Cost effectiveness of a combination of instruments for global warming: a quantitative approach for Spain

4 p.

Effects of international trade of food and feed and human diet shifts on food security and environmental safety: integrating scales

4 p.

Multistaged acceleration of ions by circularly polarized laser pulse: Monoenergetic ion beam generation

A multiple-staged ion acceleration mechanism in the interaction of a circularly polarized laser pulse with a solid target is studied by one-dimensional particle-in-cell simulation. The ions are accelerated from rest to several MeV monoenergetically at the front surface of the target. After all the plasma ions are accelerated, the acceleration process is repeated on the resulting monoenergetic ions. Under suitable conditions multiple repetitions can be realized and a high-energy quasi-monoenergetic ion beam can be obtained.

Lehiaketa motor baten direkzio piparen diseinua

[EU]Hurrengo orrialdeetan aurkezten den proiektu honetan, lehiaketa motor baten direkzio piparen diseinua proposatzen da zeinak Moto Engineering Foundation fundazioak sustatutako nazioarteko Motostudent txapelketan parte hartzeko motorrera egokituta egon beharko den. Honako helburu honekin beraz, direkzio piparen diseinu egoki bat egin ahal izateko piezak sufrituko dituen karga egoerak aurreikusi beharko ditugu hauen arabera jasan beharreko tentsio egoerak aztertu ahal izateko. Piezaren tentsioen analisia aurrera eraman beharko da beraz, diseinaturiko piezaren funtzionamendu egokia ziurtatu ahal izateko. Historian zehar existitutako diseinu modelo ezberdinak eta baita gaur egunean gehien erabilitakoak ere aurkeztu eta gero, gure kasura hobekien moldatuko zaion adibidetik ekingo zaio diseinuari, aldez aurretik eskuratutako datu eta errodamenduetatik abiatuz. Horrenbestez, oinarritzat hartutako direkzio sistema modeloa eta bestelako elementuen neurriak datutzat hartuta, tija zein norabide ardatzarena esate baterako, direkzio piparen hasierako geometria definituko da. Eskuragarri ditugun analisi metodo ezberdinak aztertu eta gure kasura hobekien moldatzen dena aukeratu eta eraikitako piezari aplikatuko zaio. Lorturiko emaitzen arabera hasiera batean planteaturiko diseinua onartu edo baztertzea erabaki beharko dugu. Beraz, gure diseinua optimizatuz joateko aukera izango dugu, baldintzak eta betebeharrak egiztatuko dituen amaierako pieza diseinua lortu arte. Bukatzeko, proiektuari itxiera emango dion atala aurkeztuko da, hala nola, proiektuaren garapenean zehar lorturiko emaitzak eta ondorioak biltzen dituen atala non lorturiko direkzio piparen funtzionamendu egokia bermatzen dituzten parametroak aurkeztuko diren. Gainera, direkzio sistemaren funtsezko atala izango diren errodamenduen kalkulu eta aukeraketa bideratuko da baita ere.

Análisis de la influencia de la orientación de las fibras metálicas en la resistencia de la matriz de hormigón de acuerdo al Ensayo Barcelona

[ES]El objetivo de este trabajo de fin de grado es analizar la influencia que tiene la cuantía y orientación de fibras metálicas presentes en el interior de probetas de hormigón autocompactante y cuyo objetivo es reforzar y aumentar la resistencia a tracción de este material. Se expondrán las propiedades que combina el HACRFA gracias a la autocompactación del hormigón y la inclusión de fibras en su interior y los beneficios que este nuevo material aporta. Por otro lado, se tratara de situar este estudio en un contexto, analizando a la vez cuál es el alcance y los objetivos más importantes que se han tenido en cuenta. A continuación, y a modo de complementación de su contexto, este trabajo tiene un estado del arte, en el que se mencionarán métodos y ensayos necesarios para llegar a un resultado que permita predecir cuál será la resistencia del material, y por tanto su tenacidad o capacidad de absorber energía, sin necesidad de emplear más que un método fácil y rápido, obviando el resto de ensayos destructivos utilizados en este trabajo. Para tal fin, se establece una metodología que, gracias a ensayos de laboratorio, permita establecer una relación entre el método sencillo que se ha mencionado, el método inductivo, y un resultado teórico de la tenacidad que presenta el HACRFA. Se observará cómo la desviación entre los ensayos experimentales y los resultados teóricos obtenidos es prácticamente nula, despreciando situaciones en las que se presenten comportamientos muy diferentes debido a fallos durante los ensayos.

