Population synthesis of isolated neutron stars with magneto-rotational evolution

We revisit the population synthesis of isolated radio-pulsars incorporating recent advances on the evolution of the magnetic field and the angle between the magnetic and rotational axes from new simulations of the magneto-thermal evolution and magnetosphere models, respectively. An interesting novelty in our approach is that we do not assume the existence of a death line. We discuss regions in parameter space that are more consistent with the observational data. In particular, we find that any broad distribution of birth spin periods with P0 ≲ 0.5 s can fit the data, and that if the alignment angle is allowed to vary consistently with the torque model, realistic magnetospheric models are favoured compared to models with classical magneto-dipolar radiation losses. Assuming that the initial magnetic field is given by a lognormal distribution, our optimal model has mean strength 〈log B0[G]〉 ≈ 13.0–13.2 with width σ(log B0) = 0.6–0.7. However, there are strong correlations between parameters. This degeneracy in the parameter space can be broken by an independent estimate of the pulsar birth rate or by future studies correlating this information with the population in other observational bands (X-rays and γ-rays).

The many lives of magnetized neutron stars

The magnetic field strength at birth is arguably one of the most important properties to determine the evolutionary path of a neutron star. Objects with very high fields, collectively known as magnetars, are characterized by high X-ray quiescent luminosities, occurrence of outbursts, and, for some of them, sporadic giant flares. While the magnetic field strength is believed to drive their collective behaviour, however, the diversity of their properties, and, especially, the observation of magnetar-like bursts from “low-field” pulsars, has been a theoretical puzzle. In this review, we discuss results of long-term simulations following the coupled evolution of the X-ray luminosity and the timing properties for a large, homogeneous sample of X-ray emitting isolated neutron stars, accounting for a range of initial magnetic field strengths, envelope compositions, and neutron star masses. In addition, by following the evolution of magnetic stresses within the neutron star crust, we can also relate the observed magnetar phenomenology to the physical properties of neutron stars, and in particular to their age and magnetic field strength and topology. The dichotomy of “high-B” field pulsars versus magnetars is naturally explained, and occasional outbursts from old, low B-field neutron stars are predicted. We conclude by speculating on the fate of old magnetars, and by presenting observational diagnostics of the neutron star crustal field topology.

Contribuciones al estudio analítico del movimiento de rotación de una Tierra deformable

Esta memoria para optar al grado de doctor por la Universidad de Alicante, en el área de Matemática Aplicada, se divide en ocho capítulos. En los cuatro primeros se lleva a cabo una revisión del problema de la rotación de la Tierra rígida y elástica, en formalismo hamiltoniano, y se introducen algunas alternativas originales a la construcción de ciertos elementos de la teoría. En los otros cuatro se presentan nuevas contribuciones al estudio analítico de los movimientos de precesión y nutación de la Tierra deformable. Estas se pueden agrupar en dos categorías: la obtención de fórmulas que describen el movimiento de rotación del eje de figura, que completan las existentes hasta la fecha, y la extensión del formalismo para hacerlo compatible con modelos reológicos de la Tierra más generales.

Coordinación para el seguimiento de la titulación Máster en Prevención de Riesgos Laborales

La titulación de postgrado Máster en Prevención de Riesgos Laborales se implantó en la Escuela Politécnica Superior de la Universidad de Alicante en el curso 2011/12. El profesorado con docencia asignada en la titulación participó durante el curso 2012/13 en el proyecto para la coordinación de las asignaturas del Máster en Prevención de Riesgos Laborales. En el marco creado por los nuevos estudios de Postgrado, dentro del EEES, el proyecto tenía como objetivo principal la coordinación de las asignaturas y la mejora de la calidad docente. La implantación de la titulación generó un esfuerzo considerable por parte de los coordinadores y docentes implicados, que adaptaron su planificación y metodología al nuevo marco del EEES. El diseño de las asignaturas del Máster ha incorporado la metodología, el cronograma del temario y la evaluación durante todas las semanas del semestre. En este sentido se tuvieron que solucionar diferentes problemas: compatibilizar horarios de los docentes, evitar solapamientos entre asignaturas y verificar la información completa de cada asignatura. El proyecto de coordinación ha resultado un instrumento útil para la interacción y coordinación entre los profesores/as con participación docente en el Máster.

