X-ray Emission from the Pre-Main Sequence Systems FU Orionis and T Tauri

We present new results from recent X-ray observations of the accreting pre-main sequence stars FU Orionis and T Tauri. XMM-Newton observations of the close binary system FU Ori reveal an unusual X-ray spectrum consisting of a cool moderately-absorbed component and a hot component viewed through much higher absorption. The two components thus originate in physically distinct regions. The double absorption spectrum is qualitatively different than observed in typical coronal sources and may signal either non-coronal emission or separate unresolved X-ray contributions from more than one star in the system. High-resolution Chandra imaging of the T Tau triple system shows that its X-ray emission is dominated by the optically-revealed northern component T Tau N. X-ray spectra of T Tau obtained with XMM can be acceptably fitted with a moderately absorbed two-temperature thermal plasma model. Its spectral properties are similar to those seen in coronal X-ray sources.     

Probing the dark ages with the Square Kilometer Array

The epoch of reionization (EoR) sets a fundamental benchmark in cosmic structure formation, corresponding to the formation of the first luminous objects that act to ionize the neutral intergalactic medium (IGM). Recent observations at near-IR and radio wavelengths imply that we are finally probing into this key epoch of galaxy formation at z 6. The Square Kilometer Array (SKA) will provide critical insight into the EoR, in a number of ways. First, the ability of the SKA to image the neutral IGM in 21-cm emission is a truly unique probe of the process of reionization, and is recognized as the next necessary and fundamental step in our study of the evolution of large scale structure and cosmic reionization. Second, study of HI 21-cm absorption toward the first radio loud objects probes small to intermediate scale structure in the neutral ‘cosmic web’, as well as HI in the first collapsed structures (proto-disks and mini-halos). And third, the incomparable sensitivity of the SKA allows for the study of the molecular gas, dust, and star formation activity in the first galaxies, as well as the radio continuum emission from the first accreting massive black holes. Such objects will be obscured at optical wavelengths due to absorption by the neutral IGM.     

Constraining Sources of Organic Matter to Tropical Coastal Sediments: Consideration of Nontraditional End-members

Molar organic carbon to total nitrogen to organic phosphorus (OC:TN:OP) ratios are used in tandem with carbon isotopic values to constrain sources of organic matter (OM) to marine sediments in a tropical coastal embayment. Analysis of end-members specific to the study site indicates that the bulk OM pool cannot be modeled as a simple mixture of two end-members (terrestrial vs. marine OM), but rather reflects a more complex, multicomponent mixture. Mangrove, coral reef ecosystems, and bacterial biomass contribute OM to tropical coastal marine sediments that is compositionally distinct from traditional marine and terrestrial end-members and thus preclude the application of a classical two end-member mixing model of the sort that has been used traditionally in sediments from temperate environments. A survey of elemental ratios and carbon isotopic values of potential OM end-members reported in the literature, as well as depth profiles before and after whole-core incubation experiments conducted as part of this study, were used to evaluate the strength of OC:TN versus OC:OP ratios as OM source indices. Our study suggests that OC:TN ratios are a weaker indicator of OM source than OC:OP ratios, because: (1) the more restricted dynamic range of OC:TN ratios prevents clear distinction of terrestrial-from marine-derived OM, and (2) post-depositional changes in OC:TN ratios occur during diagenesis, obscuring the source signature of initially deposited OM. The fidelity of OM indices during early diagenesis underscores the importance of quantifying OP in sediments to assess sedimentary OM source.     

Uptake of palytoxin‐like compounds by shellfish fed Ostreopsis siamensis (Dinophyceae)

Abstract

Greenshell? mussels (Perna canaliculus Gmelin), scallops (Pecten novaezealandiae Reeve), and Pacific oysters (Crassostrea gigas Thunberg) were fed with a New Zealand strain of mass cultured Ostreopsis siamensis Schmidt (for 27 and 84 h and with 1.5 × 10⁶ or 8.6 × 10⁶ cells, respectively) under laboratory conditions. The microalgal cells contained 0.3 pg palytoxin equivalents cell^–1 (as determined by the haemolysis neutralisation assay (HNA) of Bignami (1993)) and extracts of these cells were toxic to mice after intraperitoneal injection. No palytoxin‐like material was detected either in the hepatopancreas or the muscle and roe of mussels fed O. siamensis. Oysters contained detectable amounts of toxin in hepatopancreas muscle, and roe while higher concentrations were present in the hepatopancreas of scallops. Extracts of control shellfish (tested biotoxin free and not fed O. siamensis) were toxic to mice, and there was no definitive evidence that feeding shellfish with O. siamensis at the levels employed in the present experiment increased the toxicity of shellfish tissue extracts to mice.     