Análisis y mejora de la gestión y organización del equipo Formula Student Bizkaia usando como referencia el modelo EFQM

[ES]El presente trabajo de fin de grado tiene como objetivo analizar y mejorar la gestión y organización del equipo Formula Student Bizkaia, de tal manera que le permita ser más competitivo frente al resto de universidades. Para su realización, en primer lugar, se exponen las distintas alternativas que existen para evaluar la calidad de gestión del equipo. En segundo lugar, una vez se haya escogido el modelo más conveniente, se prosigue al estudio de los distintos criterios clave en los que se basa. En tercer lugar, cuando se haya llevado a cabo el estudio de los puntos fuertes, así como evidencias y áreas a mejorar, se procede a realizar una evaluación que permita determinar las fortalezas y debilidades, para de esta manera potenciarlas y solventarlas, respectivamente. Por último, se presenta un desglose de los gastos que conlleva realizar la elaboración de un estudio de estas características, así como un desglose de las diferentes tareas a llevar a cabo y su respectiva duración.

[R_Lumbreras_Piqueras] Seguimiento topográfico y levantamiento fotogramétrico de la excavación arqueológica de la Venta de Piqueras, campaña de 2005. Lumbreras (La Rioja)

[ES] Se trata de los restos de un puente del que persisten los pilares a ambos lados del río Piqueras en su origen, realizados en piedra y con restos del empedrado que formaba el suelo.

Did galaxies reionize the universe?

The epoch of reionization remains one of the last uncharted eras of cosmic history, yet this time is of crucial importance, encompassing the formation of both the first galaxies and the first metals in the universe. In this thesis, I present four related projects that both characterize the abundance and properties of these first galaxies and uses follow-up observations of these galaxies to achieve one of the first observations of the neutral fraction of the intergalactic medium during the heart of the reionization era.

First, we present the results of a spectroscopic survey using the Keck telescopes targeting 6.3 < z < 8.8 star-forming galaxies. We secured observations of 19 candidates, initially selected by applying the Lyman break technique to infrared imaging data from the Wide Field Camera 3 (WFC3) onboard the Hubble Space Telescope (HST). This survey builds upon earlier work from Stark et al. (2010, 2011), which showed that star-forming galaxies at 3 < z < 6, when the universe was highly ionized, displayed a significant increase in strong Lyman alpha emission with redshift. Our work uses the LRIS and NIRSPEC instruments to search for Lyman alpha emission in candidates at a greater redshift in the observed near-infrared, in order to discern if this evolution continues, or is quenched by an increase in the neutral fraction of the intergalactic medium. Our spectroscopic observations typically reach a 5-sigma limiting sensitivity of < 50 AA. Despite expecting to detect Lyman alpha at 5-sigma in 7-8 galaxies based on our Monte Carlo simulations, we only achieve secure detections in two of 19 sources. Combining these results with a similar sample of 7 galaxies from Fontana et al. (2010), we determine that these few detections would only occur in < 1% of simulations if the intrinsic distribution was the same as that at z ~ 6. We consider other explanations for this decline, but find the most convincing explanation to be an increase in the neutral fraction of the intergalactic medium. Using theoretical models, we infer a neutral fraction of X_HI ~ 0.44 at z = 7.

Second, we characterize the abundance of star-forming galaxies at z > 6.5 again using WFC3 onboard the HST. This project conducted a detailed search for candidates both in the Hubble Ultra Deep Field as well as a number of additional wider Hubble Space Telescope surveys to construct luminosity functions at both z ~ 7 and 8, reaching 0.65 and 0.25 mag fainter than any previous surveys, respectively. With this increased depth, we achieve some of the most robust constraints on the Schechter function faint end slopes at these redshifts, finding very steep values of alpha_{z~7} = -1.87 +/- 0.18 and alpha_{z~8} = -1.94 +/- 0.23. We discuss these results in the context of cosmic reionization, and show that given reasonable assumptions about the ionizing spectra and escape fraction of ionizing photons, only half the photons needed to maintain reionization are provided by currently observable galaxies at z ~ 7-8. We show that an extension of the luminosity function down to M_{UV} = -13.0, coupled with a low level of star-formation out to higher redshift, can fit all available constraints on the ionization history of the universe.

