The rotational broadening of V395 Car - implications on compact object's mass

CONTEXT: The masses previously obtained for the X-ray binary 2S0921-630 inferred a compact object that was either a high-mass neutron star or low-mass black-hole, but used a previously published value for the rotational broadening (vsini) with large uncertainties. AIMS: We aim to determine an accurate mass for the compact object through an improved measurement of the secondary star's projected equatorial rotational velocity. METHODS: We have used UVES echelle spectroscopy to determine the vsini of the secondary star (V395 Car) in the low-mass X-ray binary 2S0921-630 by comparison to an artificially broadened spectral-type template star. In addition, we have also measured vsini from a single high signal-to-noise ratio absorption line profile calculated using the method of Least-Squares Deconvolution (LSD). RESULTS: We determine vsini to lie between 31.3+/-0.5km/s to 34.7+/-0.5km/s (assuming zero and continuum limb darkening, respectively) in disagreement with revious results based on intermediate resolution spectroscopy obtained with the 3.6m NTT. Using our revised vsini value in combination with the secondary star's radial velocity gives a binary mass ratio of 0.281+/-0.034. Furthermore, assuming a binary inclination angle of 75 degrees gives a compact object mass of 1.37+/-0.13Mo. CONCLUSIONS: We find that using relatively low-resolution spectroscopy can result in systemic uncertainties in the measured vsini values obtained using standard methods. We suggest the use of LSD as a secondary, reliable check of the results as LSD allows one to directly discern the shape of the absorption line profile. In the light of the new vsini measurement, we have revised down the compact object's mass, such that it is now compatible with a canonical neutron star mass.Comment: 5 pages, 7 figures, accpeted by A

Electronic States in Diffused Quantum Wells

In the present study we calculate the energy values and the spatial distributions of the bound electronic states in some diffused quantum wells. The calculations are performed within the virtual crystal approximation, $sp^3 s^*$ spin dependent empirical tight-binding model and the surface Green function matching method. A good agreement is found between our results and experimental data obtained for AlGaAs/GaAs quantum wells with thermally induced changes in the profile at the interfaces. Our calculations show that for diffusion lengths $L_{D}=20\div100$ {\AA} the transition (C3-HH3) is not sensitive to the diffusion length, but the transitions (C1-HH1), (C1-LH1), (C2-HH2) and (C2-LH2) display large "blue shifts" as L_{D} increases. For diffusion lengths $L_{D}=0\div20$ {\AA} the transitions (C1-HH1) and (C1-LH1) are less sensitive to the L_{D} changes than the (C3-HH3) transition. The observed dependence is explained in terms of the bound states spatial distributions.Comment: ReVTeX file, 7pp., no macros, 4 figures available on the reques

Investigating the post-stimulus undershoot of the BOLD signal – A simultaneous fMRI and fNIRS study

3

Angle dependence of Andreev scattering at semiconductor-superconductor interfaces

We study the angle dependence of the Andreev scattering at a semiconductor-superconductor interface, generalizing the one-dimensional theory of Blonder, Tinkham and Klapwijk. An increase of the momentum parallel to the interface leads to suppression of the probability of Andreev reflection and increase of the probability of normal reflection. We show that in the presence of a Fermi velocity mismatch between the semiconductor and the superconductor the angles of incidence and transmission are related according to the well-known Snell's law in optics. As a consequence there is a critical angle of incidence above which only normal reflection exists. For two and three-dimensional interfaces a lower excess current compared to ballistic transport with perpendicular incidence is found. Thus, the one-dimensional BTK model overestimates the barrier strength for two and three-dimensional interfaces.Comment: 8 pages including 3 figures (revised, 6 references added

Near-infrared spectroscopy can detect brain activity during a color-word matching Stroop task in an event-related design

