bluuebunny/crossref_metadata_2025_split huggingface dataset:
From unit-and-ten to ten-before-unit order in the history of English numerals
Authors: Berg Thomas , Neubauer Marion 
Published: April 2014

AbstractIn the course of its history, English underwent a significant structural change in its numeral system. The number words from 21 to 99 switched from the unit-and-ten to the ten-before-unit pattern. This change is traced on the basis of more than 800 number words. It is argued that this change, which took seven centuries to complete and in which the Old English pattern was highly persistent, can be broken down into two parts—the reordering of the units and tens and the loss of the conjoining element. Although the two steps logically belong to the same overall change, they display a remarkably disparate behavior. Whereas the reordering process affected the least frequent number words first, the deletion process affected the most frequent words first. This disparity lends support to the hypothesis that the involvement or otherwise of low-level aspects of speech determines the role of frequency in language change (Phillips, 2006). Finally, the order change is likely to be a contact-induced phenomenon and may have been facilitated by a reduction in mental cost.
VISUALIZING UNCERTAINTIES, OR HOW ALBERT HIRSCHMAN AND THE WORLD BANK DISAGREED ON PROJECT APPRAISAL AND WHAT THIS SAYS ABOUT THE END OF “HIGH DEVELOPMENT THEORY”
Authors: Alacevich Michele 
Published: April 2014

Since its birth in 1944, the World Bank has had a strong focus on development projects. Yet, a project evaluation function was not made operational until the early 1970s. An early attempt to conceptualize project appraisal had been initiated in the 1960s by Albert Hirschman, whose undertaking raised high expectations at the Bank. Yet, Hirschman’s conclusions—published first in internal Bank reports and finally as a book in 1967—disappointed many at the Bank, primarily because they were found impractical. Hirschman attempted to offer the Bank a new Weltanschauung by transforming the Bank’s approach to project design, project management, and project appraisal. Instead, what the Bank expected from Hirschman was not a revolution, but rather an examination of the Bank’s projects and advice on how to make project design and management more measurable, more controllable, and more suitable for replication.The history of this failed collaboration gives useful insights on the unstable equilibrium between operations and evaluation within the Bank. In addition, it shows that the Bank was active in the development economics debates of the 1960s. These insights should be of interest for those development economists today who reflect on the future of the discipline and emphasize the need for a non-dogmatic approach to the study of development issues. It should also be of interest for the Bank itself, with its renewed attention to the importance of evaluation for effective development policies. The history of the practice of development economics, together with the use of archival material, can bring new perspectives that contribute to a better understanding of the evolution of this discipline.
Options to improve family income, labor input and soil organic matter balances by soil management and maize–livestock interactions. Exploration of farm-specific options for a region in Southwest Mexico
Authors: Flores-Sánchez Diego , Groot Jeroen C.J. , Lantinga Egbert A. , Kropff Martin J. , Rossing Walter A.H. 
Published: April 2014

AbstractFarming systems in the Costa Chica region in Mexico face limitations linked to low yields and soil fertility degradation. Several alternative maize-based cropping systems have been proposed to improve current limitations. These field-level options need to be evaluated at farm level in order to assess their feasibility, taking into account input requirements, contributions to self-sufficiency in food and long-term soil fertility, and the availability of labor. In this study, we defined four scenarios to explore consequences of changes in current farming systems for eight typical farms in the region; the first two scenarios comprised redressing current imbalances in crop nutrition and organic matter (OM) supply, respectively, and the last two scenarios explored high fertilizer input and animal husbandry. Farms responded in different ways to the various options depending on available land, current soil quality, current cropping systems and presence of livestock. Improvements in crop nutrition based on mineral fertilizers increased family income but only had substantial effects on soil OM (SOM) balances when fertilizer rates were double the amount currently subsidized. Addition of organic fertilizers resulted in positive effects on SOM balance, but with often strong trade-offs with family income due to costs of acquisition, transport and application. Animals played an important role in increasing SOM balances, but had relatively little effect on improving family income. The results demonstrated that improvements in family income and SOM balance at farm scale were feasible but that without more fundamental system changes trade-offs between short-term yield increases and longer-term soil fertility increases should be expected. The results highlight the need for policies that take into account farm-specific differences in crop and livestock intensification opportunities.
Transit & RV Observations of Exoplanets by the 1-m Telescope at Weihai
Authors: Cao Chen , Ren Dayong , Gao Dongyang , Zhang Jicheng , Song Nan , Wang Feige 
Published: April 2014

