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Anders als in religionspolemischen Werken früherer Autoren, die auf die exegetische Diskussion zentriert sind, argumentiert Petrus Alfonsi in seinem Dialogus (um 1110 verfasst) gleichermaßen auf der Grundlage von auctoritas (der Bibel) und von ratio. In diesem Beitrag wird diskutiert, wie Petrus Alfonsi die vernunftbasierte Argumentation begrifflich fasst und umsetzt. An einer Stelle präzisiert Petrus Alfonsi drei Quellen der rationalen Erkenntnis. Die Aussage wird anhand einer genauen Lektüre und durch die Heranziehung der Quelle, das Werk des jüdischen Philosophen Saadia Gaon, Emunoth we-Deoth, interpretiert. Petrus Alfonsi unterscheidet darin die spontane Erkenntnis durch die Sinne, die deduktive Argumentation auf der Grundlage von allgemein anerkannten Prämissen (necessariae rationes) und die similitudo, die sich als die evidenzbasierte Argumentation verstehen lässt. Im Dialogus argumentiert Petrus Alfonsi nur selten auf der Grundlage von Prämissen, immer wieder findet sich eine Argumentation, die auf beobachtbaren Phänomenen basiert. Häufig legt Petrus Erkenntnisse der Naturphilosophie dar, die er durch Naturbespiele erläutert. Für dieses Verfahren setzt er auch den Begriff similitudo ein.

Die anonyme astronomische Schrift Preceptum Canonis Ptolomei wurde 534/5 vielleicht in Rom verfasst und gilt als eine Quelle des Kapitels zur Astronomie in Cassiodors nur wenig jüngeren Institutiones, in denen der berühmte Staats-mann eine Art Literaturkanon vorstellt. Eine genauere Betrachtung führt jedoch zum Schluss, dass Cassiodor das Preceptum nicht heranzog. Von Ptolemaios’ astronomischen Schriften scheint er nur die Procheiroi kanones eingesehen zu haben, mit deren griechischem Text er jedoch sehr unbeholfen umgeht. Wir vermuten daher, Cassiodor habe das ihm von der Materie her fremde Werk nicht selber konsultiert, sondern diese Aufgabe an eine Hilfskraft delegiert.

We give a closed form evaluation of the zeta determinant of the Laplace operator on spheres and projective spaces that clearly describes the arithmetic structure of this number. All the factors in the final formula for the determinant are easily computable.