Discussing the physical meaning of the absorption feature at 2.1 keV in 4U 1538–52

High resolution X-ray spectroscopy is a powerful tool for studying the nature of the matter surrounding the neutron star in X-ray binaries and its interaction between the stellar wind and the compact object. In particular, absorption features in their spectra could reveal the presence of atmospheres of the neutron star or their magnetic field strength. Here we present an investigation of the absorption feature at 2.1 keV in the X-ray spectrum of the high mass X-ray binary 4U 1538–52 based on our previous analysis of the XMM-Newton data. We study various possible origins and discuss the different physical scenarios in order to explain this feature. A likely interpretation is that the feature is associated with atomic transitions in an O/Ne neutron star atmosphere or of hydrogen and helium like Fe or Si ions formed in the stellar wind of the donor.

El proceso enseñanza-aprendizaje de la física para la ingeniería/arquitectura

Cuando finalice el curso 2013-14 se producirá la salida de la primera promoción de graduados en la Escuela Politécnica Superior (EPS). Teniendo en cuenta que antes de que transcurran seis años se debe renovar la acreditación de los títulos oficiales de Grado, consideramos adecuado efectuar un análisis crítico del proceso de enseñanza-aprendizaje. En este trabajo presentamos los resultados del seguimiento realizado en el contexto educativo de los fundamentos físicos en los títulos de grado de la EPS. Estos resultados muestran la necesidad de abordar los cambios necesarios para corregir las deficiencias detectadas y mejorar la calidad del aprendizaje. Conviene recordar que el cambio que se pretendía realizar en la enseñanza universitaria era para centrarse en el aprendizaje del alumnado. Además incluimos un estudio de la evolución del aprendizaje de la física analizando las calificaciones de acceso en física y matemáticas y comparándolas con las obtenidas en los fundamentos físicos de los diferentes grados impartidos en la EPS. También presentaremos buena parte de las actividades realizadas para facilitar el aprendizaje continuo de nuestro alumnado mediante el uso de nuevas herramientas informáticas, como blogs, OpenCourseWare, materiales audiovisuales (pUAs), etc.

Neutron Stars—Thermal Emitters

Confronting theoretical models with observations of thermal radiation emitted by neutron stars is one of the most important ways to understand the properties of both, superdense matter in the interiors of the neutron stars and dense magnetized plasmas in their outer layers. Here we review the theory of thermal emission from the surface layers of strongly magnetized neutron stars, and the main properties of the observational data. In particular, we focus on the nearby sources for which a clear thermal component has been detected, without being contaminated by other emission processes (magnetosphere, accretion, nebulae). We also discuss the applications of the modern theoretical models of the formation of spectra of strongly magnetized neutron stars to the observed thermally emitting objects.

Diseño de materiales y actividades interactivas para el autoaprendizaje de la física

Numerosos estudios han puesto de manifiesto la dificultad del aprendizaje de la física tanto en la educación secundaria y bachillerato como en la educación universitaria. El espacio Europeo de Educación Superior (EEES) pone énfasis en el aprendizaje del alumnado y modifica el rol del profesorado como tutor de su aprendizaje, potenciando la adquisición de los conocimientos mediante metodologías activas. Nosotros nos centraremos en desarrollar competencias transversales y favorecer un aprendizaje interactivo y global. Por ejemplo, se potenciará la búsqueda de información relacionada con un tema, se provocará la reacción o participación del alumnado sobre aspectos de aplicación de los fundamentos físicos en la edificación y en la ingeniería, se comprobará mediante la autoevaluación la adquisición de los objetivos, se favorecerá el aprendizaje atemporal, etc. También proporcionará el trabajo de algunas capacidades como la planificación de las tareas, la comunicación y exposición de ideas sobre aspectos académicos o profesionales, la generación de nuevas ideas o la construcción de conocimiento a partir de sus aportaciones. Finalmente se recogerán los comentarios y sugerencias del alumnado para adaptar los materiales diseñados a sus necesidades.