Third, we investigate the strength of nebular emission in 3 < z < 5 star-forming galaxies. We begin by using the Infrared Array Camera (IRAC) onboard the Spitzer Space Telescope to investigate the strength of H alpha emission in a sample of 3.8 < z < 5.0 spectroscopically confirmed galaxies. We then conduct near-infrared observations of star-forming galaxies at 3 < z < 3.8 to investigate the strength of the [OIII] 4959/5007 and H beta emission lines from the ground using MOSFIRE. In both cases, we uncover near-ubiquitous strong nebular emission, and find excellent agreement between the fluxes derived using the separate methods. For a subset of 9 objects in our MOSFIRE sample that have secure Spitzer IRAC detections, we compare the emission line flux derived from the excess in the K_s band photometry to that derived from direct spectroscopy and find 7 to agree within a factor of 1.6, with only one catastrophic outlier. Finally, for a different subset for which we also have DEIMOS rest-UV spectroscopy, we compare the relative velocities of Lyman alpha and the rest-optical nebular lines which should trace the cites of star-formation. We find a median velocity offset of only v_{Ly alpha} = 149 km/s, significantly less than the 400 km/s observed for star-forming galaxies with weaker Lyman alpha emission at z = 2-3 (Steidel et al. 2010), and show that this decrease can be explained by a decrease in the neutral hydrogen column density covering the galaxy. We discuss how this will imply a lower neutral fraction for a given observed extinction of Lyman alpha when its visibility is used to probe the ionization state of the intergalactic medium.

Finally, we utilize the recent CANDELS wide-field, infra-red photometry over the GOODS-N and S fields to re-analyze the use of Lyman alpha emission to evaluate the neutrality of the intergalactic medium. With this new data, we derive accurate ultraviolet spectral slopes for a sample of 468 3 < z < 6 star-forming galaxies, already observed in the rest-UV with the Keck spectroscopic survey (Stark et al. 2010). We use a Bayesian fitting method which accurately accounts for contamination and obscuration by skylines to derive a relationship between the UV-slope of a galaxy and its intrinsic Lyman alpha equivalent width probability distribution. We then apply this data to spectroscopic surveys during the reionization era, including our own, to accurately interpret the drop in observed Lyman alpha emission. From our most recent such MOSFIRE survey, we also present evidence for the most distant galaxy confirmed through emission line spectroscopy at z = 7.62, as well as a first detection of the CIII]1907/1909 doublet at z > 7.

We conclude the thesis by exploring future prospects and summarizing the results of Robertson et al. (2013). This work synthesizes many of the measurements in this thesis, along with external constraints, to create a model of reionization that fits nearly all available constraints.

A quantitative investigation of the solar modulation of cosmic-ray protons and helium nuclei

The differential energy spectra of cosmic-ray protons and He nuclei have been measured at energies up to 315 MeV/nucleon using balloon- and satellite-borne instruments. These spectra are presented for solar quiet times for the years 1966 through 1970. The data analysis is verified by extensive accelerator calibrations of the detector systems and by calculations and measurements of the production of secondary protons in the atmosphere.

The spectra of protons and He nuclei in this energy range are dominated by the solar modulation of the local interstellar spectra. The transport equation governing this process includes as parameters the solar-wind velocity, V, and a diffusion coefficient, K(r,R), which is assumed to be a scalar function of heliocentric radius, r, and magnetic rigidity, R. The interstellar spectra, j_D, enter as boundary conditions on the solutions to the transport equation. Solutions to the transport equation have been calculated for a broad range of assumed values for K(r,R) and j_D and have been compared with the measured spectra.

