119233030
Dynamics of neutrino-driven winds: inclusion of accurate weak interaction rates in strong magnetic fields
Solving Newtonian steady-state wind equations while considering the accurate weak interaction rates and magnetic fields (MFs) of young neutron stars, we study the dynamics and nucleosynthesis of neutrino-driven winds (NDWs) from proto neutron stars (PNSs). For a typical 1.4 M ⊙ PNS model, we find that the nucleosynthesis products are closely related to the luminosity of neutrinos and anti-neutrinos. The lower the luminosity is, the larger is the effect on the NDWs caused by weak interactions and MFs. At a high anti-neutrino luminosity of typically 8 × 10 51 erg s −1 , neutrinos and anti-neutrinos dominate the processes in an NDW and the MFs hardly change the wind’s properties. But at a low anti-neutrino luminosity of 10 51 erg s −1 at the late stage of an NDW the mass of the product and process of nucleosynthesis are changed significantly in strong MFs. Therefore, in most of the models considered for the NDWs from PNSs, based on our calculations, the influences of MFs and the net weak interactions on the nucleosynthesis are not significant.
119390755
The X-Ray Position and Infrared Counterpart of the Eclipsing X-Ray Pulsar OAO 1657–415
We have measured the precise position of the 38 s eclipsing X-ray pulsar OAO 1657-415 with the Chandra X-Ray Observatory: (J2000) = 17h00m4890, (J2000) = -4139216, error radius = 05. Based on the previously measured pulsar mass function and X-ray eclipse duration, this 10.4 day high-mass X-ray binary is believed to contain a B supergiant companion. Deep optical imaging of the field did not detect any stars at the Chandra source position, setting a limit of V > 23. However, near-infrared imaging revealed a relatively bright star (J = 14.1, H = 11.9, Ks = 10.7) coincident with the Chandra position, and we identify this star as the infrared counterpart of OAO 1657-415. The infrared colors and magnitudes and the optical nondetections for this star are all consistent with a highly reddened B supergiant (AV = 20.4
18351437
Search for the Optical Counterparts of Southern Anomalous X-Ray Pulsars and Radio-Quiet Neutron Stars in Young Supernova Remnants
We report on our search for the optical counterparts of the Southern Hemisphere anomalous X-ray pulsar 1E1048.1-5937 and the radio-quiet neutron stars in supernova remnants Puppis A, RCW 103, and PKS 1209-52. The observations were carried out with the new MIT/CfA MagIC camera on the Magellan-I 6.5 m telescope in Chile. We present deep multiband optical images of the X-ray error circles for each of these targets and discuss the resulting candidates and limits.
119229485
Classification study of WISE infrared sources: identification of candidate asymptotic giant branch stars
In the Wide-field Infrared Survey Explorer (WISE) all-sky source catalog there are 76 million mid-infrared point sources that were detected in the first three WISE bands and have association with only one 2MASS near-IR source within 3′′. We search for their identifications in the SIMBAD database and find 3.2 million identified sources. Based on these known sources, we establish three criteria for selecting candidate asymptotic giant branch (AGB) stars in the Galaxy, which are three defined zones in a color-color diagram, Galactic latitude |b| ≤ 20°, and “corrected” WISE third-band W3 c ≤11. Applying these criteria to the WISE+2MASS sources, 1.37 million of them are selected. We analyze the WISE third-band W3 distribution of the selected sources, and further establish that W3≤8 is required in order to exclude a large fraction of normal stars from them. We therefore find 0.47 million candidate AGB stars in our Galaxy from the WISE source catalog. Using W3 c , we estimate their distances and derive their Galactic distributions. The candidates are generally distributed around the Galactic center uniformly, with 68% (1-σ) of them within approximately 8 kpc. We discuss the idea that optical spectroscopy can be used to verify the C-rich AGB stars in our candidates, and thus a fraction of them (~10%) will be good targets for the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) survey that is planned to start in fall of 2012.
119069538
Search for gamma-ray emission from four accreting millisecond pulsars with Fermi/LAT
We report our search for -ray emission in the energy range from 100 MeV to 300 GeV from four Accreting Millisecond Pulsars (AMPs), SAX J1808.4 3658, IGR J00291+5934, XTE J1814 338, and XTE J0929 314. The data are from four-year observations carried out by Large Area Telescope (LAT) onboard the Fermi -ray Space Telescope. The AMPs were not detected, and their -ray luminosity upper limits we obtain are 5.1 × 10 33 ergs s −1 for SAX J1808.4 3658, 2.1 × 10 33 ergs s −1 for IGR J00291+5934, 1.2 × 10 34 ergs s −1 for XTE J1814 338, and 2.2 × 10 33 ergs s −1 for XTE J0929 314. We compare our results with -ray irradiation luminosities required for producing optical modulations seen from the companions in the AMPs, which has been suggested by Takata et al. (2012), and our upper limits have excluded -ray emission as the heating source in these systems except XTE J0929 314, the upper limit of which is not deep enough. Our results also do not support the model proposed by Takata et al. (2012) that relatively strong -ray emission could arise from the outer gap of a high-mass neutron star controlled by the photon-photon pair-creation for the AMPs. Two AMPs, SAX J1808.4 3658 and IGR J00291+5934, have the measurements of their spin-down rates, and we derive the upper limits of their -ray conversion efficiencies, which are 57% and 3%, respectively. We discuss the implications to the AMP systems by comparing the efficiency upper limit values with that of 20 -ray millisecond pulsars (MSP) detected by Fermi and the newly discovered transitional MSP binary J1023+0038. Subject headings: pulsars: general – stars: neutron – binaries: close – gamma rays: stars
