Zu drei Typen der palatinischen Campanaplatten

Vor einer Generation, als Grabungen am Palatin das Haus des Augustus beim Heiligtum des Apollo zutage brachten, wurden architektonische Tonreliefs der frühaugusteischen Zeit gefunden. Von diesen werden hier drei zusammengehörende Typen neu nach ihrem Inhalt befragt. Sie sind trotz ihres ornamentalen Charakters Zeitzeugnisse; doch steht Hercules beim Dreifußstreit nicht, wie bisher zum Teil angenommen, für Marcus Antonius. Da uns der gleiche Relieftypus am römischen Capitol wie am entsprechenden Heiligtum in Cosa begegnet, weist er auf den ältesten Orakelgott Jupiter hin. Bei ihm waren in Rom die sibyllinischen Orakel aufbewahrt, bis Augustus sie 12 v.Chr. in den palatinischen Tempel überführte. Der Plan dazu dürfte nach Aussage der Campanareliefs schon früher bestanden haben: Apollo und Hercules versöhnen sich nach dem Willen ihres Vaters Jupiter und ersetzen ihn als Orakelgott. Der Palatin wurde zum Parnass, und Hercules hatte in Ostia und Latium Orakelstätten.A generation ago, when excavations at the Palatine unearthed the house of Augustus near the sanctuary of Apollon, architectural clay reliefs of the early augustean period were discovered. Of these, three interrelated types are reanalysed for their meaning. Despite their ornamental character they need to be treated as documents; contrary to previous opinion, in the scene depicting an argument about a tripod Hercules does not stand for Marcus Antonius. Th e same type of relief also exists on the Roman Capitol and the Sanctuary in Cosa, and hence refers to Jupiter as the oldest god of oracles. At the temple of Jupiter Capitolinus the Sibylline oracles were kept until Augustus transferred them to the Palatine in 12 BC. By the interpretation of the Campana reliefs proposed here, the plan to transfer the Sibylline oracles was formed earlier: Apollo and Hercules reconcile their diff erences according to the will of their father Jupiter and replace him as the god of oracles. Th e Palatine became the Parnass, and Hercules had oracles at Ostia and in Latium.Hace una generación, cuando las excavaciones en el Palatino descubierto la casa de Augusto, cerca del santuario de Apolo, de arquitectura relieves de barro de principios del periodo de Augusto fueron descubiertos. De éstos, tres tipos interrelacionados se volvieron a analizar su significado. A pesar de su carácter ornamental que necesitan ser tratados como documentos, en contra a la opinión anterior, en la escena que representa un argumento sobre un trípode Hércules no representa a Marco Antonio. Th e mismo tipo de alivio También existe en el Capitolio romano y el Santuario de la Cosa, y por lo tanto se refiere a Júpiter como el dios más antiguo de los oráculos. En el templo de Júpiter Capitolino oráculos sibilinos del fueron mantenidos hasta que Augusto los trasladó a la colina Palatina, en el año 12 aC. En la interpretación de la Campana relieves que aquí se propone, el plan para transferir los oráculos sibilinos se formó antes: Apolo y Hércules conciliar sus rencias según diff a la voluntad de su padre Júpiter y reemplazarlo como el dios de los oráculos. Th e Palatino se convirtió en el Parnaso, y el Hércules tuvo oráculos en Ostia, y en el Lacio

Investigation of heat transfer phenomenon in green peas at fluid bed draying and tray drying

In this paper, the heat transfer was studied in case of spherical material. Green peas were dried in a heat pump operated tray- and fluid bed dryer. The weight loss and the water content of the product were tested during each measuring set on different temperature levels. The physical properties of the samples were measured in the interest of determination of heat transfer data. The calculation of heat transfer on the basis of measured data was shown a difference from the results of heat transfer data - including dimensionless equations - derived from literature