It is found that the solutions may be characterized in terms of a dimensionless parameter, ψ(r,R) = ^∞∫_r V dr'/(K(r',R). The amount of modulation is roughly proportional to ψ. At high energies or far from the Sun, where the modulation is weak, the solution is determined primarily by the value of ψ (and the interstellar spectrum) and is not sensitive to the radial dependence of the diffusion coefficient. At low energies and for small r, where the effects of adiabatic deceleration are found to be large, the spectra are largely determined by the radial dependence of the diffusion coefficient and are not very sensitive to the magnitude of ψ or to the interstellar spectra. This lack of sensitivity to j_D implies that the shape of the spectra at Earth cannot be used to determine the interstellar intensities at low energies.

Values of ψ determined from electron data were used to calculate the spectra of protons and He nuclei near Earth. Interstellar spectra of the form j_D α (W - 0.25m)^-2.65 for both protons and He nuclei were found to yield the best fits to the measured spectra for these values of ψ, where W is the total energy and m is the rest energy. A simple model for the diffusion coefficient was used in which the radial and rigidity dependence are separable and K is independent of radius inside a modulation region which has a boundary at a distance D. Good agreement was found between the measured and calculated spectra for the years 1965 through 1968, using typical boundary distances of 2.7 and 6.1 A.U. The proton spectra observed in 1969 and 1970 were flatter than in previous years. This flattening could be explained in part by an increase in D, but also seemed to require that a noticeable fraction of the observed protons at energies as high at 50 to 100 MeV be attributed to quiet-time solar emission. The turnup in the spectra at low energies observed in all years was also attributed to solar emission. The diffusion coefficient used to fit the 1965 spectra is in reasonable agreement with that determined from the power spectra of the interplanetary magnetic field (Jokipii and Coleman, 1968). We find a factor of roughly 3 increase in ψ from 1965 to 1970, corresponding to the roughly order of magnitude decrease in the proton intensity at 250 MeV. The change in ψ might be attributed to a decrease in the diffusion coefficient, or, if the diffusion coefficient is essentially unchanged over that period (Mathews et al., 1971), might be attributed to an increase in the boundary distance, D.

Adaptações transgeracionais do pâncreas endócrino em camundongos provenientes de restrição proteica materna In Utero

A exposição materna durante o período gestacional a uma dieta restrita em proteínas (LP) prejudica o desenvolvimento do pâncreas endócrino em sua prole e aumenta a susceptibilidade à hipertensão, diabetes e obesidade na vida adulta. Há evidências de que esse fenômeno pode persistir em gerações subsequentes. Objetivou-se avaliar o efeito da restrição proteica sobre o metabolismo da glicose e morfometria pancreática na prole F3 de camundongos ao nascimento e ao desmame. Para tanto, fêmeas virgens de camundongos Suíços (F0) foram acasaladas e receberam dieta normo-proteica (19% de proteína - NP) ou uma dieta isocalórica restrita em proteínas (5% de proteína - LP) durante toda a gravidez. Durante a lactação e o restante do experimento, todos os grupos receberam a dieta NP. Os filhotes machos foram nomeados F1 (NP1 e LP1). As fêmeas F1 e F2 foram acasaladas para produzir F2 e F3 (NP2, LP2, NP3 e LP3), respectivamente. Semanalmente, os filhotes foram pesados e calculada a taxa de crescimento alométrico (log [massa corporal] = log a + log b [idade]). Os animais foram sacrificados nos dias 1 e 21 de idade, a glicemia foi determinada e o pâncreas retirado, pesado e analisado por estereologia e imunofluorescência; a insulina foi mensurada aos 21 dias. Como resultados, os filhotes restritos na primeira geração (LP1) foram menores ao nascer, mas apresentaram um crescimento acelerado nos primeiros sete dias de vida, mostrando catch-up com os controles; a prole LP2 demonstrou a maior massa corporal ao nascimento e tiveram uma taxa de crescimento mais lenta durante a lactação; não houve diferença na massa corporal e na taxa de crescimento na geração F3. A massa de pâncreas foi diminuída em LP1-LP3 ao nascimento, contudo foi aumentada em LP2 ao desmame. A densidade de volume e o diâmetro das ilhotas foram menores em todos os grupos restritos no dia 1 e 21, somente LP1 teve o menor número de ilhotas. Ao nascer, a massa de células beta foi menor em LP1-LP3 e permaneceu baixa durante a lactação. No dia 1 e 21, os filhotes foram normoglicêmicos, entretanto foram hipoinsulinêmicos ao desmame. Portanto, a restrição de proteínas em camundongos durante a gestação produz alterações morfológicas nas ilhotas pancreáticas, sugerindo que a homeostase da glicose foi mantida por um aumento da sensibilidade à insulina durante os primeiros estágios de vida na prole ao longo de três gerações consecutivas.