Probing large-scale wind structures in Vela X–1 using off-states with INTEGRAL

Vela X–1 is the prototype of the class of wind-fed accreting pulsars in high-mass X-ray binaries hosting a supergiant donor. We have analysed in a systematic way 10 years of INTEGRAL data of Vela X–1 (22–50 keV) and we found that when outside the X-ray eclipse, the source undergoes several luminosity drops where the hard X-rays luminosity goes below ∼3 × 1035 erg s−1, becoming undetected by INTEGRAL. These drops in the X-ray flux are usually referred to as ‘off-states’ in the literature. We have investigated the distribution of these off-states along the Vela X–1 ∼ 8.9 d orbit, finding that their orbital occurrence displays an asymmetric distribution, with a higher probability to observe an off-state near the pre-eclipse than during the post-eclipse. This asymmetry can be explained by scattering of hard X-rays in a region of ionized wind, able to reduce the source hard X-ray brightness preferentially near eclipse ingress. We associate this ionized large-scale wind structure with the photoionization wake produced by the interaction of the supergiant wind with the X-ray emission from the neutron star. We emphasize that this observational result could be obtained thanks to the accumulation of a decade of INTEGRAL data, with observations covering the whole orbit several times, allowing us to detect an asymmetric pattern in the orbital distribution of off-states in Vela X–1.

An XMM-Newton view of FeKα in high-mass X-ray binaries

We present a comprehensive analysis of the whole sample of available XMM-Newton observations of high-mass X-ray binaries (HMXBs) until August 2013, focusing on the FeKα emission line. This line is key to better understanding the physical properties of the material surrounding the X-ray source within a few stellar radii (the circumstellar medium). We collected observations from 46 HMXBs and detected FeKα in 21 of them. We used the standard classification of HMXBs to divide the sample into different groups. We find that (1) different classes of HMXBs display different qualitative behaviours in the FeKα spectral region. This is visible especially in SGXBs (showing ubiquitous Fe fluorescence but not recombination Fe lines) and in γ Cass analogues (showing both fluorescent and recombination Fe lines). (2) FeKα is centred at a mean value of 6.42 keV. Considering the instrumental and fits uncertainties, this value is compatible with ionization states that are lower than Fe xviii. (3) The flux of the continuum is well correlated with the flux of the line, as expected. Eclipse observations show that the Fe fluorescence emission comes from an extended region surrounding the X-ray source. (4) We observe an inverse correlation between the X-ray luminosity and the equivalent width of FeKα (EW). This phenomenon is known as the X-ray Baldwin effect. (5) FeKα is narrow (σline< 0.15 keV), reflecting that the reprocessing material does not move at high speeds. We attempt to explain the broadness of the line in terms of three possible broadening phenomena: line blending, Compton scattering, and Doppler shifts (with velocities of the reprocessing material V ~ 1000 km s-1). (6) The equivalent hydrogen column (NH) directly correlates to the EW of FeKα, displaying clear similarities to numerical simulations. It highlights the strong link between the absorbing and the fluorescent matter. (7) The observed NH in supergiant X-ray binaries (SGXBs) is in general higher than in supergiant fast X-ray transients (SFXTs). We suggest two possible explanations: different orbital configurations or a different interaction compact object – wind. (8) Finally, we analysed the sources IGR J16320-4751 and 4U 1700-37 in more detail, covering several orbital phases. The observed variation in NH between phases is compatible with the absorption produced by the wind of their optical companions. The results clearly point to a very important contribution of the donor’s wind in the FeKα emission and the absorption when the donor is a supergiant massive star.

The X-ray outburst of the Galactic Centre magnetar SGR J1745−2900 during the first 1.5 year