Objective: Medical conversation plays a central role in disease management and therapy. In teaching, standardized patients (SPs) are increasingly being used to present conversation situations with students and provide feedback afterwards. In order to maintain this teaching concept under pandemic conditions, a digital model was developed that should offer both high security and high authenticity. Methodology: A total of 176 teaching units of 45 minutes each were conducted digitally from May to August 2020. During the teaching units, medical students conducted interviews with SPs portraying various patients. The online conference software "HeiConf" was used for this purpose. During the teaching units, a total of 354 students were able to practice conversation techniques such as NURSE and SPIKES. After the teaching units, feedback was provided by students and SPs. Results: The digital lessons about medical conversation with SPs received positive feedback from SPs and students. The authenticity of the role portrayal of SPs seemed to be unaffected by the new format. Students were successful in training and observing conversation techniques. However, aspects of non-verbal communication, atmosphere and group dynamics as well as further discussions could not be carried out to the same extent as in the usual classroom teaching.Conclusion: The conversion of SP-based teaching to a digital format was successful in a short period of time and was able to prevent a cancellation of teaching units about medical conversation. Concrete conversation techniques could be tried out digitally by students. Due to the deficits of digital teaching in terms of non-verbal communication and atmosphere, a blended-learning format is planned for the future. In the first instance, concrete conversation techniques will be learned online in order to focus more on profound aspects of communication and discussions in a later physical teaching unit with SPs, thus enabling a learning experience that is as, Zielsetzung: Die ärztliche Gesprächsführung spielt eine zentrale Rolle bei der Krankheitsbewältigung und Therapie. In der Lehre kommen immer häufiger Simulationspersonen (SPs) zum Einsatz, die mit den Studierenden Gesprächssituationen darstellen und im Anschluss Feedback geben. Um dieses Unterrichtskonzept auch unter Pandemiebedingungen aufrechtzuerhalten, wurde ein digitales Modell entwickelt, das sowohl hohe Sicherheit, als auch hohe Authentizität bieten sollte. Methodik: Insgesamt wurden von Mai bis August 2020 176 Unterrichtseinheiten à 45 Minuten digital durchgeführt. Im Rahmen der Unterrichtseinheiten führten Medizinstudierende Gespräche mit SPs, die verschiedene PatientInnen darstellten. Hierbei wurde die Online-Konferenz-Software "HeiConf" genutzt. Im Rahmen der Unterrichtseinheiten konnten insgesamt 354 Studierenden Gesprächstechniken wie NURSE und SPIKES üben. Im Anschluss an die Unterrichtseinheiten wurde eine Rückmeldung von Studierenden und SPs eingeholt. Ergebnisse: Der digitale Unterricht zu ärztlicher Gesprächsführung mit SPs erhielt positive Rückmeldungen seitens der SPs und Studierenden. Die Authentizität der Rollendarstellung der SPs erschien von dem neuen Format unbeeinträchtigt. Das Trainieren und Beobachten von Gesprächstechniken gelang Studierenden gut. Aspekte der nonverbalen Kommunikation, Atmosphäre und Gruppendynamik sowie weiterführende Diskussionen konnten jedoch nicht in dem Umfang aufgegriffen werden, wie dies bei der üblichen Präsenzlehre geschieht.Schlussfolgerung: Die Umstellung der SP-basierten Lehre auf ein digitales Format ist in kurzer Zeit gelungen und konnte einen Ausfall des Unterrichts zu ärztlicher Gesprächsführung verhindern. Konkrete Gesprächstechniken konnten digital von Studierenden erprobt werden. Aufgrund der Defizite von digitalem Unterricht in Bezug auf nonverbale Kommunikation und Atmosphäre wird für die Zukunft ein Blended-Learning-Format angestrebt. Hierbei sollen zunächst konkrete Gesprächstechniken online erler

The evolution of young stars and disks is driven by the interplay of several processes, notably accretion and ejection of material. Critical to correctly describe the conditions of planet formation, these processes are best probed spectroscopically. About five-hundred orbits of the Hubble Space Telescope (HST) are being devoted in 2020-2022 to the ULLYSES public survey of about 70 low-mass (M<2Msun) young (age<10 Myr) stars at UV wavelengths. Here we present the PENELLOPE Large Program that is being carried out at the ESO Very Large Telescope (VLT) to acquire, contemporaneous to HST, optical ESPRESSO/UVES high-resolution spectra to investigate the kinematics of the emitting gas, and UV-to-NIR X-Shooter medium-resolution flux-calibrated spectra to provide the fundamental parameters that HST data alone cannot provide, such as extinction and stellar properties. The data obtained by PENELLOPE have no proprietary time, and the fully reduced spectra are made available to the whole community. Here, we describe the data and the first scientific analysis of the accretion properties for the sample of thirteen targets located in the Orion OB1 association and in the sigma-Orionis cluster, observed in Nov-Dec 2020. We find that the accretion rates are in line with those observed previously in similarly young star-forming regions, with a variability on a timescale of days of <3. The comparison of the fits to the continuum excess emission obtained with a slab model on the X-Shooter spectra and the HST/STIS spectra shows a shortcoming in the X-Shooter estimates of <10%, well within the assumed uncertainty. Its origin can be either a wrong UV extinction curve or due to the simplicity of this modelling, and will be investigated in the course of the PENELLOPE program. The combined ULLYSES and PENELLOPE data will be key for a better understanding of the accretion/ejection mechanisms in young stars., Comment: Accepted for publication on Astronomy & Astrophysics. 15 pages + appendix, language edited version

We give an explicit formula for the L2 analytic torsion of the finite metric cone over an oriented compact connected Riemannian manifold. We provide an interpretation of the different factors appearing in this formula. We prove that the analytic torsion of the cone is the finite part of the limit obtained collapsing one of the boundaries, of the ratio of the analytic torsion of the frustum to a regularising factor. We show that the regularising factor comes from the set of the non square integrable eigenfunctions of the Laplace Beltrami operator on the cone.