Multipole moments in general relativity and dynamical perturbations of black-hole magnetospheres

This thesis consists of two parts. In Part I, we develop a multipole moment formalism in general relativity and use it to analyze the motion and precession of compact bodies. More specifically, the generic, vacuum, dynamical gravitational field of the exterior universe in the vicinity of a freely moving body is expanded in positive powers of the distance r away from the body's spatial origin (i.e., in the distance r from its timelike-geodesic world line). The expansion coefficients, called "external multipole moments,'' are defined covariantly in terms of the Riemann curvature tensor and its spatial derivatives evaluated on the body's central world line. In a carefully chosen class of de Donder coordinates, the expansion of the external field involves only integral powers of r ; no logarithmic terms occur. The expansion is used to derive higher-order corrections to previously known laws of motion and precession for black holes and other bodies. The resulting laws of motion and precession are expressed in terms of couplings of the time derivatives of the body's quadrupole and octopole moments to the external moments, i.e., to the external curvature and its gradient.

In part II, we study the interaction of magnetohydrodynamic (MHD) waves in a black-hole magnetosphere with the "dragging of inertial frames" effect of the hole's rotation - i.e., with the hole's "gravitomagnetic field." More specifically: we first rewrite the laws of perfect general relativistic magnetohydrodynamics (GRMHD) in 3+1 language in a general spacetime, in terms of quantities (magnetic field, flow velocity, ...) that would be measured by the ''fiducial observers” whose world lines are orthogonal to (arbitrarily chosen) hypersurfaces of constant time. We then specialize to a stationary spacetime and MHD flow with one arbitrary spatial symmetry (e.g., the stationary magnetosphere of a Kerr black hole); and for this spacetime we reduce the GRMHD equations to a set of algebraic equations. The general features of the resulting stationary, symmetric GRMHD magnetospheric solutions are discussed, including the Blandford-Znajek effect in which the gravitomagnetic field interacts with the magnetosphere to produce an outflowing jet. Then in a specific model spacetime with two spatial symmetries, which captures the key features of the Kerr geometry, we derive the GRMHD equations which govern weak, linealized perturbations of a stationary magnetosphere with outflowing jet. These perturbation equations are then Fourier analyzed in time t and in the symmetry coordinate x, and subsequently solved numerically. The numerical solutions describe the interaction of MHD waves with the gravitomagnetic field. It is found that, among other features, when an oscillatory external force is applied to the region of the magnetosphere where plasma (e⁺e^-) is being created, the magnetosphere responds especially strongly at a particular, resonant, driving frequency. The resonant frequency is that for which the perturbations appear to be stationary (time independent) in the common rest frame of the freshly created plasma and the rotating magnetic field lines. The magnetosphere of a rotating black hole, when buffeted by nonaxisymmetric magnetic fields anchored in a surrounding accretion disk, might exhibit an analogous resonance. If so then the hole's outflowing jet might be modulated at resonant frequencies ω=(m/2) Ω_H where m is an integer and Ω_H is the hole's angular velocity.

Key to the larvae of the genera of the sub-family Orthocladiinae from Larvae and Pupae of midges of the sub-family Orthocladiinae of the fauna of the USSR. [Translation from: Larvae and pupae of midges of the subfamily Orthocladiinae of the fauna of the USSR (Diptera, Chironomidae = Tendipedidae) (ed. Pankratova V.Ya.), 51-55. Leningrad, Nauka, 1970. ]

A key to the larvae of the genera of the sub-family Orthocladiinae from Larvae and Pupae of midges of the sub-family Orthocladiinae. Parts of the key refer to the rest of the publication which is not included in this partial translation.