14349816
The Near-infrared Counterpart to the Anomalous X-ray Pulsar 1e 1048.1−5937
We report our discovery of the likely near-infrared counter part to the anomalous X-ray pulsar (AXP) 1E 1048.1−5937, using observations from the 6.5 m Baade (Magellan I) te lescope in Chile. We derived a precise position for the X-ray source using archival data from t heChandra X-Ray Observatory. Since this position is inconsistent with a position reported earlier from XMM-Newton, we conservatively considered eight optical and near-infrared sources within both error circles as cand id te counterparts, although we also show that the XMM-Newton observation likely suffered from attitude reconstruction problems. Two of the infrared objects have unusual colors, and one of these has colors consistent with t hose of the identified counterparts of two other AXPs. The latter object is the only source detected within the Chandra error circle, and we identify it as the counterpart to 1E 1048.1 −5937. This is the first AXP counterpart detected in multiple i nfrared bands, with magnitudes J=21.7(3),H=20.8(3), andK=19.4(3). There is marginal evidence for spectral flattenin g at longer wavelengths. Subject headings: pulsars: individual (1E 1048.1 −5937) — stars: neutron
119184301
The Zb(10610) and Zb(10650) as axial-vector tetraquark states in the QCD sum rules
Abstract In this article, we study the axial-vector mesons Z b ( 10 610 ) and Z b ( 10 650 ) with the C γ μ – C γ 5 type and C γ μ – C γ ν type interpolating currents, respectively, by carrying out the operator product expansion to the vacuum condensates up to dimension 10. In calculations, we explore the energy scale dependence of the QCD spectral densities of the hidden bottom tetraquark states in detail for the first time, and suggest a formula μ = M X / Y / Z 2 − ( 2 M b ) 2 with the effective mass M b = 5.13 GeV to determine the energy scales. The numerical results favor assigning the Z b ( 10 610 ) and Z b ( 10 650 ) as the C γ μ – C γ 5 type and C γ μ – C γ ν type hidden bottom tetraquark states, respectively. We obtain the mass of the J PC = 1 + + hidden bottom tetraquark state as a byproduct, which can be compared to the experimental data in the futures. Furthermore, we study the strong decays Z b ± ( 10 610 ) → ϒ π ± , η b ρ ± with the three-point QCD sum rules, the decay widths also support assigning the Z b ( 10 610 ) as the C γ μ – C γ 5 type hidden bottom tetraquark state.
15030872
The Strong coupling constant g(D* D pi) and final-state interactions
In this article, we study the contribution from the final-state interactions to the strong coupling constant $g_{D^* D \pi}$. We take an assumption that the momentum transfers in the strong decay $D^{*+} \to D^0 \pi^+$ be large to validate the operator product expansion in the light-cone QCD sum rules. At large momentum transfers, the final-state interactions play an important role, and we should take them into account.
18719624
Warm Molecular Gas in Galaxy-Galaxy Merger NGC 6090
We present Submillimeter Array observations of the CO (2-1) and (3-2) transitions toward the merging galaxies of NGC 6090. The high-resolution CO data reveal three gas concentrations. The main component is peaking in the overlap region between the two galaxies, where the near-IR and radio continuum emission are weak. The CO (2-1) emission from the face-on galaxy NGC 6090E is somewhat stronger than that from the edge-on galaxy NGC 6090W. The CO (3-2) emission peaks in the overlap region, similar to the CO (2-1) emission. More than 50% of the CO (3-2) emission arises from the 2'' (1.2 kpc) area of the overlap region. There appears to be CO (3-2) emission toward the nuclear region and the northwest arm of NGC 6090E, while no CO (3-2) emission is detected toward NGC 6090W. Unlike the CO gas, most of the radio continuum emission comes from NGC 6090E. The strong CO emission, together with the weak radio continuum emission, suggests that star formation in the overlap region has not proceeded long enough to produce significant numbers of supernovae that would be detectable from their radio continuum emission.
55540815
Abelian and non-Abelian anyons in integer quantum anomalous Hall effect and topological phase transitions via superconducting proximity effect
We study the quantum anomalous Hall effect described by a class of two-component Haldane models on square lattices. We show that the latter can be transformed into a pseudospin triplet p + ip-wave paired superfluid. In the long wavelength limit, the ground-statewave function is described by Halperin's ( 1,1,-1) state of neutral fermions analogous to the double-layer quantum Hall effect. The vortex excitations are charge e/2 Abelian anyons which carry a neutral Dirac fermion zero mode. The superconducting proximity effect induces "tunneling" between "layers" which leads to topological phase transitions whereby the Dirac fermion zero mode fractionalizes and Majorana fermions emerge in the edge states. The charge e/2 vortex excitation carrying a Majorana zero mode is a non-Abelian anyon. The proximity effect can also drive a conventional insulator into a quantum anomalous Hall effect state with a Majorana edge mode and the non-Abelian vortex excitations.
117063918
Recent physics results at BES
¢ 2 S£ and 33 pb¤ 1 ψ ¥¥ events collected at BES-II detector, some charm physics results are obtained. In J ¡ ψ decay, we observed an unknown resonance X(1835) and study the controversial particle σ and κ. In ψ ¢ 2 S£ decay, we test the " 12% rule " via many decay modes and find many new χ cJ decay channels. In ψ ¥¥ decay, we observed the non-D ¯ D decay via ψ ¥¥ § ¦ π ¨ π ¤ J ¡ ψ and study the semi-leptonic decay of D meson. In addition, we give the preliminary ψ ¥¥ resonance parameters with higher precision. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence.