general planetary community regarding the need for controlled products, and improved or consensus rotation models for Mars, Jupiter, and Saturn.  相似文献   

Angular momentum exchange during secular migration of two-planet systems     

Adri��n Rodr��guez  Tatiana A. Michtchenko  Octavio Miloni 《Celestial Mechanics and Dynamical Astronomy》2011,111(1-2):161-178

We investigate the secular dynamics of two-planet coplanar systems evolving under mutual gravitational interactions and dissipative forces. We consider two mechanisms responsible for the planetary migration: star-planet (or planet-satellite) tidal interactions and interactions of a planet with a gaseous disc. We show that each migration mechanism is characterized by a specific law of orbital angular momentum exchange. Calculating stationary solutions of the conservative secular problem and taking into account the orbital angular momentum leakage, we trace the evolutionary routes followed by the planet pairs during the migration process. This procedure allows us to recover the dynamical history of two-planet systems and constrain parameters of the involved physical processes.  相似文献   

Erratum to: Reports of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2006 & 2009     

B. A. Archinal  M. F. A��Hearn  A. Conrad  G. J. Consolmagno  R. Courtin  T. Fukushima  D. Hestroffer  J. L. Hilton  G. A. Krasinsky  G. Neumann  J. Oberst  P. K. Seidelmann  P. Stooke  D. J. Tholen  P. C. Thomas  I. P. Williams 《Celestial Mechanics and Dynamical Astronomy》2011,110(4):401-403

The primary poles for (243) Ida and (134340) Pluto and its satellite (134340) Pluto : I Charon were redefined in the IAU Working Group on Cartographic Coordinates and Rotational Elements (WGCCRE) 2006 report (Seidelmann et al. in Celest Mech Dyn Astr 98:155, 2007), and 2009 report (Archinal et al. in Celest Mech Dyn Astr 109:101, 2011), respectively, to be consistent with the primary poles of similar Solar System bodies. However, the WGCCRE failed to take into account the effect of the redefinition of the poles on the values of the rotation angle W at J2000.0. The revised relationships in Table 3 of Archinal et al. 2011) are $$\begin{array}{llll} W & = & 274^{\circ}.05 +1864^{\circ}.6280070\, d\;{\rm for\; (243)\,Ida} \\ W & = & 302^{\circ} .695 + 56^{\circ} .3625225\, d\;{\rm for\; (134340)\,Pluto,\; and}\\ W & = & 122^{\circ} .695 + 56^{\circ} .3625225\, d\;{\rm for\; (134340)\,Pluto : I \,Charon}\end{array}$$ where d is the time in TDB days from J2000.0 (JD2451545.0).  相似文献   

On type-I migration near opacity transitions. A generalized Lindblad torque formula for planetary population synthesis     

Fr��d��ric S. Masset 《Celestial Mechanics and Dynamical Astronomy》2011,111(1-2):131-160

We give an expression for the Lindblad torque acting on a low-mass planet embedded in a protoplanetary disk that is valid even at locations where the surface density or temperature profile cannot be approximated by a power law, such as an opacity transition. At such locations, the Lindblad torque is known to suffer strong deviation from its standard value, with potentially important implications for type I migration, but the full treatment of the tidal interaction is cumbersome and not well suited to models of planetary population synthesis. The expression that we propose retains the simplicity of the standard Lindblad torque formula and gives results that accurately reproduce those of numerical simulations, even at locations where the disk temperature undergoes abrupt changes. Our study is conducted by means of customized numerical simulations in the low-mass regime, in locally isothermal disks, and compared to linear torque estimates obtained by summing fully analytic torque estimates at each Lindblad resonance. The functional dependence of our modified Lindblad torque expression is suggested by an estimate of the shift of the Lindblad resonances that mostly contribute to the torque, in a disk with sharp gradients of temperature or surface density, while the numerical coefficients of the new terms are adjusted to seek agreement with numerics. As side results, we find that the vortensity related corotation torque undergoes a boost at an opacity transition that can counteract migration, and we find evidence from numerical simulations that the linear corotation torque has a non-negligible dependency upon the temperature gradient, in a locally isothermal disk.  相似文献