More bang for your buck: Super-adiabatic quantum engines

The practical untenability of the quasi-static assumption makes any realistic engine intrinsically irreversible and its operating time finite, thus implying friction effects at short cycle times. An important technological goal is thus the design of maximally efficient engines working at the maximum possible power. We show that, by utilising shortcuts to adiabaticity in a quantum engine cycle, one can engineer a thermodynamic cycle working at finite power and zero friction. Our findings are illustrated using a harmonic oscillator undergoing a quantum Otto cycle.

Characterization of the Kepler-101 planetary system with HARPS-N. A hot super-Neptune with an Earth-sized low-mass companion

We characterize the planetary system Kepler-101 by performing a combined differential evolution Markov chain Monte Carlo analysisof Kepler data and forty radial velocities obtained with the HARPS-N spectrograph. This system was previously validated and iscomposed of a hot super-Neptune, Kepler-101b, and an Earth-sized planet, Kepler-101c. These two planets orbit the slightly evolvedand metal-rich G-type star in 3.49 and 6.03 days, respectively. With mass Mp = 51.1+5.1−4.7 M⊕, radius Rp = 5.77+0.85−0.79 R⊕, and density ρp = 1.45+0.83 −0.48 g cm−3, Kepler-101b is the first fully characterized super-Neptune, and its density suggests that heavy elements makeup a significant fraction of its interior; more than 60% of its total mass. Kepler-101c has a radius of 1.25+0.19−0.17 R⊕, which implies theabsence of any H/He envelope, but its mass could not be determined because of the relative faintness of the parent star for highly precise radial-velocity measurements (Kp = 13.8) and the limited number of radial velocities. The 1σ upper limit, Mp < 3.8 M⊕, excludes a pure iron composition with a probability of 68.3%. The architecture of the planetary system Kepler-101 − containing aclose-in giant planet and an outer Earth-sized planet with a period ratio slightly larger than the 3:2 resonance − is certainly of interest for scenarios of planet formation and evolution. This system does not follow the previously reported trend that the larger planet has the longer period in the majority of Kepler systems of planet pairs with at least one Neptune-sized or larger planet.

Hydrogel-Forming Microneedles Prepared from ‘‘Super Swelling’’ Polymers Combined with Lyophilised Wafers for Transdermal Drug Delivery

We describe, for the first time, hydrogel-forming microneedle arrays prepared from "super swelling" polymeric compositions. We produced a microneedle formulation with enhanced swelling capabilities from aqueous blends containing 20% w/w Gantrez S-97, 7.5% w/w PEG 10,000 and 3% w/w Na2CO3 and utilised a drug reservoir of a lyophilised wafer-like design. These microneedle-lyophilised wafer compositions were robust and effectively penetrated skin, swelling extensively, but being removed intact. In in vitro delivery experiments across excised neonatal porcine skin, approximately 44 mg of the model high dose small molecule drug ibuprofen sodium was delivered in 24 h, equating to 37% of the loading in the lyophilised reservoir. The super swelling microneedles delivered approximately 1.24 mg of the model protein ovalbumin over 24 h, equivalent to a delivery efficiency of approximately 49%. The integrated microneedle-lyophilised wafer delivery system produced a progressive increase in plasma concentrations of ibuprofen sodium in rats over 6 h, with a maximal concentration of approximately 179 µg/ml achieved in this time. The plasma concentration had fallen to 71±6.7 µg/ml by 24 h. Ovalbumin levels peaked in rat plasma after only 1 hour at 42.36±17.01 ng/ml. Ovalbumin plasma levels then remained almost constant up to 6 h, dropping somewhat at 24 h, when 23.61±4.84 ng/ml was detected. This work represents a significant advancement on conventional microneedle systems, which are presently only suitable for bolus delivery of very potent drugs and vaccines. Once fully developed, such technology may greatly expand the range of drugs that can be delivered transdermally, to the benefit of patients and industry. Accordingly, we are currently progressing towards clinical evaluations with a range of candidate molecules.

Properties of Super-Hydrophobic Copper and Stainless Steel Meshes: Applications in Controllable Water Permeation and Organic Solvents/Water Separation

The wettability and hydrophobicity of super-hydrophobic (SH) meshes is greatly influenced by their topographic structures, chemical composition and coating process. In this study, the properties of copper and stainless steel meshes, coated with super-hydrophobic electrolessly deposited silver were investigated. A new method to test the pressure resistance of super-hydrophobic mesh was applied to avoid any deformation of mesh. Results showed that SH copper mesh and SH stainless steel meshes with the same pore size have almost the same contact angle and the same hydrophobicity. SH copper mesh with a pore size of 122 μm can resist water pressure of 4900 Pa and a decrease of pore size of mesh can increase the pressure resistance of SH copper mesh. The SH copper mesh modified with 0.1 M HS(CH2)10COOH solution in ethanol has a controllable water permeation property by simply adjusting the pH of water solution. SH copper mesh shows super-oleophilicity with organic solvents and so with a water contact angle of 0° and it can be an effective tool for organic solvents/water separation. The separation efficiency of SH copper mesh for separating mixtures of organic solvent and water can be as high as 99.8%.

