Miracle-dz/UniFAR-FTUs huggingface dataset:
Petroleum Exploration in Geologically Complex Areas: Opportunities for Geochemical and Non-Seismic Hydrocarbon Detection Methods

The petroleum potential of geologically complex areas — such as highly faulted and folded terranes — is often poorly known due to technical challenges affecting seismic acquisition and imaging. When these areas occur in jungles and highlands, the logistical challenges only add to the difficulty of evaluating the petroleum potential of such terranes. For such areas, surface geochemical and non-seismic hydrocarbon-detection methods provide an opportunity to reliably detect and map the elevated hydrocarbon concentrations and hydrocarbon-induced changes commonly associated with undiscovered oil and gas accumulations. It has long been known that (1) all petroleum basins exhibit some type of near-surface hydrocarbon leakage, (2) that petroleum accumulations are dynamic and their seals imperfect, (3) that hydrocarbon seepage can be active or passive, and that it can be visible (macroseepage) or only detectable analytically (microseepage). The surface and near-surface expressions of hydrocarbon migration and seepage can take many forms, ranging from elevated hydrocarbon concentrations in soils to complex mineralogic, microbial, and geophysical changes. While such hydrocarbon leakage does not require significant faulting and fracturing, the common presence of faults and fractures in structurally complex and tectonically active terranes provides additional migration pathways for hydrocarbon seepage and microseepage. Hydrocarbon-detection surveys in geologically complex areas require careful planning, close sample spacing, and are most effective when results are integrated with satellite remote sensing data and available geophysical data. Such surveys are ideally suited for an early stage evaluation since they can quickly identify those parts of the area possessing the highest petroleum potential, as well as determine the characteristics of petroleum in the areas of interest. The inclusion of hydrocarbon-detection surveys early in an exploration strategy focuses attention and resources on a relatively small number of high-potential areas, thereby minimizing both risks and expenses. The presentation illustrates examples from Asia and South America.
CP violation, the CKM matrix and New Physics

Loop corrections for physics beyond the Standard Model are computed. DWe discuss the influence of new physics on CP-violating observables. Assuming the standard model gives a correct description of tree level processes, we show how a consistent procedure can determine the parameters of the standard model and check its validity also in loop induced processes. A method to include new physics in a systematic way is sketched.
Interaction of Low -energy Induced Gravity with Quantized Matter and Phase Transition Induced by Curvature

At high energy scale the only quantum effect of any asymptotic free and asymptoti-cally conformal invariant GUT is the trace anomaly of the energy-momentum tensor. Anomaly generates the new degree of freedom, that is propagating conformal factor. At lower energies conformal factor starts to interact with scalar field because of the violation of conformal invari-ance. We estimate the effect of such an interaction and find the running of the nonminimal coupling from conformal value 1 6 to 0. Then we discuss the possibility of the first order phase transition induced by curvature in a region close to the stable fixed point and calculate the induced values of Newtonian and cosmological constants.
Calibração biostratigráfica das unidades sísmicas da Bacia offshore do Algarve: contribuição do core SWIM04-39

1INETI, Departamento de Geologia Marinha. Estrada da Portela, Zambujal. Apartado 7586. 2720-Amadora 2Departamento de Geologia, FCUL, Campo Grande C6, Piso4, 1740-016 Lisboa 3Centro de Geologia, UL, Campo Grande C6, Piso3, 1740-016 Lisboa 4Centro de Estudos Geológicos, Departamento de Ciências da Terra da FCTUNL, Quinta da Torre, 2829-516 Caparica 5-ISMAR, Via Gobetti 101, 40129 Bolonha, Itália cristina.roque@ineti.pt
FORECASTING TOURIST ARRIVALS TO LANGKAWI ISLAND MALAYSIA

Tourism is the act of travelling for a person or group of people from their own locality to a specific destination in a short term or long term period either for leisure or business purposes. Tourism is an important sector in the Malaysian economy where tourism development will lead to the positive economic development of the country and in general improve the quality of life for all citizens. Therefore, forecasting tourist arrivals with high accuracy becomes important since it may ensure the development and the readiness of all tourism related industries such as hotels, transportation, food and services industries and their best shape. This study focuses on tourist arrivals in Langkawi Island as one of the major tourist attractions situated in the northerly region of Peninsular Malaysia. Importantly, this paper attempts to measure and compare the performance of forecasting with Exponential Smoothing, ARIMA and ARFIMA models using the R software package.
Correlated X-Ray and Optical Variability in V404 Cygni in Quiescence

