Multiple flaring activity in the supergiant fast X-ray transient IGR J08408−4503 observed with Swift

IGR  J08408−4503  is a supergiant fast X–ray transient discovered in 2006 with a confirmed association with a O8.5Ib(f) supergiant star, HD 74194. We report on the analysis of two outbursts caught by Swift /Burst Alert Telescope (BAT) on 2006 October 4 and 2008 July 5, and followed up at softer energies with Swift /X-ray Telescope (XRT). The 2008 XRT light curve shows a multiple-peaked structure with an initial bright flare that reached a flux of  ∼10⁻⁹ erg cm⁻² s⁻¹  (2–10 keV), followed by two equally bright flares within 75 ks. The spectral characteristics of the flares differ dramatically, with most of the difference, as derived via time-resolved spectroscopy, being due to absorbing column variations. We observe a gradual decrease in the N _H, derived with a fit using absorbed power-law model, as time passes. We interpret these N _H variations as due to an ionization effect produced by the first flare, resulting in a significant decrease in the measured column density towards the source. The durations of the flares as well as the times of the outbursts suggest that the orbital period is ∼35 d, if the flaring activity is interpreted within the framework of the Sidoli et al. model with the outbursts triggered by the neutron star passage inside an equatorial wind inclined with respect to the orbital plane.     

The dust scattering model cannot explain the shallow X-ray decay in GRB afterglows

A dust scattering model was recently proposed to explain the shallow X-ray decay (plateau) observed prevalently in Gamma-Ray Burst (GRB) early afterglows. In this model, the plateau is the scattered prompt X-ray emission by the dust located close (about 10 to a few hundred pc) to the GRB site. In this paper, we carefully investigate the model and find that the scattered emission undergoes strong spectral softening with time, due to the model's essential ingredient that harder X-ray photons have smaller scattering angle thus arrive earlier, while softer photons suffer larger angle scattering and arrive later. The model predicts a significant change, that is  Δβ∼ 2–3  , in the X-ray spectral index from the beginning of the plateau towards the end of the plateau, while the observed data show close to zero softening during the plateau and the plateau-to-normal transition phase. The scattering model predicts a big difference between the harder X-ray light curve and the softer X-ray light curve, i.e. the plateau in harder X-rays ends much earlier than in softer X-rays. This feature is not seen in the data. The large scattering optical depths of the dust required by the model imply strong extinction in optical,   A _V ≳ 10  , which contradicts current findings of   A _V = 0.1–0.7  from optical and X-ray afterglow observations. We conclude that the dust scattering model cannot explain the X-ray plateaus.     

Kinematics of SDSS subdwarfs: structure and substructure of the Milky Way halo

We construct a new sample of ∼1700 solar neighbourhood halo subdwarfs from the Sloan Digital Sky Survey (SDSS), selected using a reduced proper-motion diagram. Radial velocities come from the SDSS spectra and proper motions from the light-motion curve catalogue of Bramich et al. Using a photometric parallax relation to estimate distances gives us the full phase-space coordinates. Typical velocity errors are in the range  30–50 km s⁻¹  . This halo sample is one of the largest constructed to date and the disc contamination is at a level of ≲1 per cent. This enables us to calculate the halo velocity dispersion to excellent accuracy. We find that the velocity dispersion tensor is aligned in spherical polar coordinates and that  (σ _r , σ_φ, σ_θ) = (143 ± 2, 82 ± 2, 77 ± 2) km s⁻¹  . The stellar halo exhibits no net rotation, although the distribution of   v _φ  shows tentative evidence for asymmetry. The kinematics are consistent with a mildly flattened stellar density falling with distance like   r ^−3.75  .
Using the full phase-space coordinates, we look for signs of kinematic substructure in the stellar halo. We find evidence for four discrete overdensities localized in angular momentum and suggest that they may be possible accretion remnants. The most prominent is the solar neighbourhood stream previously identified by Helmi et al., but the remaining three are new. One of these overdensities is potentially associated with a group of four globular clusters (NGC 5466, NGC 6934, M2 and M13) and raises the possibility that these could have been accreted as part of a much larger progenitor.     