AbstractBy using the 1-m reflecting telescope at Weihai Observatory of Shandong University, the transit observations of seven stars are carried out to accurately estimate the physical parameters of extrasolar planets. Besides, a new high-resolution spectrograph (WES) was installed on this telescope for radial velocity measurements on exoplanets, we will show some preliminary results.
Exoplanet Searches in the Habitable Zone with Gravitational Microlensing
Authors: Zakharov Alexander F. , Ingrosso Gabriele , De Paolis Francesco , Nucita Achille A. , Strafella Francesco , Novati Sebastiano Calchi , Jetzer Philippe 
Published: April 2014

AbstractThere are different methods for finding exoplanets such as radial spectral shifts, astrometrical measurements, transits, timing, etc. Gravitational microlensing (including pixel-lensing) is among the most promising techniques with the potential of detecting Earth-like planets at distances about a few astronomical units from their host stars. Here we emphasize the importance of polarization measurements which can help to resolve degeneracies in theoretical models. In particular, the polarization angle could give additional information about the relative position of the lens with respect to the source.
Image Retrieval of Earth-like Planets from Light Curves
Authors: Kawahara Hajime , Fujii Yuka 
Published: April 2014

AbstractSurface environment of habitable exoplanets will be important for astrobiologists on exoplanets in near future. Diverse surface environments on the Earth including continents, ocean, and meteorological condition (clouds and rains) serve as the backbone of biodiversity. One of the promising approaches to know the landscape of the terrestrial exoplanets is to use scattered light of the planet through direct imaging.Since spin rotation and orbital revolution change illuminating area on planetary surface and cause time variation to disk-integrated brightness, light curves carry spatial information on the planetary surface. We propose an inversion technique of annual reflected light curves to sketch a two-dimensional albedo map of exoplanets, named the spin-orbit tomography (SOT). Applying the SOT to realistic simulations of the reflected light of an Earth-twin, we demonstrate how the SOT works. The mean cloud and continental distributions can be roughly obtained with single band photometry and difference of two-bands photometry, respectively. The SOT retrieves the planetary image without actually resolving the planet, which can be used to know the habitat of the exoplanets in near future.
Detection of a Proto-planetary Clump in the Habitable Zone of GM Cephei
Authors: Chen W. P. , Hu S. C.-L. ,   the YETI Collaboration
Published: April 2014

AbstractGM Cephei is an active T Tauri star in the young open cluster Trumpler 37, showing abrupt UX Orionis type of photometric variability. Its light curves exhibit frequent, sporadic brightening events, each of <0.5 mag and lasting for days, which must have been originated from unsteady circumstellar accretion. In addition, the star undergoes a brightness drop up to ~1 mag lasting for about a month, during which the star became bluer when fainter. Moreover, the brightness drops seem to have a recurrence timescale of about 300 days. It is proposed that the brightness drop arises from obscuration of the central star by an orbiting dust concentration, exemplifying disk inhomogeneity in transition between grain coagulation and planetesimal formation in a young circumstellar disk. GM Cep was found to show a few percent polarization in the optical wavelengths, and an enhanced level of polarization during the occultation phase.
Exploring the Cosmic Context of Earth
Authors: Dominik Martin 
Published: April 2014