Characterizing K2 Planet Discoveries: A super-Earth transiting the bright K-dwarf HIP 116454

We report the first planet discovery from the two-wheeled Kepler (K2) mission: HIP 116454 b. The host star HIP 116454 is a bright (V = 10.1, K = 8.0) K1 dwarf with high proper motion and a parallax-based distance of 55.2 +/- 5.4 pc. Based on high-resolution optical spectroscopy, we find that the host star is metal-poor with [Fe/H]= -0.16 +/- 0.08 and has a radius R-star = 0.716 +/- 0.024 R-circle dot and mass M-star = 0.775 +/- 0.027M(circle dot). The star was observed by the Kepler spacecraft during its Two-Wheeled Concept Engineering Test in 2014 February. During the 9 days of observations, K2 observed a single transit event. Using a new K2 photometric analysis technique, we are able to correct small telescope drifts and recover the observed transit at high confidence, corresponding to a planetary radius of R-p = 2.53 +/- 0.18 R-circle plus. Radial velocity observations with the HARPS-N spectrograph reveal a 11.82 +/- 1.33 M-circle plus planet in a 9.1 day orbit, consistent with the transit depth, duration, and ephemeris. Follow-up photometric measurements from the MOST satellite confirm the transit observed in the K2 photometry and provide a refined ephemeris, making HIP 116454 b amenable for future follow-up observations of this latest addition to the growing population of transiting super-Earths around nearby, bright stars.

LSQ14bdq: a type Ic Super-luminous Supernova with a double-peaked light curve

We present data for LSQ14bdq, a hydrogen-poor super-luminous supernova (SLSN) discovered by the La Silla QUEST survey and classified by the Public ESO Spectroscopic Survey of Transient Objects. The spectrum and light curve are very similar to slow-declining SLSNe such as PTF12dam. However, detections within ∼1 day after explosion show a bright and relatively fast initial peak, lasting for ∼15 days, prior to the usual slow rise to maximum light. The broader, main peak can be fit with either central engine or circumstellar interaction models. We discuss the implications of the precursor peak in the context of these models. It is too bright and narrow to be explained as a normal ⁵⁶Ni-powered SN, and we suggest that interaction models may struggle to fit the two peaks simultaneously. We propose that the initial peak may arise from the post-shock cooling of extended stellar material, and reheating by a central engine drives the second peak. In this picture, we show that an explosion energy of ∼2 × 10⁵² erg and a progenitor radius of a few hundred solar radii would be required to power the early emission. The competing engine models involve rapidly spinning magnetars (neutron stars) or fallback onto a central black hole. The prompt energy required may favor the black hole scenario. The bright initial peak may be difficult to reconcile with a compact Wolf-Rayet star as a progenitor since the inferred energies and ejected masses become unphysical.

Super suburbia: developing resilience by closing resource cycles in North Belfast

Sustainability can be described as having three interlinked strands, known as the ‘trias energetica’, without which resilience is difficult to achieve. These strands are environmental, social and economic: and if taken as indicators, the suburbs of North Belfast are very poorly performing indeed. Places such as Ligoneal and Glen Cairn have poor housing stock energetically, and also little economic activity. This paper describes propositional work completed by Queens University and Belfast City Council as part of the UK’s Technology Strategy Board’s Future Cities Programme, which aimed to develop new synergies in these neighbourhoods by the insertion of closed cycle economies.

By utilising a research by design methodology, the paper develops a process-based and phased design to develop a new emergent form to these neighbourhoods, one in which new productive systems are embedded into the city, at a small-scales. These include a peak-load hydro-electric project in Ligoneal; a productive landscape in Glen Cairn and a city-wide energy refurbishment utilising neighbourhood waste streams.

These designs allow for a roadmap for development to be created that could change the modus operandi of an area over a relatively short period of time, and show that even modest investments of productive technologies at a local scale could fundamentally change the form and the economic and environmental operation of the city in the future, and create a new resilient city, one that can be less externally dependent and more socially just.

The high-energy environment in the super-Earth system CoRoT-7

High-energy irradiation of exoplanets has been identified to be a key influence on the stability of these planets' atmospheres. So far, irradiation-driven mass-loss has been observed only in two Hot Jupiters, and the observational data remain even more sparse in the super-Earth regime. We present an investigation of the high-energy emission in the CoRoT-7 system, which hosts the first known transiting super-Earth. To characterize the high-energy XUV radiation field into which the rocky planets CoRoT-7b and CoRoT-7c are immersed, we analyzed a 25 ks XMM-Newton observation of the host star. Our analysis yields the first clear (3.5σ) X-ray detection of CoRoT-7. We determine a coronal temperature of ≈ 3 MK and an X-ray luminosity of 3 × 1028 erg s-1. The level of XUV irradiation on CoRoT-7b amounts to ≈37 000 erg cm-2 s-1. Current theories for planetary evaporation can only provide an order-of-magnitude estimate for the planetary mass loss; assuming that CoRoT-7b has formed as a rocky planet, we estimate that CoRoT-7b evaporates at a rate of about 1.3 × 1011 g s-1 and has lost ≈4-10 earth masses in total.