We report simultaneous X-ray and optical observations of V404 Cyg in quiescence. The X-ray flux varied dramatically by a factor of ≳20 during a 60 ks observation. X-ray variations were well correlated with those in Hα, although the latter include an approximately constant component as well. Correlations can also be seen with the optical continuum, although these are less clear. We see no large lag between X-ray and optical line variations; this implies they are causally connected on short timescales. As in previous observations, Hα flares exhibit a double-peaked profile suggesting emission distributed across the accretion disk. The peak separation is consistent with material extending outward to at least the circularization radius. The prompt response in the entire Hα line confirms that the variability is powered by X-ray (and/or EUV) irradiation.
The exact mass-gap of the supersymmetric C P n − 1 sigma model

A formula for the mass-gap of the supersymmetric CP sigma model (n > 1) in two dimensions is derived: m/ΛMS = sin(π∆)/(π∆) where ∆ = 1/n and m is the mass of the fundamental particle multiplet. This result is obtained by comparing two expressions for the free-energy density in the presence of a coupling to a conserved charge; one expression is computed from the exact S-matrix of Köberle and Kurak via the thermodynamic Bethe ansatz and the other is computed using conventional perturbation theory. These calculations provide a stringent test of the S-matrix, showing that it correctly reproduces the universal part of the beta-function and resolving the problem of CDD ambiguities. CERN-TH.7426/94 September 1994 ∗ Supported by a fellowship from the EU Human Capital and Mobility programme. ∗∗ On leave from: Department of Physics, University of Wales, Swansea, SA2 8PP, U.K.
[ITAL]HUBBLE SPACE TELESCOPE[/ITAL][ITAL]Hubble Space Telescope[/ITAL]-NICMOS Observations of M31’[CLC]s[/CLC] Metal-Rich Globular Clusters and Their Surrounding Fields. I. Techniques

We have obtained HST-NICMOS observations of five of M31's most metal rich globular clusters. These data allow photometry of individual stars in the clusters and their surrounding fields. However, to achieve our goals -- obtain accurate luminosity functions to compare with their Galactic counterparts, determine metallicities from the slope of the giant branch, identify long period variables, and estimate ages from the AGB tip luminosity, we must be able to disentangle the true properties of the population from the observational effects associated with measurements made in very crowded fields. In this paper we present a careful analysis of photometry in crowded regions, and show how image blending affects the results and interpretation of such data. Although this analysis is specifically for our NICMOS observations in M31, the techniques we develop can be applied to any imaging data taken in crowded fields; we show how the effects of image blending will even limit NGST. We use three different techniques to analyze the effects of crowding on our data, including the insertion of artificial stars (traditional completeness tests) and the creation of completely artificial clusters. They are used to derive threshold- and critical-blending radii for each cluster, which determine how close to the cluster center reliable photometry can be achieved. The simulations also allow us to quantify and correct for the effects of blending on the slope and width of the RGB at different surface brightness levels.
Bubble wall dynamics, generalised Yukawa couplings and adequate electroweak baryogenesis in two-Higgs-doublet model

Baryogenesis at the electroweak scale depends on divers but identifiable details of bubble wall dynamics and the particle physics. We show that inclusion of the dynamics of relative phase in two-Higgs-doublet model (2HDM) enhances the adiabatic order of the mechanism proposed by McLerran-Shaposhnikov-Turok-Voloshin where the scalar-scalar-vector triangle diagram with top quark in the loop gives rise to a significant contribution to the effective chemical potential biasing the Chern-Simons number. We also show that in 2HDM with less stringent constraints on Yukawa couplings than those imposed by natural flavour conservation, there are additional diagrams contributing to the effective chemical potential. These two effects can combine with several others to produce adequate baryon asymmetry at the electroweak scale.
1 6 M ar 2 00 6 Enhanced Macroscopic Quantum Tunneling in Bi 2 Sr 2 CaCu 2 O 8 + δ Intrinsic Josephson Junction Stacks

