A 928 sq m (10000 sq ft) solar array

As the power requirements for space vehicles increases, the area of solar arrays that convert solar energy to usable electrical power increases. The requirements for a 928 sq m (10,000 sq ft) array, its design, and a full-scale demonstration of one quadrant (232 sq m (2500 sq ft)) deployed in a one-g field are described

Strong irradiation of protostellar cores in Corona Australis

The importance of the physical environment in the evolution of newly formed low-mass stars remains an open question. In particular, radiation from nearby more massive stars may affect both the physical and chemical structure of these kinds of young stars. Aims: To constrain the physical characteristics of a group of embedded low-mass protostars in Corona Australis in the vicinity of the young luminous Herbig Be star R CrA. Methods: Millimetre wavelength maps of molecular line and continuum emission towards the low-mass star forming region IRS7 near R CrA from the SMA and APEX are presented. The maps show the distribution of 18 lines from 7 species (H2CO, CH3OH, HC3N, c-C3H2, HCN, CN and SiO) on scales from 3" to 60" (400-8000 AU). Using a set of H2CO lines, we estimate the temperatures and column densities in the region using LTE and non-LTE methods. The results are compared with 1-D radiative transfer modelling of the protostellar cores. These models constrain which properties of the central source, envelope, and environment can give rise to the observed line and continuum emission. Results: Most of the H2CO emission from the regions emerges from two elongated narrow ridges dominating the emission picked up in both interferometric and single-dish measurements. The temperatures inferred from the H2CO lines are no less than ~30 K and more likely 50-60 K, and the line emission peaks are offset by ~2500 AU from the location of the embedded protostars. The temperatures can not be explained by the heating from the young stellar objects themselves. Irradiation by the nearby Herbig Be star R CrA could, however, explain the high temperatures. The elevated temperatures can in turn impact the physical and chemical characteristics of protostars and lead to enhanced abundances of typical tracers of photon dominated regions seen in single-dish line surveys of embedded protostars in the region.Comment: Accepted for publication in A&A; 21 pages, 28 figures; Added footnote in Section 2.

Paper Session II-B - The Pegasus Air-Launched Space Booster

The Pegasus Air-Launched Space Booster is an innovative new space launch vehicle now under full-scale development in a privately-funded joint venture by OSC and .Hercules Aerospace Company. Pegasus is a three-stage, solid-propellant, inertially-guided, all-composite winged vehicle that is launched at an altitude of 40,000 ft from its carrier aircraft. The 41,000 Ib vehicle can deliver payloads as massive as 900 Ib to low earth orbit. This status report on the Pegasus development program first details the \u27advantages of the airborne launch concept, then describes the design and performance of the Pegasus vehicle, and concludes with a review of the progress of the program from its conception in April 1987 through January 1989. First launch of Pegasus is scheduled for 31 July 1989 as a launch servipe under contract to the Defense Advanced Research Projects Agency. The second DARPA flight is scheduled for 15 September 1989

Macro Mineral Concentrations of Five Contrasting Temperate Grassland Species Grown in Pure Stands or Mixtures

Mixtures of grassland species often results in over-yielding (Finn et al., 2013). This may be due to complementarity in traits above- and below-ground. Here I report the concentrations of macro minerals in five grassland species grown as pure stands or in mixtures in a field fertilized with moderate amounts of nitrogen (N)

Externally heated protostellar cores in the Ophiuchus star-forming region

We present APEX 218 GHz observations of molecular emission in a complete sample of embedded protostars in the Ophiuchus star-forming region. To study the physical properties of the cores, we calculate H$_2$CO and c-C$_3$H$_2$ rotational temperatures, both of which are good tracers of the kinetic temperature of the molecular gas. We find that the H$_2$CO temperatures range between 16 K and 124 K, with the highest H$_2$CO temperatures toward the hot corino source IRAS 16293-2422 (69-124 K) and the sources in the $\rho$ Oph A cloud (23-49 K) located close to the luminous Herbig Be star S 1, which externally irradiates the $\rho$ Oph A cores. On the other hand, the c-C$_3$H$_2$ rotational temperature is consistently low (7-17 K) in all sources. Our results indicate that the c-C$_3$H$_2$ emission is primarily tracing more shielded parts of the envelope whereas the H$_2$CO emission (at the angular scale of the APEX beam; 3600 au in Ophiuchus) mainly traces the outer irradiated envelopes, apart from in IRAS 16293-2422, where the hot corino emission dominates. In some sources, a secondary velocity component is also seen, possibly tracing the molecular outflow.Comment: 19 pages, 9 figures, accepted for publication in Ap

N-ROSS: The dynamics and control issues

The Navy Remote Ocean Sensing System (N-ROSS) Dynamic Stability Study team concluded that the frozen April 1985 design was viable and contained no show stoppers, although it was also clear from the study results that the configuration required further optimization. While the frozen N-ROSS configuration used has since been superceded, and the vehicle is now under competitive procurement, several other results remain from the study that will have lasting value to the N-ROSS program. The importance of constructing an integrated simulation, to serve as a design and verification aid, has been clearly established. The two team approach to the study afforded the Navy a higher degree of confidence in the results than could have been accomplished by a single simulation, and the approach led to results that highlighted subtleties in the model and simulation development that surely would have been overlookded without the benefit of an independent companion simulation with which to compare it