Patch dynamics of soil biotic feedbacks in the Sonoran Desert

Soil fertility in arid ecosystems is spatially and temporally heterogeneous, due primarily to biotic feedbacks from perennial plants. While the “island of fertility” effect is well-established, little is known about the influence of plant functional characteristics on soil nutrients, or changes in nutrient levels following mortality or microsite succession. To assess these patterns, we studied a functionally diverse Sonoran Desert ecosystem in which all microsite state transitions were determined. The woody species (Ambrosia deltoidea, Larrea tridentata, Parkinsonia microphylla) significantly enhanced soil organic matter, nitrogen and phosphorous levels (referred to generally as fertility) to varying degrees. Effect sizes differed significantly among species but were surprisingly similar. However, following mortality, fertility remained constant beneath Ambrosia and increased significantly beneath decaying Parkinsonia, contrary to expected declines. These results suggest that nutrients are recycled within a microsite, resulting in similar pool sizes beneath live plants across species, regardless of morphological or phonological differences. Microsites occupied by cacti exhibited no differences from bare soil, indicating that cacti may erase islands of fertility. However, nitrate and phosphate levels spiked following mortality of the large cactus, Carnegiea gigantea. In general, fertility effects were correlated with morphological characteristics that should be applicable across most arid systems.     

An example of fingerprint detection of greenhouse climate change

As an example of the technique of fingerprint detection of greenhouse climate change, a multivariate signal or fingerprint of the enhanced greenhouse effect is defined using the zonal mean atmospheric temperature change as a function of height and latitude between equilibrium climate model simulations with control and doubled CO₂ concentrations. This signal is compared with observed atmospheric temperature variations over the period 1963 to 1988 from radiosonde-based global analyses. There is a significant increase of this greenhouse signal in the observational data over this period.These results must be treated with caution. Upper air data are available for a short period only, possibly too short to be able to resolve any real greenhouse climate change. The greenhouse fingerprint used in this study may not be unique to the enhanced greenhouse effect and may be due to other forcing mechanisms. However, it is shown that the patterns of atmospheric temperature change associated with uniform global increases of sea surface temperature, with El NinoSouthern Oscillation events and with decreases of stratospheric ozone concentrations individually are different from the greenhouse fingerprint used here.     

The evaluation of BATSE line candidates

We evaluated the significance of the line candidates identified by the visual search of burst spectra from BATSE's spectroscopy detectors. None of the candidates satisfy the detection criteria: anF-test probability less than 10^–4 for a feature in one detector and consistency among the detectors which viewed the burst. Most of the candidates are not very significant, and are likely to be fluctuations. Because of the expectation of finding absorption lines, the search was biased towards absorption features. We do not have a quantitative measure of the completeness of the search which would form the basis of a comparison with previous missions. Therefore a more objective computerized search has begun.     

Microwave radiometry and interferometry of Uranus

We present high-resolution interferometry of Uranus at 6 cm wavelength and single-dish observations of the disk-averaged brightness temperature, T_B, at 2.8 and 4.8 cm wavelength. The 1978 measurements of T_B of 228 ± 2,243 ± 9, and 259 ± 4 K at 2.8, 4.8, and 6 cm, respectively, support the finding of M. J. Klein and J. A. Turegano (1978, Astrophy. J.224, L31–L34) that the brightness temperature of Uranus has been rising. There is no evidence for radio emission from outside the visible disk at 6 cm. Radiation from a synchrotron radiation belt or from the Uranian rings is certainly less than 10% of the total radio flux. The interferometry shows a possible 55 ± 20 K difference in brightness temperature between the equator and the currently exposed pole. The pole appears to be ～275 K while the equator is ～220 K. However, a permanent gradient of this magnitude is insufficient to account for the rise in disk-averaged brightness by simple reorientation of Uranus' globe relative to our line of sight. The changing insolation probably triggers a redistribution of the trace constituent NH₃ which is responsible for the radio opacity. The NH₃ may be interacting strongly with H₂S on Uranus.