We have investigated macroscopic quantum tunneling in Bi2Sr2CaCu2O8+δ intrinsic Josephson junctions at millikelvin temperatures using microwave irradiation. Measurements show that the escape rate for uniformly switching stacks of N junctions is about N times higher than that of a single junction having the same plasma frequency. We argue that this gigantic enhancement of macroscopic quantum tunneling rate in stacks is boosted by current fluctuations which occur in the series array of junctions loaded by the impedance of the environment.
A ug 2 00 6 STUDIES ON SOME ASPECTS OF THE FUNDAMENTAL THEORY OF EVERYTHING

What happens to the entropy increase principle as the Universe evolve to form the bigcrunch singularity? What happens to the uncertainity relations along the process of gravitational collapses? What is the quantum mechanical description of a Radon atom in a rigid box when the distance of consecutive nodes and antinodes of ψ is equal to or less than the diameter of the atom? What is the position-space wave function of two finite volume massive bosons if we take contact interaction into account? How a photon produce electron-positron pair with finite volume concentrate rest masses? What are the charges of the electron-positron pairs forming loops in the vacuum? How two particles with threemomentums k1, k2 (k1 6= k2) produced to form a loop at a space-time point always arrive at another spacial point simultaneously? What is the microscopic explanation in terms of particle exchanges of the force in the Casimir effect? What is the mechanism of the collapse of the momentum-space wave function of a particle knocking out an elctron from an atom? What is meant by |Ψ >= c1(t)|ΨU238 > +c2(t)|ΨTh234 > ? Quantum mechanically the region between the rigid walls (which is equiprobable in classical mechanics) is non-homogeneous for a particle in a rigid box ! A photon can not reproduce Maxwell’s equations apart from moving with velocity c. How can a process involving only a few photons be described starting from the Maxwell’s equations? The large scale structure of the Universe is homogeneous. What is the screen in our brains to view objects, as they are, of sizes larger than our brains?
General Relativity in Higher Dimensions

The thesis represents an interesting and original contribution to the study of exact spacetimes within the context of higher dimensional gravity. Its topic naturally fits into the contemporary research in theoretical physics which is motivated by various attempts to generalize and extend Einstein’s general relativity, to quantize it or (hopefully) even to unify it with other forces which occur in nature. Apart from these motivations, rigorous investigation of exact solutions of generalized Einstein gravity equations is also important from purely mathematical point of view. It may elucidate in what sense are four-dimensional spacetimes privileged.
Massive Stellar Content of Giant H II Regions in M33 and M101

Far-ultraviolet (900-1200 Å) spectral synthesis of nine giant extragalactic H II regions in M33 and M101 is performed to study their massive stellar content. Several parameters are quantified, predicted, and compared to the literature: age, stellar mass, initial mass function (IMF) slope, number of O-type and Wolf-Rayet stars, and Hα and 5500 Å continuum fluxes. The results of this particular technique are consistent with other methods and observations. This work shows that a total stellar mass of a few 103 M⊙ is needed to populate the IMF bins well enough at high masses to obtain accurate results from the spectral synthesis technique in the far-ultraviolet. A flat IMF slope seems to characterize better the stellar line profiles of these objects, which is likely the first sign of a small number statistics effect on the IMF. Finally, the H II region NGC 5461 is identified as a good candidate for hosting a second generation of stars, not yet seen at far-ultraviolet wavelengths.
Magnetic flux emergence in fast rotating stars

Fast rotating cool stars are characterised by high magnetic activity levels and frequently show dark spots up to polar latitudes. Their distinctive surface distributions of magnetic flux are investigated in the context of the solar-stellar connection by applying the solar flux eruption and surface flux transport models to stars with different rotation rates, mass, and evolutionary stage. The rise of magnetic flux tubes through the convection zone is primarily buoyancy-driven, though their evolution can be strongly affected by the Coriolis force. The poleward deflection of the tube's trajectory increases with the stellar rotation rate, which provides an explanation for magnetic flux eruption at high latitudes. The formation of proper polar spots likely requires the assistance of meridional flows both before and after the eruption of magnetic flux on the stellar surface. Since small radiative cores support the eruption of flux tubes at high latitudes, low-mass pre-main sequence stars are predicted to show high mean latitudes of flux emergence. In addition to flux eruption at high latitudes, main sequence components of close binary systems show spot distributions which are non-uniform in longitude. Yet these `preferred longitudes' of flux eruption are expected to vanish beyond a certain post-main sequence evolutionary stage.
A Survey of Classical Knot Concordance

In 1926 Artin [3] described the construction of certain knotted 2–spheres in R 4. The intersection of each of these knots with the standard R 3 ⊂ R 4 is a nontrivial knot in R 3. Thus a natural problem is to identify which knots can occur as such slices of knotted 2–spheres. Initially it seemed possible that every knot is such a slice knot and it wasn't until the early 1960s that Murasugi [86] and Fox and Milnor [24, 25] succeeded at proving that some knots are not slice. Slice knots can be used to define an equivalence relation on the set of knots in S 3 : knots K and J are equivalent if K# − J is slice. With this equivalence the set of knots becomes a group, the concordance group of knots. Much progress has been made in studying slice knots and the concordance group, yet some of the most easily asked questions remain untouched. There are two related theories of concordance, one in the smooth category and the other topological. Our focus will be on the smooth setting, though the distinctions and main results in the topological setting will be included. Related topics must be excluded, in particular the study of link concordance. Our focus lies entirely in the classical setting; higher dimensional concordance theory is only mentioned when needed to understand the classical setting.
CLAY MINERAL STUDY OF PABDEH FORMATION IN TYPE SECTION AND IT´S COMPARISON WITH NGS DATA FROM KUPAL OIL FIELD (WELL NO. 12 & 38)

The calcimeteric analysis of samples from Pabdeh Formation, in type section (north of Dezful embayment subzone), represent a marl and shaly marl lithology. SEM images from these samples represent chlorite flakes with diagenetic origin (transformation of illite to chlorite) and imply the possible existence of other detrital clay minerals (include chlorite). However, XRD analysis of selected samples indicates the existence of montmorillonite, illite and chlorite showing a descending trend for clay percent and montmorillonite and ascending one for illite and chlorite from bottom to top of these deposits. Based on these evidences, we introduced the possibility for cooling in climate condition and shoaling in depth of deposition, from bottom to top of the Pabdeh Formation.
Electromagnetic form factors of the transition from the spin-3 / 2 (cid:2) to the (cid:3) hyperon

The three electromagnetic form factors for the transition from a 3 / 2 + (cid:2) ∗ hyperon to the ground-state (cid:3) hyperon are studied. At low energies, combinations of the transition form factors can be deduced from Dalitz decays of the (cid:2) ∗ hyperon to (cid:3) plus an electron-positron pair. It is pointed out how more information can be obtained with the help of the self-analyzing weak decay of the (cid:3) . In particular, it is shown that these transition form factors are complex quantities already in this kinematical region. Such measurements are feasible at hyperon factories such as, for instance, the Facility for Antiproton and Ion Research (FAIR). At higher energies, the transition form factors can be measured in electron-positron collisions. The transition form factors are related to decay distributions and differential cross sections. Using dispersion theory, the low-energy electromagnetic form factors for the (cid:2) ∗ -to- (cid:3) transition are related to the pion vector form factor. The additionally required input, i.e., the two-pion– (cid:2) ∗ – (cid:3) amplitudes, is determined from relativistic next-to-leading-order (NLO) baryon chiral perturbation theory, including the baryons from the octet and the decuplet. A poorly known NLO parameter is ﬁxed to the experimental value of the (cid:2) ∗ → (cid:3)γ decay width. Pion rescattering is taken into account by using dispersion theory and solving a Muskhelishvili-Omnès equation. Subtracted and unsubtracted dispersion relations are discussed. However, in view of the fact that the transition form factors are complex quantities, the current data situation does not allow for a full determination of the subtraction constants. To reduce the number of free parameters, unsubtracted dispersion relations are used to make predictions for the transition form factors in the low-energy space- and timelike regions.
Optical unmixing using programmable spectral source based on DMD