In this paper, we present explicit formulas for the analytic torsion of an half sphere.

The Front Cover shows Escherichia coli (E. coli) as a production chassis for microbial electrochemical synthesis. This was exemplified for the conversion of acetophenone to (R)‐1‐phenylethanol with a stereoselectivity of >99 %ee by a heterologously expressed alcohol dehydrogenase of Lactobacillus brevis. The wiring of the NAD(P)+/NAD(P)H,H+ ‐ pool of E. coli to the electrode was achieved using methyl viologen, which is colorless if oxidized and deep violet in its reduced state, as mediator combined with molecular engineering using “wire” proteins from the periplasm of Shewanella oneidensis, being a model for electroactive microorganisms. This proof‐of‐concept already demonstrates a coulombic efficiency of up to 50% and a yield of approximately 40%. Thus, the work clearly lays the foundation for further microbial electrochemical synthesis of valuable pharmaceuticals and chemical building blocks. More information can be found in the Communication by J. C. Mayr et al. on page 1631 in Issue 8, 2019 (DOI: 10.1002/cssc.201900413).

Integration of existing isotopic and geological data allows a reconsideration of the distribution and age of the Río de la Plata Craton within South America. The reinterpretation increases the area of the craton to about 2,400,000 km2 with implications for the tectonic map of South America and for global reconstruction of palaeocontinents. Four areas previously considered as separate cratons (Luís Alves, Curitiba, Tebicuary, and Paranapanema) are interpreted as part of the same Río de la Plata Craton. The craton is organized into six provinces and domains: Buenos Aires–Piedra Alta, Taquarembó, Tebicuary, Luís Alves, Encantadas, and Nico Pérez. The term ‘Transplatense’ is proposed to replace ‘Trans-Amazonian’ for Rhyacian events that occurred within the Río de la Plata Craton. The craton is formed not only by dominant Rhyacian rocks and local Archaean rocks, but also by Statherian and Mesoproterozoic rocks. The domains are all partially to totally covered by Phanerozoic basins (Paraná, Chacoparanense, Claromecó, Salado, Balcarce, and Colorado) which makes their investigation difficult. The Ediacaran–Cambrian collisions of the Brasilian orogen generated tectonic mixtures of orogenic and cratonic zones. This is more evident in the eastern margin of the craton, which behaved as a metacraton.

In order to look for signs of on-going planet formation in young disks, we carried out the first J-band polarized emission imaging of the Herbig Ae/Be stars HD 150193, HD 163296, and HD 169142 using the Gemini Planet Imager (GPI), along with new H band observations of HD 144432. We confirm the complex "double ring" structure for the nearly face-on system HD 169142 first seen in H-band, finding the outer ring to be substantially redder than the inner one in polarized intensity. Using radiative transfer modeling, we developed a physical model that explains the full spectral energy distribution (SED) and J- and H-band surface brightness profiles, suggesting that the differential color of the two rings could come from reddened starlight traversing the inner wall and may not require differences in grain properties. In addition, we clearly detect an elongated, off-center ring in HD 163296 (MWC 275), locating the scattering surface to be 18 AU above the midplane at a radial distance of 77 AU, co-spatial with a ring seen at 1.3mm by ALMA linked to the CO snow line. Lastly, we report a weak tentative detection of scattered light for HD 150193 (MWC 863) and a non-detection for HD 144432; the stellar companion known for each of these targets has likely disrupted the material in the outer disk of the primary star. For HD 163296 and HD 169142, the prominent outer rings we detect could be evidence for giant planet formation in the outer disk or a manifestation of large-scale dust growth processes possibly related to snow-line chemistry., Comment: Accepted Astrophysical Journal

