SUPERSYMMETRY IN COMPACTIFICATIONS OF THE HETEROTIC STRING

title: Microlensing binaries with brown dwarf companions

title: MICROLENSING DISCOVERY OF A TIGHT, LOW-MASS-RATIO PLANETARY-MASS OBJECT AROUND AN OLD FIELD BROWN DWARF
abstract: Observations of accretion disks around young brown dwarfs (BDs) have led to the speculation that they may form planetary systems similar to normal stars. While there have been several detections of planetary-mass objects around BDs (2MASS 1207-3932 and 2MASS 0441-2301), these companions have relatively large mass ratios and projected separations, suggesting that they formed in a manner analogous to stellar binaries. We present the discovery of a planetary-mass object orbiting a field BD via gravitational microlensing, OGLE-2012-BLG-0358Lb. The system is a low secondary/primary mass ratio (0.080 ± 0.001), relatively tightly separated (~0.87 AU) binary composed of a planetary-mass object with 1.9 ± 0.2 Jupiter masses orbiting a BD with a mass 0.022 M ☉. The relatively small mass ratio and separation suggest that the companion may have formed in a protoplanetary disk around the BD host in a manner analogous to planets.

title: A giant planet beyond the snow line in microlensing event OGLE-2011-BLG-0251
abstract: We present the analysis of the gravitational microlensing event OGLE-2011-BLG-0251. This anomalous event was observed by several survey and follow-up collaborations conducting microlensing observations towards the Galactic bulge.  Based on detailed modelling of the observed light curve, we find that the lens is composed of two masses with a mass ratioq = 1.9 × 10 −3 . Thanks to our detection of higher-order effects on the light curve due to the Earth’s orbital motion and the finite size of source, we are able to measure the mass and distance to the lens unambiguously.  We find that the lens is made up of a planet of mass 0.53 ± 0.21 MJ orbiting an M dwarf host star with a mass of 0.26 ± 0.11 M� .T he planetary system is located at a distance of 2.57 ± 0.61 kpc towards the Galactic centre. The projected separation of the planet from its host star is d = 1.408 ± 0.019, in units of the Einstein radius, which corresponds to 2.72 ± 0.75 AU in physical units. We also identified a competitive model with similar planet and host star masses, but with a smaller orbital radius of 1.50 ± 0.50 AU. The planet is therefore located beyond the snow line of its host star, which we estimate to be around ∼1−1. 5A U.

title: The calculation of planar one-loop diagrams in string theory using the BRS formalism
abstract: The fact is exploited that the operator counting the number of non-transverse modes for the bosonic string in 26 dimensions can be written as the anticommutator of the BRS charge Q with another operator to calculate planar one-loop diagrams. This results in a significant simplification over the earlier calculation of Brink and Olive.

title: Design and Construction of the SSCL Magnet Test Laboratory Cryogenic Systems
abstract: The intent of this document is to provide a brief summary of the execution, by Process Systems International, Inc. (PSI), of the Design and Construction of the SSCL Magnet Test Laboratory Cryogenic Systems. This $30 million project requires the expenditure of over 200,000 manhours and the procurement of $17 million in materials within a two year period.

title: Fission following fusion of Ni+Sn.
abstract: Excitation functions for fission were measured for /sup 58,64/Ni beams incident on the even /sup 112//sup --//sup 124/Sn targets at energies extending from well below to about 1.5 times the Coulomb barrier. Fission was identified by kinematic coincidence between fission fragments. Angle integrated fission cross sections were obtained from angular distributions taken at several energies for all systems. From these and the previously measured cross sections for evaporation residues, we obtain the total fusion cross sections and fission probabilities over the energy range 150 approx.