Unraveling the high-energy emission components of gamma-ray binaries

The high and very-high energy spectrum of gamma-ray binaries has become a challenge for all theoretical explanations since the detection of powerful, persistent GeV emission from LS 5039 and LS I +61 303 by Fermi/LAT. The spectral cutoff at a few GeV indicates that the GeV component and the fainter, hard TeV emission above 100 GeV are not directly related. We explore the possible origins of these two emission components in the framework of a young, non-accreting pulsar orbiting the massive star, and initiating the non-thermal emission through the interaction of the stellar and pulsar winds. The pulsar/stellar wind interaction in a compact orbit binary gives rise to two potential locations for particle acceleration: the shocks at the head-on collision of the winds and the termination shock caused by Coriolis forces on scales larger than the binary separation. We explore the suitability of these two locations to host the GeV and TeV emitters, respectively, through the study of their non-thermal emission along the orbit. We focus on the application of this model to LS 5039 given its well determined stellar wind with respect to other gamma-ray binaries. The application of the proposed model to LS 5039 indicates that these two potential emitter locations provide the necessary conditions for reproduction of the two-component high-energy gamma-ray spectrum of LS 5039. In addition, the ambient postshock conditions required at each of the locations are consistent with recent hydrodynamical simulations. The scenario based on the interaction of the stellar and pulsar winds is compatible with the GeV and TeV emission observed from gamma-ray binaries with unknown compact objects, such as LS 5039 and LS I +61 303.Comment: Version as published in A&

Estudio de factibilidad para la instalación de una sala de internet al servicio de la comunidad samaria: cybernet ltda

El presente trabajo tiene como finalidad determinar la factibilidad de la instalación de una sala para el acceso a la Red Mundial de Información, (CYBERNET LTDA.), puesta al servicio de la comunidad samaria, en la Avenida Libertador con Carrera 13 de esta ciudad es escaso, esto con el fin de brindarle facilidad en la obtención de la información y de servicios tecnológicos y así lograr ampliar más su conocimiento. Para la instalación de CYBERNET LTDA, se tienen en cuenta esquemas organizacionales propios de la microempresa, pero enfocando siempre factores claves como la eficiencia y calidad del servicio que se prestará, la atención y comodidad que se le debe brindar al cliente, así como incentivos para dar a conocer el servicio, mediante promociones, publicidad etc

On the origin of correlated X-ray/VHE emission from LS I +61 303

The MAGIC collaboration has recently reported correlated X-ray and very high-energy gamma-ray emission from the gamma-ray binary LS I +61 303 during ~60% of one orbit. These observations suggest that the emission in these two bands has its origin in a single particle population. We aim at improving our understanding of the source behaviour by explaining the simultaneous X-ray and VHE data through a radiation model. We use a model based on a one zone population of relativistic leptonic particles assuming dominant adiabatic losses located at the position of the compact object. The adiabatic cooling timescale is inferred from the X-ray fluxes. The model can reproduce the spectra and lightcurves in the X-ray and VHE bands. Adiabatic losses could be the key ingredient to explain the X-ray and partially the VHE lightcurves. From the best fit result, we obtain a magnetic field of B=0.2 G, a minimum luminosity budget of ~2x10^35 erg/s and a relatively high acceleration efficiency. In addition, our results seem to confirm that the GeV emission detected by Fermi does not come from the same parent particle population as the X-ray and VHE emission and the Fermi spectrum poses a constraint on the hardness of the particle spectrum at lower energies. In the context of our scenario, more sensitive observations would allow to constrain the inclination angle, which could determine the nature of the compact object

