6,835 research outputs found
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 HCO and c-CH
rotational temperatures, both of which are good tracers of the kinetic
temperature of the molecular gas. We find that the HCO temperatures range
between 16 K and 124 K, with the highest HCO temperatures toward the hot
corino source IRAS 16293-2422 (69-124 K) and the sources in the Oph A
cloud (23-49 K) located close to the luminous Herbig Be star S 1, which
externally irradiates the Oph A cores. On the other hand, the
c-CH rotational temperature is consistently low (7-17 K) in all
sources. Our results indicate that the c-CH emission is primarily
tracing more shielded parts of the envelope whereas the HCO 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
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