The very faint hard state of the persistent neutron star X-ray binary SLX 1737-282 near the Galactic centre

We report on a detailed study of the spectral and temporal properties of the neutron star low mass X-ray binary SLX 1737-282, which is located only ~1degr away from Sgr A. The system is expected to have a short orbital period, even within the ultra-compact regime, given its persistent nature at low X-ray luminosities and the long duration thermonuclear burst that it has displayed. We have analysed a Suzaku (18 ks) observation and an XMM-Newton (39 ks) observation taken 7 years apart. We infer (0.5-10 keV) X-ray luminosities in the range 3-6 x10^35erg s-1, in agreement with previous findings. The spectra are well described by a relatively cool (kTbb = 0.5 keV) black body component plus a Comptonized emission component with {\Gamma} ~1.5-1.7. These values are consistent with the source being in a faint hard state, as confirmed by the ~ 20 per cent fractional root mean square amplitude of the fast variability (0.1 - 7 Hz) inferred from the XMM-Newton data. The electron temperature of the corona is >7 keV for the Suzaku observation, but it is measured to be as low as ~2 keV in the XMM-Newton data at higher flux. The latter is significantly lower than expected for systems in the hard state. We searched for X-ray pulsations and imposed an upper limit to their semi-amplitude of 2 per cent (0.001 - 7 Hz). Finally, we investigated the origin of the low frequency variability emission present in the XMM-Newton data and ruled out an absorption dip origin. This constraint the orbital inclination of the system to 65 degr unless the orbital period is longer than 11 hr (i.e. the length of the XMM-Newton observation).Comment: 7 pages, 4 figures, 1 table. Accepted for publication in MNRA

TeV Burst of Gamma-Ray Bursts and Ultra High Energy Cosmic Rays

Some recent experiments detecting very high energy (VHE) gamma-rays above 10-20 TeV independently reported VHE bursts for some of bright gamma-ray bursts (GRBs). If these signals are truly from GRBs, these GRBs must emit a much larger amount of energy as VHE gamma-rays than in the ordinary photon energy range of GRBs (keV-MeV). We show that such extreme phenomena can be reasonably explained by synchrotron radiation of protons accelerated to \sim 10^{20-21} eV, which has been predicted by Totani (1998a). Protons seem to carry about (m_p/m_e) times larger energy than electrons, and hence the total energy liberated by one GRB becomes as large as \sim 10^{56} (\Delta \Omega / 4 \pi) ergs. Therefore a strong beaming of GRB emission is highly likely. Extension of the VHE spectrum beyond 20 TeV gives a nearly model-independent lower limit of the Lorentz factor of GRBs, as \gamma \gtilde 500. Furthermore, our model gives the correct energy range and time variability of ordinary keV-MeV gamma-rays of GRBs by synchrotron radiation of electrons. Therefore the VHE bursts of GRBs strongly support the hypothesis that ultra high energy cosmic rays observed on the Earth are produced by GRBs.Comment: Final version to appear in ApJ Lett. Emphasizing that the extremely large energy required in this model is not theoretically impossible if GRB emission is strongly beamed. References update

Quintessence and the Swampland: The Parametrically Controlled Regime of Moduli Space

We provide evidence that slow roll is not possible in any parametrically controlled regime of the moduli space of string theory. This is proven in full generality in the asymptotic limit of the moduli space of type II and heterotic Calabi-Yau compactifications for the dilaton and any number of Kähler moduli. Our results suggest that in order to build quintessence into string theory one must work in the interior of moduli space where numerical, even if not parametric, control could still be achieved

Estudio morfométrico de las abejas andaluzas

The biological and behavioral characteristics of the iberian bees are much less known than the other european races. This paper studies the morphological characteristics (Proboscis length; Forewing length; Forewing width; Cubital vein a; Cubital vein b; Cubital index a/b; Hindwing length; Hindwing width; Femur length; Tibia length; Metatarsus length; Metatarsus width; Width of tomentum at tergite 4; Pigmentation of tergite 3) of bees used in andalusian apiculture. Our results coincide with those described for Apis mellifera iberica.Las características biológicas y de comportamiento que presentan las abejas de la península ibérica son menos conocidas que las que presentan otras razas europeas. En el presente trabajo estudiamos las características morfológicas (longitud de la proboscis; longitud del ala delantera derecha; anchura del ala delantera derecha; vena cubital a; vena cubital b; índice cubital a/b; longitud del ala trasera derecha; anchura del ala trasera derecha; longitud del fémur; longitud de la tibia; longitud del metatarso; anchura del metatarso; longitud del tomentun del terguito 4º y pigmentación del terguito 3º) que presentan las abejas empleadas en la apicultura andaluza. Nuestros resultados coinciden con los descritos para Apis mellifera iberica