Binaries with the eyes of CTA

The binary systems that have been detected in gamma rays have proven very useful to study high-energy processes, in particular particle acceleration, emission and radiation reprocessing, and the dynamics of the underlying magnetized flows. Binary systems, either detected or potential gamma-ray emitters, can be grouped in different subclasses depending on the nature of the binary components or the origin of the particle acceleration: the interaction of the winds of either a pulsar and a massive star or two massive stars; accretion onto a compact object and jet formation; and interaction of a relativistic outflow with the external medium. We evaluate the potentialities of an instrument like the Cherenkov telescope array (CTA) to study the non-thermal physics of gamma-ray binaries, which requires the observation of high-energy phenomena at different time and spatial scales. We analyze the capability of CTA, under different configurations, to probe the spectral, temporal and spatial behavior of gamma-ray binaries in the context of the known or expected physics of these sources. CTA will be able to probe with high spectral, temporal and spatial resolution the physical processes behind the gamma-ray emission in binaries, significantly increasing as well the number of known sources. This will allow the derivation of information on the particle acceleration and emission sites qualitatively better than what is currently available

The keV-TeV connection in gamma-ray binaries

[eng] Gamma-ray binaries are systems that comprise a young, massive star and a compact object that can be either a young pulsar or a black hole. They emit radiation from radio up to tens of TeV and show flux variability along the whole electromagnetic spectrum. For three of the four detected gamma-ray binaries, the nature of the compact object is unknown. In this thesis we present a study of gamma-ray binaries through three approaches that involve the simultaneous study of these sources in X-rays and very high energy (VHE) gamma-rays. We present the discovery of correlated X-ray and VHE gamma-ray emission from LS I +61 303. The correlations indicates that the emission from these two bands could be originated in the same parent particle population, and we explore this idea through the calculation of a radiative model. This model allows us to significantly constrain the physical properties of the non-thermal emitter in LS I +61 303. For those systems where the compact object is a young pulsar, the interaction between the stellar and pulsar winds will give rise to strong shocks. The shocked pulsar wind is the candidate location for non-thermal emission from these systems. The shocked stellar wind should give rise to a thermal X-ray spectrum, but no such features have been detected in the X-ray spectrum of gamma-ray binaries. We present a model of the thermal emission of the shocked stellar wind and use it to constrain the pulsar properties. We have applied this method to two X-ray observations of LS 5039 and have successfully constrained the pulsar spin-down luminosity. Finally, we present a search for VHE emission from Scorpius X-1 through a simultaneous X-ray and VHE gamma-ray campaign. The X-ray observations allowed us to select black-hole states where non-thermal X-ray emission has been detected. We did not find significant VHE emission in any of the black hole states, but the upper limits derived will prove useful in future modelling of the non-thermal emitter in the source.[cat] Les binàries de raigs gamma són sistemes binaries formats per una estrella jove i massiva i un objecte compacte, que pot ser un púlsar jove o un forat negre, que emeten radiació fins a desenes de TeV i mostren variabilitat orbital en totes les bandes d'emissió, des de radio fins a raigs gamma. En el cas de tres de les quatre binàries de raigs gamma detectades avui dia, se'n desconeix la natura de l'objecte compacte. En aquesta tesi presentem un estudi de les binàries de raigs gamma mitjançant tres treballs complementaris que involucren l'estudi simultani d'aquestes fonts en raigs X i raigs gamma de molt alta energia. En primer lloc presentem el descobriment d'emissió en raigs X i raigs gamma de molt alta energia correlades en el temps al sistema LS I +61 303. Aquesta correlació ens indica que l'emissió en les dues bandes pot provenir d'una única població d'electrons, i ho confirmem mitjançant la realització d'un model teòric de radiació que ens permet restringir significativament les propietats físiques de l'emissor no tèrmic de la font. En cas que la font energètica dels sistemes sigui un púlsar, la interacció entre els vents de l'estrella i el púlsar dona lloc a una regió d'interacció on el vent xocat del púlsar accelera partícules i emet des de radio fins a raigs gamma. A l'espectre de raigs X, però, no es detecta l'emissió tèrmica del vent xocat de l'estrella, que s'escalfa fins a desenes de milers de graus. Això ens ha permès estudiar la forma de la regió d'interacció, determinada principalment per la potència del púlsar, i fer un càlcul teòric de l'emissió en raigs X tèrmics. Hem aplicat aquest model al sistema LS 5039 i hem pogut determinar la potència del púlsar, fet important per a la modelització de l'emissió no tèrmica de la font. Finalment, presentem la cerca d'emissió de raigs gamma provinent de sistemes binaris fins ara no detectats. Una campanya simultània en raigs X i raigs gamma ens va permetre seleccionar les dades de molt alta energia del microquàsar Sco X-1 en funció de l'estat d'acreció sobre l'objecte compacte. Tot i no detectar la font en raigs gamma, els límits superiors obtinguts permeten restringir les propietats físiques de Sco X-1 rellevants per a l'emissió en molt alta energia

