341 research outputs found
Coal-derived rates of atmospheric dust deposition during the Permian
Despite widespread evidence for atmospheric dust deposition prior to the Quaternary, quantitative rate data remains sparse. As dust influences both climate and biological productivity, the absence of quantitative dust data limits the comprehensiveness of models of pre-Quaternary climate and biogeochemical cycles. Here, we propose that inorganic matter contained in coal primarily records atmospheric dust deposition. To test this, we use the average concentration of inorganic matter in Permian coal to map global patterns and deposition rates of atmospheric dust over Pangea. The dust accumulation rate is calculated assuming Permian peat carbon accumulation rates in temperate climates were similar to Holocene rates and accounting for the loss of carbon during coalification. Coal-derived rates vary from 0.02 to 25 g m− 2 year− 1, values that fall within the present-day global range. A well-constrained East–West pattern of dust deposition corresponding to expected palaeoclimate gradients extends across Gondwana with maximum dust deposition rates occurring close to arid regions. A similar pattern is partially defined over the northern hemisphere. Patterns are consistent with the presence of two large global dust plumes centred on the tropics. The spatial patterns of dust deposition were also compared to dust cycle simulations for the Permian made with the Community Climate System Model version 3 (CCSM3). Key differences between the simulations and the coal data are the lack of evidence for an Antarctic dust source, higher than expected dust deposition over N and S China and greater dust deposition rates over Western Gondwana. This new coal-based dust accumulation rate data expands the pre-Neogene quantitative record of atmospheric dust and can help to inform and validate models of global circulation and biogeochemical cycles over the past 350 Myr
NGC 3576 and NGC 3603: Two Luminous Southern HII Regions Observed at High Resolution with the Australia Telescope Compact Array
NGC 3576 (G291.28-0.71; l=291.3o, b=-0.7o) and NGC 3603 (G291.58-0.43;
l=291.6o, b=-0.5o) are optically visible, luminous HII regions located at
distances of 3.0 kpc and 6.1 kpc, respectively. We present 3.4 cm Australian
Telescope Compact Array (ATCA) observations of these two sources in the
continuum and the H90a, He90a, C90a and H113b recombination lines with an
angular resolution of 7" and a velocity resolution of 2.6 km/s. All four
recombination lines are detected in the integrated profiles of the two sources.
Broad radio recombination lines are detected in both NGC 3576 (DV_{FWHM}>= 50
km/s) and NGC 3603 (DV_{FWHM}>=70 km/s). In NGC 3576 a prominent N-S velocity
gradient (~30 km/s/pc) is observed, and a clear temperature gradient (6000 K to
8000 K) is found from east to west, consistent with a known IR color gradient
in the source. In NGC 3603, the H90a, He90a and the H113b lines are detected
from 13 individual sources. The Y^+ (He/H) ratios in the two sources range from
0.08+/-0.04 to 0.26+/-0.10. We compare the morphology and kinematics of the
ionized gas at 3.4 cm with the distribution of stars, 10 micron emission and
H_2O, OH, and CH_3OH maser emission. These comparisons suggest that both NGC
3576 and NGC 3603 have undergone sequential star formation.Comment: 24 pages, 12 Postscript figure
The Giant Pillars of the Carina Nebula
Results are presented from a multi-wavelength study of the giant pillars
within the Carina Nebula. Using near-IR data from 2MASS, mid-IR data from MSX,
843MHz radio continuum maps from the MOST, and molecular line and continuum
observations from the SEST, we investigate the nature of the pillars and search
for evidence of ongoing star formation within them. Photodissociation regions
(PDRs) exist across the whole nebula and trace the giant pillars, as well as
many ridges, filaments, and condensations (Av > 7 mag). Morphological
similarities between emission features at 21um and 843MHz adjacent to the PDRs,
suggests that the molecular material has been carved by the intense stellar
winds and UV radiation from the nearby massive stars. In addition, star forming
cores are found at the tips of several of the pillars. Using a stellar density
distribution, several candidate embedded clusters are also found. One is
clearly seen in the 2MASS images and is located within a dense core
(G287.84-0.82). A search for massive young stellar objects and compact HII
regions using mid-IR colour criteria, reveal twelve candidates across the
complex. Grey-body fits to SEDs for four of these objects are suggestive of
OB-stars. We find that massive star formation in the Carina Nebula is occurring
across the whole complex and confirm it has been continuous over the past 3
Myrs.Comment: 14 pages, 10 figures (low resolution), accepted by A&
Oregon 2100: projected climatic and ecological changes
Greenhouse climatic warming is underway and exacerbated by human activities. Future outcomes of these processes can be projected using computer models checked against climatic changes during comparable past atmospheric compositions. This study gives concise quantitative predictions for future climate, landscapes, soils, vegetation, and marine and terrestrial animals of Oregon. Fossil fuel burning and other human activities by the year 2100 are projected to yield atmospheric CO2 levels of about 600-850 ppm (SRES A1B and B1), well above current levels of 400 ppm and preindustrial levels of 280 ppm. Such a greenhouse climate was last recorded in Oregon during the middle Miocene, some 16 million years ago. Oregon’s future may be guided by fossil records of the middle Miocene, as well as ongoing studies on the environmental tolerances of Oregon plants and animals, and experiments on the biological effects of global warming. As carbon dioxide levels increase, Oregon’s climate will move toward warm temperate, humid in the west and semiarid to subhumid to the east, with increased summer and winter drought in the west. Western Oregon lowlands will become less suitable for temperate fruits and nuts and Pinot Noir grapes, but its hills will remain a productive softwood forest resource. Improved pasture and winter wheat crops will become more widespread in eastern Oregon. Tsunamis and stronger storms will exacerbate marine erosion along the Oregon Coast, with significant damage to coastal properties and cultural resources