Brai nactivit ycanbemonitore dnon-invasivel ybynear-infrare dspectroscop y(NIRS) ,whic hhas severa ladvantage sincompariso nwit hothe rimagin gmethods ,suc hasflexibility ,portability ,low cost an dbiochemica lspecificity .Moreover ,patient san dchildre ncanberepetitivel yexamined .Therefore ,the objectiv eofthestud ywa stotes tthefeasibilit yofNIR Sfortheevent-relate dapproac hinfunctiona lbrain activatio nstudie swit hcognitiv eparadigms .Thus ,change sintheconcentratio nofoxy- ,deoxy- ,an dtotal hemoglobi nwer emeasure d byNIR Sin14health ysubject swhil eperformin ga color–wor d matching Stroo p tas k in an event-relate d design .Th ehemodynami crespons e(increas ein theconcentratio n of oxy-/tota lhemoglobi n an d decreas ein theconcentratio n ofdeoxy-hemoglobin )wa sstronge rduring incongruen tcompare dtocongruen tan dneutra ltrial softheStroo ptas kinthelatera lprefronta lcortex bilaterally .Thi sstronge rhemodynami crespons ewa sinterprete dasa stronge rbrai nactivatio nduring incongruen ttrial softheStroo ptask ,du etointerference .A ne w metho dforNIR Sdat aevaluatio nthat enable stheanalysi softhehemodynami crespons etoeac hsingl etria lisintroduced .Eac hhemodynamic respons ewa scharacterize dbytheparameter sgain ,lagan ddispersio nofa Gaussia nfunctio nfitte dby nonlinea rregression .Specifi cdifference sbetwee ntheincongruen tan dneutra lconditio nwer efoun dfor gai nan dlag .Further ,thes eparameter swer ecorrelate dwit hthebehaviora lperformance .Inconclusion, brai nactivit yma ybestudie d byNIR Susin gcognitiv estimul iinanevent-relate d design

Atmospheric velocity fields in tepid main sequence stars

The line profiles of the stars with v sin i below a few km/s can reveal direct signatures of local velocity fields (e.g. convection) in stellar atmospheres. This effect is well established in cool main sequence stars, and has been detected and studied in three A stars. This paper reports observations of main sequence B, A and F stars with two goals: (1) to identify additional stars having sufficiently low values of v sin i to search for spectral line profile signatures of local velocity fields, and (2) to explore how the signatures of the local velocity fields in the atmosphere depend on stellar parameters such as effective temperature T_eff and peculiarity type. For stars having T_eff below about 10000 K, we always detect local atmospheric velocity fields indirectly through a non-zero microturbulence parameter, but not for hotter stars. Among the A and F stars in our sample having the sharpest lines, direct tracers of atmospheric velocity fields are found in six new stars. The velocity field signatures identified include asymmetric excess line wing absorption, deeper in the blue line wing than in the red; line profiles of strong lines that are poorly fit by computed profiles; and strong lines that are broader than they should be for the v sin i values deduced from weak lines. These effects are found in both normal and Am stars, but seem stronger in Am stars. These data still have not been satisfactorily explained by models of atmospheric convection, including numerical simulations.Comment: Acepted for publication by Astronomy and Astrophysic

Models of infrared spectra of Sakurai's Object (V4334 Sgr) in 1997

Theoretical spectral energy distributions computed for a grid of hydrogen-deficient and carbon-rich model atmospheres have been compared with the observed infrared (1--2.5 $\mu$m) spectra of V4334 Sgr (Sakurai's Object) on 1997 April 21 and July 13. The comparison yields an effective temperature of \Tef = 5500 $\pm$ 200 K for the April date and \Tef = 5250 $\pm$ 200 K for July. The observed spectra are well fitted by Asplund et al. (1999) abundances, except that the carbon abundance is higher by 0.3 dex. Hot dust produces significant excess continuum at the long wavelength ends of the 1997 spectra. \keywords{Stars: individual: V4334 Sgr (Sakurai's Object) -- Stars: AGB and post-AGB evolution -- Stars: model atmospheres -- Stars: energy distributions -- Stars: effective temperatures}Comment: 6 pages, 7 eps figs, accepted for A

Modelling the light variability of the Ap star epsilon Ursae Majoris

We simulate the light variability of the Ap star epsUMa using the observed surface distributions of Fe, Cr, Ca, Mn, Mg, Sr and Ti obtained with the help of Doppler Imaging technique. Using all photometric data available we specified light variations of epsUMa modulated by its rotation from far UV to IR. We employed the LLmodels stellar model atmosphere code to predict the light variability in different photometric systems. The rotational period of epsUMa is refined to 5d088631(18). It is shown that the observed light variability can be explained as a result of the redistribution of radiative flux from the UV spectral region to the visual caused by the inhomogeneous surface distribution of chemical elements. Among seven mapped elements, only Fe and Cr significantly contribute to the amplitude of the observed light variability. In general, we find a very good agreement between theory and observations. We confirm the important role of Fe and Cr to the magnitude of the well-known depression around 5200 \AA\ through the analysis of the peculiar $a$-parameter. Finally, we show that the abundance spots of considered elements cannot explain the observed variability in near UV and $\beta$ index which are likely due to some other causes. The inhomogeneous surface distribution of chemical elements can explain most of the observed light variability of the A-type CP star epsUMa.Comment: Accepted in A&A, 10 pages, 9 figures, 3 table