AbstractStudying the amazingly diverse planet zoo provides us with unprecedented opportunities for understanding planet Earth and ultimately ourselves. An assessment of a planet's “habitability” reflects our Earth-centric prejudice and can serve to prioritise targets to actually search for signatures of life similar to ours. The probability for life beyond Earth to exist however remains unknown, and studies on habitability or statistics of planetary systems do not change this. But we can leave speculation behind, and embark on a journey of exploration. A sample of detected cosmic habitats would provide us with insight on the conditions for life to emerge, develop, and sustain, but disentangling the biota fraction from the duration of the biotic era would depend particularly on our knowledge about the dynamics of planetary systems. Apart from the fact that planets usually do not come alone, we also must not forget that the minor bodies in the Solar system vastly outnumber the planets. A focus on just what we might consider “habitable” planets is too narrow to understand their formation and evolution. While uniqueness prevents understanding, we need to investigate the context and embrace diversity. A comprehensive picture of planet populations can only arise by exploiting a variety of different detection techniques, where not only Kepler but also gravitational microlensing can now enter hitherto uncharted territory below the mass or size of the Earth. There is actually no shortage of planets, the Milky Way alone may host hundreds of billions, and so far we have found only about 1000.
Evidence for Solid Planets from Kepler's Near-Resonance Systems
Authors: Lee Man Hoi , Fabrycky D. , Lin D. N. C. 
Published: April 2014

AbstractThe multiple-planet systems discovered by the Kepler mission show an excess of planet pairs with period ratios just wide of exact commensurability for first-order resonances like 2:1 and 3:2. In principle, these planet pairs could be in resonance if their orbital eccentricities are sufficiently small, because the width of first-order resonances diverges in the limit of vanishingly small eccentricity. We consider a widely-held scenario in which pairs of planets were captured into first-order resonances by migration due to planet-disk interactions, and subsequently became detached from the resonances, due to tidal dissipation in the planets. In the context of this scenario, we find a constraint on the ratio of the planet's tidal dissipation function and Love number that implies that some of the Kepler planets are likely solid. However, tides are not strong enough to move many of the planet pairs to the observed separations, suggesting that additional processes are at play.
Observation and Modelling of Transits and Starspots in the WASP-19 Planetary System
Authors: Tregloan-Reed Jeremy , Southworth John 
Published: April 2014

AbstractWe have developed a new model for analysing light curves of planetary transits when there are starspots on the stellar disc. Because the parameter space contains a profusion of local minima we developed a new optimisation algorithm which combines the global minimisation power of a genetic algorithm and the Bayesian statistical analysis of the Markov chain. With these tools we modelled three transit light curves of WASP-19. Two light curves were obtained on consecutive nights and contain anomalies which we confirm as being due to the same spot. Using these data we measure the star's rotation period and velocity to be 11.76 ± 0.09 d and 3.88 ± 0.15 kms−1, respectively, at a latitude of 65°. We find that the sky-projected angle between the stellar spin axis and the planetary orbital axis is λ = 1.0° ± 1.2°, indicating axial alignment. Our results are consistent with and more precise than published spectroscopic measurements of the Rossiter-McLaughlin effect.
High Precision Photometry from EulerCam and TRAPPIST: The Case of WASP-42, WASP-49 and WASP-50
Authors: Lendl Monika , Gillon Michaël , Queloz Didier 
Published: April 2014

AbstractTransiting extrasolar planets provide unmatched insights into the structure and composition of close-in planets. When a planet transits its host star, its radius is known, which together with radial velocity measurements, allows accessing the planetary density. We present results obtained using the Euler and TRAPPIST telescopes that aim at reaching very high accuracy on the parameters derived from transit lightcurves. Here, we show the case of the recently discovered WASP-42b and WASP-49b and new observations of WASP-50b.
Aspects on the Dynamics and Detection of Additional Circumbinary Extrasolar Planets
Authors: Hinse Tobias C. , Haghighipour Nader , Goździewski Krzysztof 
Published: April 2014

AbstractThe presence of additional bodies orbiting a binary star system can be detected by monitoring the binary's eclipse timing. These so-called circumbinary objects will reveal themselves by i) either introducing a reflex motion of the binary system about the total system's barycenter creating a geometric light-travel time effect (LITE), ii) by gravitational perturbations on the binary orbit, or iii) a combination of the two effects resulting in eclipse timing (ETV) and transit timing (TTV) variations. Motivated by the four recently detected circumbinary planets by the Kepler space telescope (Kepler-16b, Kepler-34b, Kepler-35b and Kepler-38b) we have begun to study their dynamics in the presence of an additional massive perturber. In particular we used Kepler-16b as a test bed case. We are aiming to study the detectability of non-transiting and inclined circumbinary planets using the ETV effect along with the fast indicator MEGNO to quantitatively map the chaotic/quasi-periodic regions of the orbital parameter-space and to determine where the orbit of a circumbinary planet will be stable. We have calculated the amplitudes of TTV and ETV signals for different values of the mass and orbital elements of the planet and binary.
On the Habitability of Terrestrial Planets in Binary Star Systems
Authors: Pilat-Lohinger Elke , Funk Barbara , Eggl Siegfried 
Published: April 2014

