Chronology of the Life of St. Paul

Though properly an historical rather than a theological problem, the chronology of Paul\u27s life is important in the field of Bible study, and is closely related to several theological questions, including that of the reliability of Scripture and the authenticity of several books accepted by the church as canonical. Its treatment is historical, but much of the freedom for specualtion indulged in by the average student of history is denied the scholar who treats this subject. Anything which cannot be established with reasonable certainty must be left an open question, and the integrity of the Scripture must remain unmolested

Actions, Reasons and Self-Expression: A Defense of Subjectivist-Internalism about Reasons

The central question of my dissertation is: what makes it the case that certain considerations are reasons for acting? This is a question about the truth-makers of claims about reasons, that is, what makes it the case that one has a reason to Φ rather than Ψ. There are two leading camps in the philosophical debate devoted to answering this question: subjectivism and objectivism. Subjectivist theories hold that one has a reason to do something when one has a non-truth evaluable favoring attitude towards that thing, e.g. desiring it. Objectivist theories insist that one’s desires are irrelevant to establishing the existence of reasons; that some action or desire is morally good or valuable is equally and universally reason-providing, whatever else individual agents happen to desire. I argue that all reasons for action are subjective; that, conversely, there are no objective reasons. After rejecting objectivism and providing a general defense of subjectivist views, I defend a more nuanced subjectivist-internalist position called Expressive Reasons. Subjectivist-internalism is the view that reasons are not only rooted in agent’s desires, but also that it must be possible for a reason to serve as the basis for an individual’s action if it is to be a reason in the first place. Expressive Reasons is the particular view that R is a reason for A to ϕ when ϕ-ing is an expression of soundly deliberating A’s self; and A, under ordinary conditions, would act on the basis of R. I argue that Expressive Reasons has unique philosophical advantages over competing views of reasons, and that it has compelling practical advantages in how it directs us to respond to different others

A Search for Ultra-High Energy Counterparts to Gamma-Ray Bursts

A small air shower array operating over many years has been used to search for ultra-high energy (UHE) gamma radiation ($\geq 50$ TeV) associated with gamma-ray bursts (GRBs) detected by the BATSE instrument on the Compton Gamma-Ray Observatory (CGRO). Upper limits for a one minute interval after each burst are presented for seven GRBs located with zenith angles $\theta < 20^{\circ}$. A $4.3\sigma$ excess over background was observed between 10 and 20 minutes following the onset of a GRB on 11 May 1991. The confidence level that this is due to a real effect and not a background fluctuation is 99.8\%. If this effect is real then cosmological models are excluded for this burst because of absorption of UHE gamma rays by the intergalactic radiation fields.Comment: 4 pages LaTeX with one postscript figure. This version does not use kluwer.sty and will allow automatic postscript generatio

Power, Competitiveness, and Advice Taking: Why the Powerful Don't Listen

Four experiments test the prediction that feelings of power lead individuals to discount advice received from both experts and novices. Experiment 1 documents a negative relationship between subjective feelings of power and use of advice. Experiments 2 and 3 further show that individuals experiencing neutral and low levels of power weigh advice from experts and experienced advisors more heavily than advice from novices, but individuals experiencing high levels of power discount both novice and expert advice. Experiments 3 and 4 demonstrate that this tendency of individuals experiencing high levels of power to discount advice from experts and novices equally is mediated by feelings of competitiveness (Experiment 3) and confidence (Experiments 3 and 4). Finally, Experiment 4 shows that inducing high power individuals to feel cooperative with their advisors can mitigate this tendency, leading them to weigh expert advice more heavily than advice from novices. Theoretical and practical contributions are discussed

When Power Makes Others Speechless: The Negative Impact of Leader Power on Team Performance

We examine the impact of subjective power on leadership behavior and demonstrate that the psychological effect of power on leaders spills over to impact team effectiveness. Specifically, drawing from the approach/inhibition theory of power, power-devaluation theory, and organizational research on the antecedents of employee voice, we argue that a leader's experience of heightened power produces verbal dominance, which reduces perceptions of leader openness and team open communication. Consequently, there is a negative effect of leader power on team performance. Three studies find consistent support for this argument. The implications for theory and practice are discussed

Comprehensive Observations of a Solar Minimum CME with STEREO

We perform the first kinematic analysis of a CME observed by both imaging and in situ instruments on board STEREO, namely the SECCHI, PLASTIC, and IMPACT experiments. Launched on 2008 February 4, the CME is tracked continuously from initiation to 1 AU using the SECCHI imagers on both STEREO spacecraft, and is then detected by the PLASTIC and IMPACT particle and field detectors on board STEREO-B. The CME is also detected in situ by ACE and SOHO/CELIAS at Earth's L1 Lagrangian point. The CME hits STEREO-B, ACE, and SOHO on 2008 February 7, but misses STEREO-A entirely. This event provides a good example of just how different the same event can look when viewed from different perspectives. We also demonstrate many ways in which the comprehensive and continuous coverage of this CME by STEREO improves confidence in our assessment of its kinematic behavior, with potential ramifications for space weather forecasting. The observations provide several lines of evidence in favor of the observable part of the CME being narrow in angular extent, a determination crucial for deciding how best to convert observed CME elongation angles from Sun-center to actual Sun-center distances.Comment: 27 pages, 10 figures, AASTEX v5.2, accepted by Ap

Electro-kinetic technology as a low-cost method for dewatering food by-product

Increasing volumes of food waste, intense environmental awareness, and stringent legislation have imposed increased demands upon conventional food waste management. Food byproducts that were once considered to be without value are now being utilized as reusable materials, fuels, and energy in order to reduce waste. One major barrier to the valorization of food by-products is their high moisture content. This has brought about the necessity of dewatering food waste for any potential re-use for certain disposal options. A laboratory system for experimentally characterizing electro-kinetic dewatering of food by-products was evaluated. The bench scale system, which is an augmented filter press, was used to investigate the dewatering at constant voltage. Five food by-products (brewer’s spent grain, cauliflower trimmings, mango peel, orange peel, and melon peel) were studied. The results indicated that electro-kinetic dewatering combined with mechanical dewatering can reduce the percentage of moisture from 78% to 71% for brewer’s spent grain, from 77% to 68% for orange peel, from 80% to 73% for mango peel, from 91% to 74% for melon peel, and from 92% to 80% for cauliflower trimmings. The total moisture reduction showed a correlation with electrical conductivity (R2¼0.89). The energy consumption of every sample was evaluated and was found to be up to 60 times more economical compared to thermal processing

Evolution and decay of an active region: Magnetic shear, flare and CME activity

Desde abril de 1996 y hasta febrero de 1997, se observó en el disco solar un complejo de actividad. Este complejo exhibió su nivel más alto de actividad durante el nacimiento de la región activa (AR) 7978. Nuestro análisis se extiende a lo largo de seis rotaciones solares, desde la aparición de AR 7978 (julio de 1996) hasta el decaimiento y dispersión de su flujo (noviembre de 1996). Los datos en varias longitudes de onda provistas por los instrumentos a bordo del Solar and heliospheric Observatory (SOHO) y del satélite japonés Yohkoh, nos permiten seguir la evolución de la región desde la fotosfera hasta la corona. Usando los magnetogramas del disco completo obtenidos por el Michelson Doppler Imager (SOHO/MDI) como condiciones de contorno, calculamos el campo magnético coronal y determinamos su apartamiento de la potencialidad ajustando las líneas de campo calculadas a los arcos observados en rayos X blandos. Discutimos la evolución de la torsión del campo magnético coronal y su probable relación con la actividad observada en forma de eyecciones de masa coronal (CMEs) y fulguraciones.An activity complex was observed on the solar disk between April, 1996 and February, 1997 that reached its highest level of activity during the birth of AR 7978. Our observations extend over six solar rotations, from the emergence of AR 7978 (July 1996) until the decay and dispersion of its flux (November 1996). Multi-wavelength observations, provided by instruments aboard the Solar and Heliospheric Observatory (SOHO) and the Japanese spacecraft Yohkoh, follow the evolution of the region from the photosphere to the corona. Using full disk magnetograms obtained by the Michelson Doppler Imager (SOHO/MDI) as boundary condition, we calculate the coronal magnetic field and determine its shear by fitting the computed field lines to the observed soft X-ray loops. We discuss the evolution of the coronal field shear and its probable relation to flare and coronal mass ejection activity.Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: van Driel Gesztelyi, Lidia. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Thompson, B.. National Aeronautics And Space Administration; Estados UnidosFil: Plunkett, S. P.. Spece Sciences División. Naval Research Laboratory; Estados UnidosFil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Aulanier, G.. Centre National de la Recherche Scientifique. Observatoire de Paris; Franci

Stereoscopic Polar Plume Reconstructions from Stereo/Secchi Images

We present stereoscopic reconstructions of the location and inclination of polar plumes of two data sets based on the two simultaneously recorded images taken by the EUVI telescopes in the SECCHI instrument package onboard the \emph{STEREO (Solar TErrestrial RElations Observatory)} spacecraft. The ten plumes investigated show a superradial expansion in the coronal hole in 3D which is consistent with the 2D results. Their deviations from the local meridian planes are rather small with an average of $6.47^{\circ}$. By comparing the reconstructed plumes with a dipole field with its axis along the solar rotation axis, it is found that plumes are inclined more horizontally than the dipole field. The lower the latitude is, the larger is the deviation from the dipole field. The relationship between plumes and bright points has been investigated and they are not always associated. For the first data set, based on the 3D height of plumes and the electron density derived from SUMER/\emph{SOHO} Si {\sc viii} line pair, we found that electron densities along the plumes decrease with height above the solar surface. The temperature obtained from the density scale height is 1.6 to 1.8 times larger than the temperature obtained from Mg {\sc ix} line ratios. We attribute this discrepancy to a deviation of the electron and the ion temperatures. Finally, we have found that the outflow speeds studied in the O {\sc vi} line in the plumes corrected by the angle between the line of sight and the plume orientation are quite small with a maximum of 10 $\mathrm{km s^{-1}}$. It is unlikely that plumes are a dominant contributor to the fast solar wind.Comment: 25 pages, 13 figure