Infraestructuras verdes : análisis de la práctica de los anillos verdes

En los últimos años, alcanzar la Economía Verde parece ser la aspiración perseguida por la sociedad, dado que representa un paso decisivo para lograr el Desarrollo Sostenible y con ello una ciudad sostenible. Sin embargo, las ciudades de todo el mundo han experimentado cambios en su fisonomía debido a los continuos procesos de urbanización que han fomentado un crecimiento desmedido de las mismas, además de generar una serie de efectos negativos que las alejan del camino hacia la sostenibilidad. De tal manera, que a medida que dicho crecimiento aumenta, cada vez son menores las áreas verdes localizadas en las periferias de las ciudades. Para responder a estos problemas asociados al crecimiento urbano y, por ende, al consumo de tierra, se han diseñado diversos instrumentos entre los que destaca la práctica de los Anillos Verdes, siendo el estudio de dicha práctica el objetivo de este trabajo. Con el fin de tener una amplia visión de la implementación de la práctica de los Anillos Verdes, en primer lugar, se describen de manera general algunos casos a nivel internacional, para, a continuación, profundizar en algunas de las principales prácticas europeas y españolas, confirmando, de este modo, que representan una práctica muy extendida en Europa, mientras que en España todavía se encuentran en un estado emergente.

Comparative investigations on the respiratory physiology of euryhaline gammarids with special reference to salinity adaptation. [Translation from: Helgolaender Wissenschaftliche Meeresuntersuchungen 23(4) 485-534, 1972.]

Members of the family Gammaridae are very closely interrelated. There arises the question as to how far they also differ amongst themselves through physiological characteristics. Comparative respiratory and physiological experiments were made on the five euryhaline species Gammarus locusta, G. oceanicus, G. salinus, G. zaddachi and G. duebeni. The respiratory measurements carried out within the framework of this experiment were occupied with the relationships between oxygen consumption and body size depending on salinity. They also had the object of determing the variations in metabolic intensity after an abrupt change in the salt content of the external medium, and to establish the period of time for the process of adaptation. As the experiments were carried out polarographically in a testing plant with continuous flow-through, and the method which was applied permitted continuous recording over prolonged intervals, there could also be carried out comparisons between metabolism at rest and under activity, and the alterations of oxygen consumption during the process of moulting could be measured.

Toward Understanding Astrophysical Phenomena

Fast radio bursts (FRBs), a novel type of radio pulse, whose physics is not yet understood at all. Only a handful of FRBs had been detected when we started this project. Taking account of the scant observations, we put physical constraints on FRBs. We excluded proposals of a galactic origin for their extraordinarily high dispersion measures (DM), in particular stellar coronas and HII regions. Therefore our work supports an extragalactic origin for FRBs. We show that the resolved scattering tail of FRB 110220 is unlikely to be due to propagation through the intergalactic plasma. Instead the scattering is probably caused by the interstellar medium in the FRB's host galaxy, and indicates that this burst sits in the central region of that galaxy. Pulse durations of order $\ms$ constrain source sizes of FRBs implying enormous brightness temperatures and thus coherent emission. Electric fields near FRBs at cosmological distances would be so strong that they could accelerate free electrons from rest to relativistic energies in a single wave period. When we worked on FRBs, it was unclear whether they were genuine astronomical signals as distinct from `perytons', clearly terrestrial radio bursts, sharing some common properties with FRBs. Recently, in April 2015, astronomers discovered that perytons were emitted by microwave ovens. Radio chirps similar to FRBs were emitted when their doors opened while they were still heating. Evidence for the astronomical nature of FRBs has strengthened since our paper was published. Some bursts have been found to show linear and circular polarizations and Faraday rotation of the linear polarization has also been detected. I hope to resume working on FRBs in the near future. But after we completed our FRB paper, I decided to pause this project because of the lack of observational constraints.