Abejas, apicultura y el nuevo mundo

In the New World, some stingless bees were kept by the native population. In Central America, maya beekeepers worked with Mellipona beecheii, in Yucatan and adjacent regions. The arrival in North America of the first beehives was in 1691 and it were sent to Virginia by the Council of the Virginia Company in London. Concerning the introduction to Central and South America the first ones arrived from Spain and Portugal towards the end of the 18th century, probably to Brazil. Prior to 1800, the european breeds taken to America were probably Apis mellifera mellifera and Apis mellifera iberica. At the turn of the century, a new european breed was imported from Italy (Apis mellifera ligustica). American apiculture has used these breeds and crossbreeds virtually up to the present day. In 1956, tropical african queens of the breed Apis mellifera scutellata were introduced to Brazil. Its crosses involving european breeds gave rise to africanized bees, which have spread over almost the whole of South, Central and North America.Los nativos del Nuevo Mundo utilizaban algunas abejas sin aguijón. En América Central los apicultores mayas trabajaron, en el Yucatán y regiones adyacentes, con Mellipona beecheii. Los nativos del Nuevo Mundo utilizaban algunas abejas sin aguijón. En América Central los apicultores mayas trabajaron, en el Yucatán y regiones adyacentes, con Mellipona beecheii. La llegada a América del Norte de las primeras colmenas se produjo en 1691. Fueron enviadas a Virginia desde Inglaterra por la Virginia Company. Las primeras colmenas enviadas a América Central y del Sur, probablemente a Brasil, a finales del siglo XVIII, procedían de España y Portugal. Antes de 1800 las razas europeas llevadas a Amé-rica fueron, probablemente, Apis mellifera mellifera y Apis mellifera iberica. A fin de siglo se introduce otra (Apis mellifera ligustica) procedente de Italia. La apicultura americana ha empleado las razas mencionadas y sus cruces, hasta nuestros días. En 1956 se introdujeron en Brasil reinas de Apis mellifera scutellata, procedentes de Africa tropical. Las abejas procedentes de su cruce con razas europeas, “africanizadas”, se han extendido por casi la totalidad del continente americano

Galaxy Clusters in the Line of Sight to Background Quasars: I. Survey Design and Incidence of MgII Absorbers at Cluster Redshifts

We describe the first optical survey of absorption systems associated with galaxy clusters at z= 0.3-0.9. We have cross-correlated SDSS DR3 quasars with high-redshift cluster/group candidates from the Red-Sequence Cluster Survey. We have found 442 quasar-cluster pairs for which the MgII doublet might be detected at a transverse (physical) distance d<2 Mpc from the cluster centers. To investigate the incidence (dN/dz) and equivalent-width distribution n(W) of MgII systems at cluster redshifts, two statistical samples were drawn out of these pairs: one made of high-resolution spectroscopic quasar observations (46 pairs), and one made of quasars used in MgII searches found in the literature (375 pairs). The results are: (1) the population of strong MgII systems (W_0>2.0 Ang.) near cluster redshifts shows a significant (>3 sigma) overabundance (up to a factor of 15) when compared with the 'field' population; (2) the overabundance is more evident at smaller distances (d<1 Mpc) than larger distances (d<2 Mpc) from the cluster center; and, (3) the population of weak MgII systems (W_0<0.3 Ang.) near cluster redshifts conform to the field statistics. Unlike in the field, this dichotomy makes n(W) in clusters appear flat and well fitted by a power-law in the entire W-range. A sub-sample of the most massive clusters yields a stronger and still significant signal. Since either the absorber number density or filling-factor/cross-section affects the absorber statistics, an interesting possibility is that we have detected the signature of truncated halos due to environmental effects. Thus, we argue that the excess of strong systems is due to a population of absorbers in an overdense galaxy environment, and the lack of weak systems to a different population, that got destroyed in the cluster environment. (Abridged)Comment: Accepted for publication in the Astrophysical Journa