X-Ray Emission from the Super-Earth Host GJ 1214

Stellar activity can produce large amounts of high-energy radiation, which is absorbed by the planetary atmosphere leading to irradiation-driven mass loss. We present the detection and an investigation of high-energy emission in a transiting super-Earth host system, GJ 1214, based on XMM-Newton observations. We derive an X-ray luminosity of LX = 7.4 × 1025 erg s-1 and a corresponding activity level of log (LX /L bol) ~ -5.3. Further, we determine a coronal temperature of about ~3.5 MK, which is typical for coronal emission of moderately active low-mass stars. We estimate that GJ 1214 b evaporates at a rate of 1.3× 1010 g s-1 and has lost a total of ≈2-5.6 M ⊕.

Resposta do Olival Intensivo e Super-Intensivo a Dois Regimes de Rega: Parâmetros Fisiológicos, Produção e Qualidade

O olival de regadio tem tido grande expansão nos últimos anos no Alentejo, sendo a administração da rega mais adequada às necessidades hídricas um dos fatores determinantes da sua boa gestão. No presente trabalho, avaliou-se a resposta de duas variedades de Olea europaea, Cobrançosa e Arbequina, em regime intensivo e super- intensivo, respetivamente, a duas dotações de rega, a normalmente utilizada pelo agricultor (RA) e outra experimental, com dotações acima (RA+) ou abaixo (RA−) das praticados em RA. Mediram-se os principais parâmetros hídricos das plantas e o teor em clorofilas, e registou-se a assinatura espectral em folhas adultas e jovens, ao meio- dia solar, em três épocas do ano, primavera, final do verão e inverno de 2011. Em Outubro foi feita a colheita, tendo-se quantificado a produção em termos de produção total e teor de óleo na matéria seca, e a qualidade do azeite em termos de acidez e oxidação. Face aos resultados, conclui-se que no olival intensivo de Cobrançosa, na rega experimental (RA+), acima da praticada pelo agricultor, não se verificou diferenças significativas na produção total nem no teor de óleo na matéria seca. Não se verificaram também diferenças significativas entre as regas nos parâmetros hídricos avaliados. Quanto ao olival super-intensivo de Arbequina, a rega experimental (RA−), deficitária relativamente à do agricultor (RA), acarretou menor produção, associada a menor teor relativo de água nas folhas, potenciais hídricos mais negativos e menor condutância estomática no final do verão e inverno, mantendo-se no entanto o teor de óleo nos frutos. O teor em clorofilas e alguns índices de vegetação foram influenciados pelo regime de rega apenas em algumas das datas. Nos dois olivais, as regas experimentais não influenciaram a qualidade do azeite, tendo-se obtido azeites extra virgem com propriedades semelhantes aos das modalidades RA. O estudo prossegue em 2012.

Pegada hídrica de um olival super-intensivo sob clima mediterrânico, utilizando medições de campo e deteção remota

A pegada hídrica de uma cultura representa o volume de água necessário para produzir, relacionando as necessidades hídricas da cultura com a produção. As suas componentes, pegadas hídricas azul, verde e cinzenta, referem-se respectivamente aos volumes de água superficial e subterrânea, precipitação e de água necessária para assimilar a poluição utilizados pela cultura. A determinação das pegadas hídricas azul e verde é normalmente conseguida através da estimativa da evapotranspiração cultural, aplicando coeficientes culturais a uma evapotranspiração de referência, calculada a partir de dados meteorológicos. No presente estudo foram utilizadas medições da evapotranspiração para estimar a pegada hídrica de um olival super-intensivo na região de Évora. As necessidades hídricas foram medidas utilizando um método de fluxo de seiva para determinar a transpiração e o método micrometeorológico das flutuações instantâneas para medir directamente a evapotranspiração. Esta técnica foi utilizada durante um período de tempo limitado, enquanto as medições do fluxo de seiva, que foram efectuadas para períodos alargados, permitiram a extensão dos registos. A evapotranspiração medida directamente apresentou valores de cerca de 3 mm d-1 e o quociente entre evapotranspiração real e evapotranspiração de referência é próximo de 0,6 para o mesmo período. Comparou-se a estimativa da pegada hídrica obtida com o procedimento habitual com a resultante de medições in-situ e utilizando técnicas de deteção remota. A pegada hídrica do olival sob estudo foi inferior às simulações encontradas na literatura, o que pode ser explicado por diferenças na densidade de plantação, produção e gestão da rega. O olival em estudo obteve uma produção elevada, com um azeite que preencheu as características essenciais à classificação de azeite extra virgem, o mais valorizado, o que contraria o efeito do elevado consumo de água, resultando numa pegada hídrica inferior à de olivais não regados ou com menor densidade de plantação.