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We present a near-IR survey for the visual multiples in the Orion molecular clouds region at separations between 100 and 1000 AU. These data were acquired at 1.6~$\mu$m with the NICMOS and WFC3 cameras on the Hubble Space Telescope. Additional photometry was obtained for some of the sources at 2.05~$\mu$m with NICMOS and in the $L'$-band with NSFCAM2 on the IRTF. Towards 129 protostars and 197 pre-main sequence stars with disks observed with WFC3, we detect 21 and 28 candidate companions between the projected separations of 100---1000 AU, of which less than 5 and 8, respectively, are chance line of sight coincidences. The resulting companion fraction ($CF$) after the correction for the line of sight contamination is 14.4$^{+1.1}_{-1.3}$% for protostars and 12.5$^{+1.2}_{-0.8}$% for the pre-main sequence stars. These values are similar to those found for main sequence stars, suggesting that there is little variation in the $CF$ with evolution, although several observational biases may mask a decrease in the $CF$ from protostars to the main sequence stars. After segregating the sample into two populations based on the surrounding surface density of YSOs, we find that the $CF$ in the high stellar density regions ($\Sigma_{YSO} > 45$~pc$^{-2}$) is approximately 50% higher than that found in the low stellar density regions ($\Sigma_{YSO} < 45$~pc$^{-2}$). We interpret this as evidence for the elevated formation of companions at 100 to 1000 AU in the denser environments of Orion. We discuss possible reasons for this elevated formation., Comment: 20 pages, 7 tables, 22 figures Accepted to ApJ

We present key results from the Herschel Orion Protostar Survey (HOPS): spectral energy distributions (SEDs) and model fits of 330 young stellar objects, predominantly protostars, in the Orion molecular clouds. This is the largest sample of protostars studied in a single, nearby star-formation complex. With near-infrared photometry from 2MASS, mid- and far-infrared data from Spitzer and Herschel, and sub-millimeter photometry from APEX, our SEDs cover 1.2-870 $\mu$m and sample the peak of the protostellar envelope emission at ~100 $\mu$m. Using mid-IR spectral indices and bolometric temperatures, we classify our sample into 92 Class 0 protostars, 125 Class I protostars, 102 flat-spectrum sources, and 11 Class II pre-main-sequence stars. We implement a simple protostellar model (including a disk in an infalling envelope with outflow cavities) to generate a grid of 30400 model SEDs and use it to determine the best-fit model parameters for each protostar. We argue that far-IR data are essential for accurate constraints on protostellar envelope properties. We find that most protostars, and in particular the flat-spectrum sources, are well-fit. The median envelope density and median inclination angle decrease from Class 0 to Class I to flat-spectrum protostars, despite the broad range in best-fit parameters in each of the three categories. We also discuss degeneracies in our model parameters. Our results confirm that the different protostellar classes generally correspond to an evolutionary sequence with a decreasing envelope infall rate, but the inclination angle also plays a role in the appearance, and thus interpretation, of the SEDs., Comment: Accepted by ApJS; 87 pages; 2 online-only figure sets; corrected typos and other minor fixes