Color in solar granulation

Pairs of spectra exposed simultaneously in the yellow and ultraviolet show exactly the same solar granulation in the two colors. This is contrary to Vassilyeva's earlier results. The difference is probably due to her neglect of atmospheric dispersion.     

16–40 Å coronal X-ray emission during the 12 November 1966 eclipse

The solar eclipse of 12 November 1966 was used to study the coronal emission near the limbs in selected emission lines between 16 and 40 Å. Eight fixed-wavelength, curved crystal spectrometers were carried in each of 3 rocket launches to an altitude of 290 km and monitored the flux in each of eight narrow-wavelength intervals encompassing the principal emission lines from the hydrogen-like and helium-like ions of C, N, and O. At totality the emissions dropped to background levels of 1% or less of the full sun values, showing that on the solar limbs on that day there was very little emission above 17000 km in these lines.Work performed under the auspices of the U.S. Atomic Energy Commission.     

Microearthquakes in the TDP swarm, Turkey: clustering in space and time

Summary. The third occupation (experiment TDP3) of recording sites above a persistent swarm of microearthquakes near the North Anatolian Fault, with a larger seismic network and over a longer period of time, confirms and refines previous observations with greater resolution. The greater resolution in earthquake locations has revealed marked clustering in time and space. Many, perhaps most, of the earthquakes belong to clusters, where successive earthquakes originate in a very small volume and have similar fault mechanisms. Such studies allow the progression of seismic activity of small earthquakes to be followed in some detail, and may reveal features which are hidden in larger and more complex earthquake sequences.     

Simultaneous optical and incoherent scatter observations of two low-latitude auroras

During the last sunspot maximum, major auroras occurred over Boston, MA (L = 3.1) on 23/24 March 1969 and 8/9 March 1970, during which optical and incoherent scatter radar measurements were made simultaneously from the Blue Hill Observatory and Millstone Field Station, respectively. The paper presents the results of these measurements and attempts a self-consistent interpretation of them. It is found that a major increase (5–10 times) in the abundance of molecular species (O₂ and N₂) at F-region heights must have occurred; this was not accompanied by any appreciable increase in the major neutral species, atomic oxygen. From the radar data, the energy input to the F-region can be separated into direct heating by secondary electrons, downward heat flow from the magnetosphere and a low-energy non-ionizing electron flux. The total observed intensity of the predominant optical emission from atomic oxygen at 6300 Å can then be predicted satisfactorily by summing the contributions to this emission from impact excitation by ambient electrons, from the low-energy precipitating electrons and from dissociative recombination.     

Effects of random phase changes on the formation of synthetic aperture radar imagery

The effects of Gaussian random and linear phase change on the response of the matched azimuth processor of a synthetic aperture imaging radar is analyzed numerically.     

The relationship between sedimentary diatom assemblages and lakewater pH in 35 Quebec lakes,Canada

Surface sediment diatoms from 35 soft-water lakes in southern Quebec were studied to examine the relationship with lakewater pH. The lakes ranged in pH from 5.25 to 7.66. The species composition and the relative abundance of diatoms in the study lakes was found to be closely related to pH and/or factors closely associated with pH. Predictive models were developed to infer lakewater pH using simple linear regression equations of index alpha, index B, and multiple regressions using pH preference categories. Among the predictive models examined here, the multiple regression technique provided the highest correlation coefficient (r²=0.88) and the lowest standard error (±0.26 of a pH unit) in computing diatom-inferred pH. This model appears to be the most appropriate to reconstruct lake pH histories in Quebec region.     

On the mass and distance of the Quasi-Stellar Object 3C 273

For the QSO 3C 273 we derive, on the basis of two different theoretical models, expressions for a lower limit to the mass of the QSO, as a function of its distance. We conclude that an appreciable gravitational redshift component is consistent with the observational data only if the QSO mass is at least Galactic in magnitude. The setting of an independent upper limit to the QSO massM10¹⁰ M could indicate that the QSO redshift is predominantly cosmological in nature.