In 2013 April a new magnetar, SGR 1745−2900, was discovered as it entered an outburst, at only 2.4 arcsec angular distance from the supermassive black hole at the centre of the Milky Way, Sagittarius A*. SGR 1745−2900 has a surface dipolar magnetic field of ∼2 × 1014 G, and it is the neutron star closest to a black hole ever observed. The new source was detected both in the radio and X-ray bands, with a peak X-ray luminosity LX ∼ 5 × 1035 erg s−1. Here we report on the long-term Chandra (25 observations) and XMM–Newton (eight observations) X-ray monitoring campaign of SGR 1745−2900 from the onset of the outburst in 2013 April until 2014 September. This unprecedented data set allows us to refine the timing properties of the source, as well as to study the outburst spectral evolution as a function of time and rotational phase. Our timing analysis confirms the increase in the spin period derivative by a factor of ∼2 around 2013 June, and reveals that a further increase occurred between 2013 October 30 and 2014 February 21. We find that the period derivative changed from 6.6 × 10−12 to 3.3 × 10−11 s s−1 in 1.5 yr. On the other hand, this magnetar shows a slow flux decay compared to other magnetars and a rather inefficient surface cooling. In particular, starquake-induced crustal cooling models alone have difficulty in explaining the high luminosity of the source for the first ∼200 d of its outburst, and additional heating of the star surface from currents flowing in a twisted magnetic bundle is probably playing an important role in the outburst evolution.

Pulsar science with the SKA

The unprecedented sensitivity and large field of view of SKA will be of paramount importance for pulsar science, and for many related research fields. In particular, beside the obvious discovery of many more pulsars (even those with very low luminosity), and the extremely accurate timing analysis of the current pulsar population, SKA will allow to use pulsars to measure or put strong constraints on gravitational waves, Galactic magnetism, planet masses, general relativity and nuclear physics.

The donor star of the X-ray pulsar X1908+075

High-mass X-ray binaries consist of a massive donor star and a compact object. While several of those systems have been well studied in X-rays, little is known for most of the donor stars as they are often heavily obscured in the optical and ultraviolet regime. There is an opportunity to observe them at infrared wavelengths, however. The goal of this study is to obtain the stellar and wind parameters of the donor star in the X1908+075 high-mass X-ray binary system with a stellar atmosphere model to check whether previous studies from X-ray observations and spectral morphology lead to a sufficient description of the donor star. We obtained H- and K-band spectra of X1908+075 and analysed them with the Potsdam Wolf-Rayet (PoWR) model atmosphere code. For the first time, we calculated a stellar atmosphere model for the donor star, whose main parameters are: Mspec = 15 ± 6 M⊙, T∗ = 23-3+6 kK, log geff = 3.0 ± 0.2 and log L/L⊙ = 4.81 ± 0.25. The obtained parameters point towards an early B-type (B0–B3) star, probably in a supergiant phase. Moreover we determined a more accurate distance to the system of 4.85 ± 0.50 kpc than the previously reported value.

Quiescent thermal emission from neutron stars in low-mass X-ray binaries

Context. We monitored the quiescent thermal emission from neutron stars in low-mass X-ray binaries after active periods of intense activity in X-rays (outbursts). Aims. The theoretical modeling of the thermal relaxation of the neutron star crust may be used to establish constraints on the crust composition and transport properties, depending on the astrophysical scenarios assumed. Methods. We numerically simulated the thermal evolution of the neutron star crust and compared them with inferred surface temperatures for five sources: MXB 1659−29, KS 1731−260, XTE J1701−462, EXO 0748−676  and IGR J17480−2446. Results. We find that the evolution of MXB 1659−29, KS 1731−260 and EXO 0748−676 can be well described within a deep crustal cooling scenario. Conversely, we find that the other two sources can only be explained with models beyond crustal cooling. For the peculiar emission of XTE J1701−462 we propose alternative scenarios such as residual accretion during quiescence, additional heat sources in the outer crust, and/or thermal isolation of the inner crust due to a buried magnetic field. We also explain the very recent reported temperature of IGR J17480−2446 with an additional heat deposition in the outer crust from shallow sources.

Red de seguimiento e indicadores de calidad de la titulación máster universitario en prevención de riesgos laborales

El profesorado de la red participó durante el curso 2013/14 en un proyecto para el seguimiento e indicadores de calidad de la titulación máster universitario en prevención de riesgos laborales. Este Máster comenzó a impartirse en la Escuela Politécnica Superior de la Universidad de Alicante en el curso 2012/13. En el curso 2015/16 al Máster en prevención de riesgos laborales le corresponde la renovación de su acreditación, en base a los resultados de la docencia de los cursos 2013/14 y 2014/15, por lo que los resultados del presente proyecto son de interés para la renovación de la acreditación de la titulación.