We analyze the spatial distribution of dusty young stellar objects (YSOs) identified in the Spitzer Survey of the Orion Molecular clouds, augmenting these data with Chandra X-ray observations to correct for incompleteness in dense clustered regions. We also devise a scheme to correct for spatially varying incompleteness when X-ray data are not available. The local surface densities of the YSOs range from 1 pc$^{-2}$ to over 10,000 pc$^{-2}$, with protostars tending to be in higher density regions. This range of densities is similar to other surveyed molecular clouds with clusters, but broader than clouds without clusters. By identifying clusters and groups as continuous regions with surface densities $\ge10$ pc$^{-2}$, we find that 59% of the YSOs are in the largest cluster, the Orion Nebular Cluster (ONC), while 13% of the YSOs are found in a distributed population. A lower fraction of protostars in the distributed population is evidence that it is somewhat older than the groups and clusters. An examination of the structural properties of the clusters and groups show that the peak surface densities of the clusters increase approximately linearly with the number of members. Furthermore, all clusters with more than 70 members exhibit asymmetric and/or highly elongated structures. The ONC becomes azimuthally symmetric in the inner 0.1 pc, suggesting that the cluster is only $\sim 2$ Myr in age. We find the star formation efficiency (SFE) of the Orion B cloud is unusually low, and that the SFEs of individual groups and clusters are an order of magnitude higher than those of the clouds. Finally, we discuss the relationship between the young low mass stars in the Orion clouds and the Orion OB 1 association, and we determine upper limits to the fraction of disks that may be affected by UV radiation from OB stars or by dynamical interactions in dense, clustered regions., Comment: Accepted to AJ. Higher resolution and two column version of paper as well as photometry data available at http://astro1.physics.utoledo.edu/~megeath/Orion/The_Spitzer_Orion_Survey.html

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Ion microprobe age determinations of 102 detrital zircon crystals from a sand extrudite, Cretaceous Paraná volcanic province, set limits on the origin of the numerous sand layers present in this major flood basalt province. The zircon U-Pb ages reflect four main orogenic cycles: Mesoproterozoic (1155-962 Ma), latest Proterozoic-early Cambrian (808-500 Ma) and two Palaeozoic (Ordovician– 480 to 450 Ma, and Permian to Lower Triassic– 296 to 250 Ma). Two additional small concentrations are present in the Neoarchean (2.8 to 2.6 Ga) and Paleoproterozoic (2.0 to 1.7 Ga). Zircon age peaks closely match the several pulses of igneous activity in the Precambrian Brazilian Shield and active orogeny in Argentina. A main delimitation of the origin of the sand is the absence of zircon ages from the underlying Cretaceous basalts, thus supporting an injectite origin of the sand as an extrudite that emanated from the paleoerg that constitutes the Botucatu Formation.

We present an education paradigm that stimulates innovation and entrepreneurship through a master's-level university course: "Turning Technology into Business". The course was specifically designed to connect technological research with education using patented technologies developed at the research faculties of a technical university in the Netherlands. We outline the structure and the main content of the course and explain the selection process of both the patents used in the course and the students admitted to the course. This program was initiated at Delft University of Technology in 2003 and has resulted in 10 startups that have commercialized new technologies and at least two additional dozen startups that are indirect spinoffs. To illustrate the potential of this approach, we describe the case of Holland Container Innovations, a company founded by students who developed a foldable sea container during the course., Copyright - Copyright Talent First Network Dec 2014 Last updated - 2014-12-19, Delft Centre for Entrepreneurship

Delft Centre for Entrepreneurship

Delft Centre for Entrepreneurship

Purpose – Durham Zoo (hereinafter – DZ) is a project to design and operate a concept search engine for science and technology. In DZ, a concept includes a solution to a problem in a particular context. Design – Concept searching is rendered complex by the fuzzy nature of a concept, the many possible implementations of the same concept, and the many more ways that the many implementations can be expressed in natural language. An additional complexity is the diversity of languages and formats, in which the concepts can be disclosed. Humans understand language, inference, implication and abstraction and, hence, concepts much better than computers, that in turn are much better at storing and processing vast amounts of data. We are 7 billion on the planet and we have the Internet as the backbone for Collective Intelligence. So, our concept search engine uses humans to store concepts via a shorthand that can be stored, processed and searched by computers: so, humans IN and computers OUT. The shorthand is classification: metadata in a structure that can define the content of a disclosure. The classification is designed to be powerful in terms of defining and searching concepts, whilst suited to a crowdsourcing effort. It is simple and intuitive to use. Most importantly, it is adapted to restrict ambiguity, which is the poison of classification, without imposing a restrictive centralised management. In the classification scheme, each entity is shown together in a graphical representation with related entities. The entities are arranged on a sliding scale of similarity. This sliding scale is effectively fuzzy classification. Findings – The authors of the paper have been developing a first classification scheme for the technology of traffic cones, this in preparation for a trial of a working system. The process has enabled the authors to further explore the practicalities of concept classification. The CmapTools knowledge modelling kit to develop the g, Delft Centre for Entrepreneurship