On the origin of correlated X-ray/VHE emission from LS I +61 303

The MAGIC collaboration has recently reported correlated X-ray and very high-energy gamma-ray emission from the gamma-ray binary LS I +61 303 during ~60% of one orbit. These observations suggest that the emission in these two bands has its origin in a single particle population. We aim at improving our understanding of the source behaviour by explaining the simultaneous X-ray and VHE data through a radiation model. We use a model based on a one zone population of relativistic leptonic particles assuming dominant adiabatic losses located at the position of the compact object. The adiabatic cooling timescale is inferred from the X-ray fluxes. The model can reproduce the spectra and lightcurves in the X-ray and VHE bands. Adiabatic losses could be the key ingredient to explain the X-ray and partially the VHE lightcurves. From the best fit result, we obtain a magnetic field of B=0.2 G, a minimum luminosity budget of ~2x10^35 erg/s and a relatively high acceleration efficiency. In addition, our results seem to confirm that the GeV emission detected by Fermi does not come from the same parent particle population as the X-ray and VHE emission and the Fermi spectrum poses a constraint on the hardness of the particle spectrum at lower energies. In the context of our scenario, more sensitive observations would allow to constrain the inclination angle, which could determine the nature of the compact object

Análisis a priori de una situación de optimización en segundo de Educación Primaria

Resumen tomado de la publicaciónSe presenta una manera de introducir un problema de optimización en el primer ciclo de Educación Primaria, mediante una transposición didáctica que preserva la esencia de la optimización en un contexto matemático escolar propio de la etapa. Se afronta un problema de este tipo en el tránsito del número natural a la medida, utilizando la ingeniería didáctica como método de investigación. En este marco se diseña una situación didáctica basada en el análisis a priori. El objetivo de esta situación es doble: por un lado, la intervención razonada en los sistemas didácticos; por otra parte, producir conocimiento sobre la forma en la que se construyen y comunican problemas de optimización relativos a la medida, en edad infantil.CantabriaES

Thermal X-Ray emission from the shocked stellar wind of pulsar gamma-ray binaries

Gamma-ray loud X-ray binaries are binary systems that show non-thermal broadband emission from radio to gamma rays. If the system comprises a massive star and a young non-accreting pulsar, their winds will collide producing broadband non-thermal emission, most likely originated in the shocked pulsar wind. Thermal X-ray emission is expected from the shocked stellar wind, but until now it has neither been detected nor studied in the context of gamma-ray binaries. We present a semi-analytic model of the thermal X-ray emission from the shocked stellar wind in pulsar gamma-ray binaries, and find that the thermal X-ray emission increases monotonically with the pulsar spin-down luminosity, reaching luminosities of the order of 10^33 erg/s. The lack of thermal features in the X-ray spectrum of gamma-ray binaries can then be used to constrain the properties of the pulsar and stellar winds. By fitting the observed X-ray spectra of gamma-ray binaries with a source model composed of an absorbed non-thermal power law and the computed thermal X-ray emission, we are able to derive upper limits on the spin-down luminosity of the putative pulsar. We applied this method to LS 5039, the only gamma-ray binary with a radial, powerful wind, and obtain an upper limit on the pulsar spin-down luminosity of ~6x10^36 erg/s. Given the energetic constraints from its high-energy gamma-ray emission, a non-thermal to spin-down luminosity ratio very close to unity may be required