Experimental study of heat and mass transfer in porous spheres during drying

The heat and mass transfer was studied in case of porous material. The models were spheres which were made in different sizes from gypsum and the mixtures of gypsum and paper. The weight loss, the water content and the temperature of the product were tested on different air velocities during each experiment. The physical properties of the samples were measured in the interest of determination of heat transfer data. The calculated heat transfer coefficients on the basis of measured data have shown a difference from the results of heat transfer data - including dimensionless equations - derived from literature. The mass transfer was studied during the steady-state period and the results confirm the tendency the dimensionless Sh equations suggested in the literature

Validation of an Instrument to Assess Fear Avoidance in Adolescents Who Have Been Diagnosed with a Concussion

Please enjoy Volume 6, Issue 1 of the JSMAHS. In this issue, you will find Professional, Graduate, and Undergraduate research abstracts, and case reports. Thank you for viewing this 6th Annual OATA Special Edition

Post-Outburst Observations of V1647 Ori: Detection of a Brief Warm, Molecular Outflow

We present new observations of the fundamental ro-vibrational CO spectrum of V1647 Ori, the young star whose recent outburst illuminated McNeil's Nebula. Previous spectra, acquired during outburst in 2004 February and July, had shown the CO emission lines to be broad and centrally peaked-similar to the CO spectrum of a typical classical T Tauri star. In this paper, we present CO spectra acquired shortly after the luminosity of the source returned to its pre-outburst level (2006 February) and roughly one year later (2006 December and 2007 February). The spectrum taken in 2006 February revealed blue-shifted CO absorption lines superimposed on the previously observed CO emission lines. The projected velocity, column density, and temperature of this outflowing gas was 30 km/s, 3^{+2}_{-1}E18 cm^{-2$, and 700^{+300}_{-100} K, respectively. The absorption lines were not observed in the 2006 December and 2007 February data, and so their strengths must have decreased in the interim by a factor of 9 or more. We discuss three mechanisms that could give rise to this unusual outflow.Comment: 14 pages, 2 figures, accepted for publication in ApJ

Dust Stratification in Young Circumstellar Disks

We present high-resolution infrared spectra of four YSOs (T Tau N, T Tau S, RNO 91, and HL Tau). The spectra exhibit narrow absorption lines of 12CO, 13CO, and C18O as well as broad emission lines of gas phase12CO. The narrow absorption lines of CO are shown to originate from the colder circumstellar gas. We find that the line of sight gas column densities resulting from the CO absorption lines are much higher than expected for the measured extinction for each source and suggest the gas to dust ratio is measuring the dust settling and/or grain coagulation in these extended disks. We provide a model of turbulence, dust settling and grain growth to explain the results. The techniques presented here allow us to provide some observationally-motivated bounds on accretion disk alpha in protostellar systems

When Quantum Fluctuations Meet Structural Instabilities: The Isotope- and Pressure-Induced Phase Transition in the Quantum Paraelectric NaOH

Anhydrous sodium hydroxide, a common and structurally simple compound, shows spectacular isotope effects: NaOD undergoes a first-order transition, which is absent in NaOH. By combining ab initio electronic structure calculations with path integrals, we show that NaOH is an unusual example of a quantum paraelectric: zero-point quantum fluctuations stretch the weak hydrogen bonds (HBs) until they become unstable and break. By strengthening HBs via isotope substitution or applied pressure, the system can be driven down to a broken-symmetry antiferroelectric phase. We also provide a simple quantitative criterion for HB breaking in layered crystals and show that nuclear quantum effects are crucial in paraelectric to ferroelectric transitions in hydrogen-bonded hydroxides

Discovery of CO Gas in the Inner Disk of TW Hydrae

We report the detection of rovibrationally excited CO emission from the inner disk of the classical T Tauri star (cTTS) TW Hya. We observe ~6 × 1021 g of CO gas with a rotational temperature of 430 ± 40 K. The linearity of the excitation plot suggests that the CO is optically thin. Atypical for cTTSs, hot CO was not detected, implying that TW Hya has cleared its inner disk region out to a radial distance of ~0.5 AU. We discuss implications for the structure of the disk as it relates to replenishment and planet formation