Searching for concepts in science and technology is often a difficult task. To facilitate concept search, different types of human-generated metadata have been created to define the content of scientific and technical disclosures. Classification schemes such as the International Patent Classification (IPC) and MEDLINE's MeSH are structured and controlled, but require trained experts and central management to restrict ambiguity (Mork, 2013). While unstructured tags of folksonomies can be processed to produce a degree of structure (Kalendar, 2010; Karampinas, 2012; Sarasua, 2012; Bragg, 2013) the freedom enjoyed by the crowd typically results in less precision (Stock 2007). Existing classification schemes suffer from inflexibility and ambiguity. Since humans understand language, inference, implication, abstraction and hence concepts better than computers, we propose to harness the collective wisdom of the crowd. To do so, we propose a novel classification scheme that is sufficiently intuitive for the crowd to use, yet powerful enough to facilitate search by analogy, and flexible enough to deal with ambiguity. The system will enhance existing classification information. Linking up with the semantic web and computer intelligence, a Citizen Science effort (Good, 2013) would support innovation by improving the quality of granted patents, reducing duplicitous research, and stimulating problem-oriented solution design. A prototype of our design is in preparation. A crowd-sourced fuzzy and faceted classification scheme will allow for better concept search and improved access to prior art in science and technology. Crowd-Sourcing Fuzzy and Faceted Classification for Concept Search | Request PDF. Available from: https://www.researchgate.net/publication/263544917_Crowd-Sourcing_Fuzzy_and_Faceted_Classification_for_Concept_Search [accessed Jul 26 2018]., Delft Centre for Entrepreneurship

First phases of the process of star formation are characterized by excess in infrared and high X-ray emission. With Spitzer and XMM-Newton we have surveyed the Orion A part relative to the filamentary cloud Lynds 1641 (L1641). Furthermore, an extended spectroscopic survey has been realized to better constraint the cluster membership of stars without IR excess.

New U-Pb zircon geochronological data integrated with field relationships and an airborne geophysical survey suggest that the Nova Brasilândia and Aguapeí belts are part of the same monocyclic, metaigneous and metasedimentary belt formed in the late Mesoproterozoic (1150 Ma-1110 Ma). This geological history is very similar to the within-plate origin of the Sunsás belt, in eastern Bolivia. Thus, we propose that the Nova Brasilândia, Aguapeí and Sunsás belts represent a unique geotectonic unit (here termed the Western Amazon belt) that became amalgamated at the end of the Mesoproterozoic and originated through the reactivation of a paleo-suture (Guaporé suture zone) in an intracontinental rift environment. Therefore, its geological history involves a short, complete Wilson cycle of ca. 40 Ma. Globally, this tectonic evolution may be related with the final breakup of the supercontinent Columbia. Mafic rocks and trondhjemites in the northernmost portion of the belt yielded U-Pb zircon ages ca. 1110 Ma, which dates the high-grade metamorphism and the closure of the rift. This indicates that the breakup of supercontinent Columbia was followed in short sequence by the assembly of supercontinent Rodinia at ca. 1.1-1.0 Ga and that the Western Amazon belt was formed during the accretion of the Arequipa-Antofalla basement to the Amazonian craton.