Traditional spectral unmixing involves intense signal processing applied on multispectral or hyperspectral data captured from an imaging device, which is highly time-consuming. In this article, a novel method, namely "optical unmixing", is proposed to alleviate the post processing effort by replacing the heavy computation with a spectrally tunable light source. By choosing spectral features of the light source intelligently, the abundance map of each material can be retrieved with minimum computation from gray value images captured by a normal camera. For n unknown endmembers, 3n + 1 measurements are required to retrieve the abundance maps with proposed algorithms.
Quiescence Detection in Multiagent Negotiation

In a distributed multiagent negotiation involving multiple issues, it is often desirable to nalize deals only when all related issues are resolved. However, detecting that a multiagent negotiation has reached a globally quiescent state can be a nontrivial task in a distributed, asynchronous system. We present a quies-cence detection protocol based on the Dijkstra-Scholten algorithm for distributed termination detection. The protocol operates as a layer on top of an underlying mediated negotiation protocol. If agents conform to the detection protocol, the detection process terminates ii the negotiation is quiescent. We discuss agent incentives to deviate from the protocol, and describe extensions that enforce adherence with respect to the most signiicant potential deviations.
Measurement of the Isolated Prompt Photon Production Cross Section in pp Col

The differential cross section for the inclusive production of isolated prompt photons has been measured as a function of the photon transverse energy E T in pp collisions at ffiffi s p 1⁄4 7 TeV using data recorded by the CMS detector at the LHC. The data sample corresponds to an integrated luminosity of 2:9 pb . Photons are required to have a pseudorapidity j j< 1:45 and E T > 21 GeV, covering the kinematic region 0:006< xT < 0:086. The measured cross section is found to be in agreement with nextto-leading-order perturbative QCD calculations.
The Fulmar Field, Blocks 30/16, 30/11b, UK North Sea

Abstract The Fulmar Field is located on the southwestern margin of the Central Graben in Blocks 30/16 and 30/11b of the UK sector of the North Sea. The Fulmar Field was discovered 1975 and began producing in 1982. Currently (2000) the field produces at a rate of 8000 BOPD at a watercut above 90% mainly through the process of rinsing of residual oil. Total STOIIP is 822 MMBBL and ultimate recovery is 567 MMBBL of oil and 342 BSCF of wet gas. As of the end of 1999, 547 MMSTB of oil and 325 BSCF of wet gas had been produced. The high recovery factor (69%) of the field is thought to be linked to the combination of well density, large length of reservoir perforated, excellent reservoir quality, sweep by water injection, good pressure support and oil stripping from a secondary gas cap formed early in field life. The Fulmar Field is a small triangular, partly eroded domal anticline with steeply dipping flanks, located on a fault terrace within the western margin of the South West Central Graben at a depth between 9900 and 11 500 ft TVDss. The field has been shaped by three major tectonic processes: (1) halokinesis, (2) syndepositional reactivation of Caledonian basement faults; and (3) syndepositional through post-depositional displacements along the nearby Auk Horst Boundary Fault. The reservoir consists of thick Upper Jurassic, shallow marine, very bioturbated sandstones of the Fulmar Formation overlain by the deeper marine Ribble Sands interbedded within the Kimmeridge Clay Formation. Reservoir seal is provided by the Kimmeridge Clay in the west and Upper Cretaceous chalks which unconformably overlie the Fulmar Formation in the east. The reservoir section has been lithostratigraphically subdivided into six reservoir units and 24 sub-units. Integration of bio- and lithostratigraphic data has led to a sequence stratigraphic model of the Jurassic succession in the Fulmar Field. In total four depositional sequences are identified, which progressively onlap Triassic basement towards the southwest. The older Jurassic sequences are characterized by rapid progradation of shoreface sands, whereas aggradation of thick sediment packages is typical of the younger intervals. This change of depositional architecture is linked to syndepositional reactivation of basement faults. Major transgressive intervals form intra-reservoir barriers or baffles to flow. Facies changes (Mersey-Clyde Sands) from proximal to distal facies are abrupt and are also linked to basement faults.