AbstractThe growing number of detected planets in binary star systems requires methods for a quick assessment of possible habitability of planets in such environments. We offer an analytic method to determine habitability of a terrestrial planet in binary star systems. In this context we give an answer to the most important question: Do the radiative and gravitational perturbations of a secondary influence the extent of the habitable zone (HZ)?After we have defined the borders of the HZ, we will show the dynamical behaviour of a terrestrial planet in the HZ when adding a Jupiter to the system. In such a system the HZ shows signs of mean motion resonances and secular resonances, depending on the architecture of the planetary system.
The Cumulative Effect of Stellar Encounters on Multi-Planet Systems in Star Clusters
Authors: Hao Wei , Kouwenhoven M. B. N. 
Published: April 2014

AbstractDistant stellar encouters can substantially affect the dynamical evolution of existing stellar and planetary systems (e.g., Malmberg et al. 2007; Spurzem et al. 2009). Although planets with small orbital periods are not directly affected by encountering stars, the secular evolution of a perturbed system may result in the ejection of the innermost planets, or physical collisions between the innermost planets and the host star, hundreds of thousands of years after a weak encounter with a neighboring star occurs. Here we present the results of our study on the cumulative effect of distant stellar encounters on multi-planet systems in star clusters, and how these results depend on the properties of the star cluster in which a planetary system is born (for details we refer to Hao & Kouwenhoven, in prep.). With our simulations we explain the scarcity of exoplanets in star clusters, not only for those in wide orbits (affected by stellar encounters), but also in close orbits (affected by the secular evolution of the system following an encounter).
The CARMENES Survey: A Search for Terrestrial Planets in the Habitable Zones of M Dwarfs
Authors: Quirrenbach A. , Amado P. J. , Caballero J. A. , Mandel H. , Mundt R. , Reiners A. , Ribas I. , Carrasco M. A. Sánchez , Seifert W. , Azzaro M. , Galadí D. ,   the CARMENES Consortium
Published: April 2014

AbstractCARMENES (Calar Alto high-Resolution search for M dwarfs with Exo-earths with Near-infrared and optical Echelle Spectrographs) is a next-generation instrument under construction for the 3.5 m telescope at the Calar Alto Observatory by a consortium of eleven Spanish and German institutions. The scientific goal of the project is a five-year exoplanet survey targeting 300 M stars with the completed instrument. The CARMENES hardware consists of two separate échelle spectrographs covering the wavelength range from 0.55 to 1.7 μm at a spectral resolution of R = 82,000, fed by fibers from the Cassegrain focus of the telescope. Both spectrographs are housed in a temperature-stabilized environment in vacuum tanks, to enable a long-term radial velocity precision of 1 m s−1 employing a simultaneous calibration with Th-Ne and U-Ne emission line lamps.
Habitable Worlds Around M Dwarf Stars: The CAPSCam Astrometric Planet Search
Authors: Boss Alan P. , Weinberger Alycia J. , Anglada-Escudé Guillem , Thompson Ian B. , Brahm Rafael 
Published: April 2014

AbstractM dwarf stars are attractive targets in the search for habitable worlds as a result of their relative abundance and proximity, making them likely targets for future direct detection efforts. Hot super-Earths as well as gas giants have already been detected around a number of early M dwarfs, and the former appear to be the high-mass end of the population of rocky, terrestrial exoplanets. The Carnegie Astrometric Planet Search (CAPS) program has been underway since March 2007, searching ~ 100 nearby late M, L, and T dwarfs for gas giant planets on orbits wide enough for habitable worlds to orbit interior to them. The CAPSCam-N camera on the 2.5-m du Pont telescope at the Las Campanas Observatory has demonstrated the ability to detect planets as low in mass as Saturn orbiting at several AU around late M dwarfs within 15 pc. Over the next decade, the CAPS program will provide new constraints on the planetary census around late M dwarf stars, and hence on the suitability of these nearby planetary systems for supporting life.
An Astrobiological Experiment to Explore the Habitability of Tidally Locked M-Dwarf Planets
Authors: Angerhausen Daniel , Sapers Haley , Simoncini Eugenio , Lutz Stefanie , Alexandre Marcelo da Rosa , Galante Douglas 
Published: April 2014