Delft Centre for Entrepreneurship

Delft Centre for Entrepreneurship

The dust sublimation walls of disks around T Tauri stars represent a directly observable cross-section through the disk atmosphere and midplane. Their emission properties can probe the grain size distribution and composition of the innermost regions of the disk, where terrestrial planets form. Here we calculate the inner dust sublimation wall properties for four classical T Tauri stars with a narrow range of spectral types and inclination angles and a wide range of mass accretion rates to determine the extent to which the walls are radially curved. Best-fits to the near- and mid-IR excesses are found for curved, 2-layer walls in which the lower layer contains larger, hotter, amorphous pyroxene grains with Mg/(Mg+Fe)=0.6 and the upper layer contains submicron, cooler, mixed amorphous olivine and forsterite grains. As the mass accretion rates decrease from 10^(-8) to 10^(-10) Msol/yr, the maximum grain size in the lower layer decreases from 3 to 0.5 microns. We attribute this to a decrease in fragmentation and turbulent support for micron-sized grains with decreasing viscous heating. The atmosphere of these disks is depleted of dust with dust-gas mass ratios 1x10^(-4) of the ISM value, while the midplane is enhanced to 8 times the ISM value. For all accretion rates, the wall contributes at least half of the flux in the optically thin 10 micron silicate feature. Finally, we find evidence for an iron gradient in the disk, suggestive of that found in our solar system., Comment: 18 pages, 12 figures, 1 table, accepted to ApJ

Using NASA IRTF SpeX data from 0.8 to 4.5 $\mu$m, we determine self-consistently the stellar properties and excess emission above the photosphere for a sample of classical T Tauri stars (CTTS) in the Taurus molecular cloud with varying degrees of accretion. This process uses a combination of techniques from the recent literature as well as observations of weak-line T Tauri stars (WTTS) to account for the differences in surface gravity and chromospheric activity between the TTS and dwarfs, which are typically used as photospheric templates for CTTS. Our improved veiling and extinction estimates for our targets allow us to extract flux-calibrated spectra of the excess in the near-infrared. We find that we are able to produce an acceptable parametric fit to the near-infrared excesses using a combination of up to three blackbodies. In half of our sample, two blackbodies at temperatures of 8000 K and 1600 K suffice. These temperatures and the corresponding solid angles are consistent with emission from the accretion shock on the stellar surface and the inner dust sublimation rim of the disk, respectively. In contrast, the other half requires three blackbodies at 8000, 1800, and 800 K, to describe the excess. We interpret the combined two cooler blackbodies as the dust sublimation wall with either a contribution from the disk surface beyond the wall or curvature of the wall itself, neither of which should have single-temperature blackbody emission. In these fits, we find no evidence of a contribution from optically thick gas inside the inner dust rim., Comment: Accepted to ApJ, 22 pages, 2 appendices, 12 figures, 7 tables

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A major Mesoproterozoic paleo-plate boundary in the southwestern Amazonian Craton, the Guaporé Suture Zone, is investigated by U–Pb zircon geochronology, Sr–Nd isotope geochemistry and aeromagnetic data. This suture zone is constituted dominantly by ophiolitic mafic–ultramafic rocks of the Trincheira Complex, and minor proportion of tonalites of the Rio Galera and São Felipe complexes, Colorado Complex, amphibolites of the Rio Alegre Terrane and syn- to late-kinematic mafic to felsic plutonic rocks. The ophiolitic Trincheira Complex formed during an accretionary phase from 1470 to 1430 Ma and was overprinted by upper amphibolite–granulite facies metamorphism during the collisional phase of the Ectasian followed by syntectonic emplacement of gabbro and granite plutons (1350–1340 Ma). The ophiolites were intruded by syntectonic tonalitic–plagiogranitic plutons ca. 1435 Ma. Mafic–ultramafic rocks of the Trincheira ophiolites show moderate to highly positive initial epsilon Nd (t = 1.46 Ga) values (+2.6 to +8.8) and very low initial 87Sr/86Sr ratio (0.7013–0.7033). It is suggested that these magmas originated from a depleted mantle source in an island-arc–back-arc setting. The identification of a fossil ophiolite in the Guaporé Suture Zone early as 1470–1435 Ma and later collisional phase, as late as 1350 Ma, marks the impingement of the proto-Amazonian Craton against the Paragua Block, before the formation of the Rodinia supercontinent. The results provide important insights into the geodynamic history of the SW Amazonian Craton, with evidence for both accretionary orogen and subduction of oceanic lithosphere in the Mesoproterozoic, and provide information that allows other workers to evaluate the configuration of supercontinents.