The pulsar triple system, J0733+1715, has its orbital parameters fitted to high accuracy owing to the precise timing of the central $\ms$ pulsar. The two orbits are highly hierarchical, namely $P_{\mathrm{orb,1}}\ll P_{\mathrm{orb,2}}$, where 1 and 2 label the inner and outer white dwarf (WD) companions respectively. Moreover, their orbital planes almost coincide, providing a unique opportunity to study secular interaction associated purely with eccentricity beyond the solar system. Secular interaction only involves effect averaged over many orbits. Thus each companion can be represented by an elliptical wire with its mass distributed inversely proportional to its local orbital speed. Generally there exists a mutual torque, which vanishes only when their apsidal lines are parallel or anti-parallel. To maintain either mode, the eccentricity ratio, $e_1/e_2$, must be of the proper value, so that both apsidal lines precess together. For J0733+1715, $e_1\ll e_2$ for the parallel mode, while $e_1\gg e_2$ for the anti-parallel one. We show that the former precesses $\sim 10$ times slower than the latter. Currently the system is dominated by the parallel mode. Although only a little anti-parallel mode survives, both eccentricities especially $e_1$ oscillate on $\sim 10^3\yr$ timescale. Detectable changes would occur within $\sim 1\yr$. We demonstrate that the anti-parallel mode gets damped $\sim 10^4$ times faster than its parallel brother by any dissipative process diminishing $e_1$. If it is the tidal damping in the inner WD, we proceed to estimate its tidal quantity parameter ($Q$) to be $\sim 10^6$, which was poorly constrained by observations. However, tidal damping may also happen during the preceding low-mass X-ray binary (LMXB) phase or hydrogen thermal nuclear flashes. But, in both cases, the inner companion fills its Roche lobe and probably suffers mass/angular momentum loss, which might cause $e_1$ to grow rather than decay.

Several pairs of solar system satellites occupy mean motion resonances (MMRs). We divide these into two groups according to their proximity to exact resonance. Proximity is measured by the existence of a separatrix in phase space. MMRs between Io-Europa, Europa-Ganymede and Enceladus-Dione are too distant from exact resonance for a separatrix to appear. A separatrix is present only in the phase spaces of the Mimas-Tethys and Titan-Hyperion MMRs and their resonant arguments are the only ones to exhibit substantial librations. When a separatrix is present, tidal damping of eccentricity or inclination excites overstable librations that can lead to passage through resonance on the damping timescale. However, after investigation, we conclude that the librations in the Mimas-Tethys and Titan-Hyperion MMRs are fossils and do not result from overstability.

Rubble piles are common in the solar system. Monolithic elements touch their neighbors in small localized areas. Voids occupy a significant fraction of the volume. In a fluid-free environment, heat cannot conduct through voids; only radiation can transfer energy across them. We model the effective thermal conductivity of a rubble pile and show that it is proportional the square root of the pressure, $P$, for $P\leq \epsy^3\mu$ where $\epsy$ is the material's yield strain and $\mu$ its shear modulus. Our model provides an excellent fit to the depth dependence of the thermal conductivity in the top $140\,\mathrm{cm}$ of the lunar regolith. It also offers an explanation for the low thermal inertias of rocky asteroids and icy satellites. Lastly, we discuss how rubble piles slow down the cooling of small bodies such as asteroids.

Electromagnetic (EM) follow-up observations of gravitational wave (GW) events will help shed light on the nature of the sources, and more can be learned if the EM follow-ups can start as soon as the GW event becomes observable. In this paper, we propose a computationally efficient time-domain algorithm capable of detecting gravitational waves (GWs) from coalescing binaries of compact objects with nearly zero time delay. In case when the signal is strong enough, our algorithm also has the flexibility to trigger EM observation {\it before} the merger. The key to the efficiency of our algorithm arises from the use of chains of so-called Infinite Impulse Response (IIR) filters, which filter time-series data recursively. Computational cost is further reduced by a template interpolation technique that requires filtering to be done only for a much coarser template bank than otherwise required to sufficiently recover optimal signal-to-noise ratio. Towards future detectors with sensitivity extending to lower frequencies, our algorithm's computational cost is shown to increase rather insignificantly compared to the conventional time-domain correlation method. Moreover, at latencies of less than hundreds to thousands of seconds, this method is expected to be computationally more efficient than the straightforward frequency-domain method.