AbstractWe present a summary of a three-year academic research proposal drafted during the Sao Paulo Advanced School of Astrobiology (SPASA) to prepare for upcoming observations of tidally locked planets orbiting M-dwarf stars. The primary experimental goal of the suggested research is to expose extremophiles from analogue environments to a modified space simulation chamber reproducing the environmental parameters of a tidally locked planet in the habitable zone of a late-type star. Here we focus on a description of the astronomical analysis used to define the parameters for this climate simulation.
Search for Low-Mass Planets Around Late-M Dwarfs Using IRD
Authors: Omiya Masashi , Sato Bun'ei , Harakawa Hiroki , Kuzuhara Masayuki , Hirano Teruyuki , Narita Norio ,   IRD team
Published: April 2014

AbstractWe have a plan to conduct a Doppler planet search for low-mass planets around nearby middle-to-late M dwarfs using IRD. IRD is the near-infrared high-precision radial velocity instrument for the Subaru 8.2-m telescope. We expect to achieve the accuracy of the radial velocity measurements of 1 m/s using IRD with a frequency comb as a wavelengh calibrator. Thus, we would detect super-Earths in habitable zone and low-mass rocky planets in close-in orbits around late-M dwarfs. In this survey, we aim to understand and discuss statistical properties of low-mass planets around low-mass M dwarfs compared with those derived from theoretical simulations.
Migration & Extra-solar Terrestrial Planets: Watering the Planets
Authors: Carter-Bond Jade C. , O'Brien David P. , Raymond Sean N. 
Published: April 2014

AbstractA diverse range of terrestrial planet compositions is believed to exist within known extrasolar planetary systems, ranging from those that are relatively Earth-like to those that are highly unusual, dominated by species such as refractory elements (Al and Ca) or C (as pure C, TiC and SiC)(Bond et al. 2010b). However, all prior simulations have ignored the impact that giant planet migration during planetary accretion may have on the final terrestrial planetary composition. Here, we combined chemical equilibrium models of the disk around five known planetary host stars (Solar, HD4203, HD19994, HD213240 and Gl777) with dynamical models of terrestrial planet formation incorporating various degrees of giant planet migration. Giant planet migration is found to drastically impact terrestrial planet composition by 1) increasing the amount of Mg-silicate species present in the final body; and 2) dramatically increasing the efficiency and amount of water delivered to the terrestrial bodies during their formation process.
Water in Protoplanetary Disks
Authors: Nomura H. , Walsh C. , Heinzeller D. , Millar T. J. 
Published: April 2014

AbstractInfrared water line emission from protoplanetary disks, recently observed by the Spitzer and Herschel space telescopes, is thought to trace the surface layer of the inner to outer regions of the disks. We have modelled the water abundance profile and line emission, especially focusing on the effects of dust size growth and turbulent mixing. Comparison between model calculations and observations suggests a small grain model with turbulent mixing is preferred.
Formation of Habitable Planets in Inclined Planetary Systems
Authors: Ji Jianghui , Jin Sheng 
Published: April 2014

AbstractWe extensively investigate the terrestrial planetary formation for the inclined planetary systems (considering the OGLE-2006-BLG-109L system as example) in the late stage. In the simulations, we show that the occurrence of terrestrial planets appears to be common in the final assembly stage. Moreover, we find that a lot of runs finally occupy at least one planet in the habitable zone (HZ). On the other hand, the numerical results also indicate that the inner region of the planetesimal disk, ranging from ~ 0.1 to 0.3 AU, plays an important role in building up terrestrial planets. The outcomes suggest that it may exist moderate possibility for the inclined systems to harbor terrestrial planets in the HZ.