Hydrogels based on nanocomposites of statistical poly(hydroxyethyl acrylate-co-ethyl acrylate) and silica, prepared by simultaneous copolymerization and generation of silica nanoparticles by sol-gel process at various copolymer compositions and silica contents, characterized by a fine dispersion of filler, were investigated with respect to glass transition and polymer dynamics by dielectric techniques. These include thermally stimulated depolarization currents and dielectric relaxation spectroscopy, covering together broad ranges of frequency and temperature. In addition, equilibrium water sorption isotherms were recorded at room temperature (25 A degrees C). Special attention was paid to the investigation of effects of silica on glass transition, polymer dynamics (secondary gamma and beta (sw) relaxations and segmental alpha relaxation), and electrical conductivity in the dry systems (xerogels) and in the hydrogels at various levels of relative humidity/water content. An overall reduction of molecular mobility is observed in the nanocomposite xerogels, in particular at high silica contents. Analysis of the results and comparison with previous work on similar systems enable to discuss this reduction of molecular mobility in terms of constraints to polymeric motion imposed by interfacial polymer-filler interactions and by the formation of a continuous silica network interpenetrated with the polymer network at filler contents higher than about 15 wt%.

High-energy radiation from T Tauri stars (TTS) influences the amount and longevity of gas in disks, thereby playing a crucial role in the creation of gas giant planets. Here we probe the high-energy ionizing radiation from TTS using high-resolution mid-infrared (MIR) Spitzer IRS Neon forbidden line detections in a sample of disks from IC 348, NGC 2068, and Chamaeleon. We report three new detections of [Ne III] from CS Cha, SZ Cha, and T 54, doubling the known number of [Ne III] detections from TTS. Using [Ne III]-to-[Ne II] ratios in conjunction with X-ray emission measurements, we probe high-energy radiation from TTS. The majority of previously inferred [Ne III]/[Ne II] ratios based on [Ne III] line upper limits are significantly less than 1, pointing to the dominance of either X-ray radiation or soft Extreme-Ultraviolet (EUV) radiation in producing these lines. Here we report the first observational evidence for hard EUV dominated Ne forbidden line production in a T Tauri disk: [Ne III]/[Ne II]~1 in SZ Cha. Our results provide a unique insight into the EUV emission from TTS, by suggesting that EUV radiation may dominate the creation of Ne forbidden lines, albeit in a minority of cases., Comment: 16 pages, accepted ApJ

We present a survey of the Orion A and B molecular clouds undertaken with the IRAC and MIPS instruments onboard Spitzer. In total, five distinct fields were mapped covering 9 sq. degrees in five mid-IR bands spanning 3-24 microns. The survey includes the Orion Nebula Cluster, the Lynds 1641, 1630 and 1622 dark clouds, and the NGC 2023, 2024, 2068 and 2071 nebulae. These data are merged with the 2MASS point source catalog to generate a catalog of eight band photometry. We identify 3479 dusty young stellar objects (YSOs) in the Orion molecular clouds by searching for point sources with mid-IR colors indicative of reprocessed light from dusty disks or infalling envelopes. The YSOs are subsequently classified on the basis of their mid-IR colors and their spatial distributions are presented. We classify 2991 of the YSOs as pre-main sequence stars with disks and 488 as likely protostars. Most of the sources were observed with IRAC in 2-3 epochs over 6 months; we search for variability between the epochs by looking for correlated variability in the 3.6 and 4.5 micron bands. We find that 50% of the dusty YSOs show variability. The variations are typically small (0.2 mag.) with the protostars showing a higher incidence of variability and larger variations. The observed correlations between the 3.6, 4.5, 5.8 and 8 micron variability suggests that we are observing variations in the heating of the inner disk due to changes in the accretion luminosity or rotating accretion hot spots., Comment: Accepted to the Astronomical Journal. A full resolution version of the paper and the point source catalog can be found at http://astro1.physics.utoledo.edu/~megeath/Orion/The_Spitzer_Orion_Survey.html