Photodissociation regions and star formation in the Carina Nebula
We have obtained wide-field thermal infrared (IR) images of the Carina
Nebula, using the SPIREX/Abu telescope at the South Pole. Emission from
poly-cyclic aromatic hydrocarbons (PAHs) at 3.29um, a tracer of
photodissociation regions (PDRs), reveals many interesting well defined clumps
and diffuse regions throughout the complex. Near-IR images (1--2um), along with
images from the Midcourse Space Experiment (MSX) satellite (8--21um) were
incorporated to study the interactions between the young stars and the
surrounding molecular cloud in more detail. Two new PAH emission clumps have
been identified in the Keyhole Nebula and were mapped in 12CO(2--1) and (1--0)
using the SEST. Analysis of their physical properties reveals they are dense
molecular clumps, externally heated with PDRs on their surfaces and supported
by external pressure in a similar manner to the other clumps in the region. A
previously identified externally heated globule containing IRAS 10430-5931 in
the southern molecular cloud, shows strong 3.29-, 8- and 21-um emission, the
spectral energy distribution (SED) revealing the location of an ultra-compact
(UC) HII region. The northern part of the nebula is complicated, with PAH
emission inter-mixed with mid-IR dust continuum emission. Several point sources
are located here and through a two-component black-body fit to their SEDs, we
have identified 3 possible UC HII regions as well as a young star surrounded by
a circumstellar disc. This implies that star formation in this region is
on-going and not halted by the intense radiation from the surrounding young
massive stars.Comment: 14 pages, 12 figures. Accepted by MNRAS. Higher resolution figures
available at http://www.phys.unsw.edu.au/~jmr/papers.htm
Detection of the 205 um [NII] Line from the Carina Nebula
We report the first detection of the 205 um 3P1 - 3P0 [NII] line from a
ground-based observatory using a direct detection spectrometer. The line was
detected from the Carina star formation region using the South Pole Imaging
Fabry-Perot Interferometer (SPIFI) on the Antarctic Submillimeter Telescope and
Remote Observatory (AST/RO) at South Pole. The [NII] 205 um line strength
indicates a low-density (n ~ 32 cm^-3 ionized medium, similar to the
low-density ionized halo reported previously in its [OIII] 52 and 88 um line
emission. When compared with the ISO [CII] observations of this region, we find
that ~27% of the [CII] line emission arises from this low-density ionized gas,
but the large majority ~ 73% of the observed [CII] line emission arises from
the neutral interstellar medium. This result supports and underpins prior
conclusions that most of the observed [CII] 158 um line emission from Galactic
and extragalactic sources arises from the warm, dense photodissociated surfaces
of molecular clouds. The detection of the [NII] line demonstrates the utility
of Antarctic sites for THz spectroscopy.Comment: 8 pages, 2 figures. To appear in the Astrophysical Journal Letter
Revisiting 2D Numerical Models for the 19th century outbursts of Carinae
We present here new results of two-dimensional hydrodynamical simulations of
the eruptive events of the 1840s (the great) and the 1890s (the minor)
eruptions suffered by the massive star Car. The two bipolar nebulae
commonly known as the Homunculus and the little Homunculus were formed from the
interaction of these eruptive events with the underlying stellar wind. As in
previous work (Gonzalez et al. 2004a, 2004b), we assume here an interacting,
nonspherical multiple-phase wind scenario to explain the shape and the
kinematics of both Homunculi, but adopt a more realistic parametrization of the
phases of the wind. During the 1890s eruptive event, the outflow speed {\it
decreased} for a short period of time. This fact suggests that the little
Homunculus is formed when the eruption ends, from the impact of the
post-outburst Car wind (that follows the 1890s event) with the eruptive
flow (rather than by the collision of the eruptive flow with the pre-outburst
wind, as claimed in previous models; Gonzalez et al. 2004a, 2004b). Our
simulations reproduce quite well the shape and the observed expansion speed of
the large Homunculus. The little Homunculus (which is embedded within the large
Homunculus) becomes Rayleigh-Taylor unstable and develop filamentary structures
that resembles the spatial features observed in the polar caps. In addition, we
find that the interior cavity between the two Homunculi is partially filled by
material that is expelled during the decades following the great eruption. This
result may be connected with the observed double-shell structure in the polar
lobes of the Car nebula. Finally, as in previous work, we find the
formation of tenuous, equatorial, high-speed features that seem to be related
to the observed equatorial skirt of Car.Comment: accepted for publication in MNRA
The Earliest Post-Paleozoic Freshwater Bivalves Preserved in Coprolites from the Karoo Basin, South Africa
Background: Several clades of bivalve molluscs have invaded freshwaters at various times throughout Phanerozoic history. The most successful freshwater clade in the modern world is the Unionoida. Unionoids arose in the Triassic Period, sometime after the major extinction event at the End-Permian boundary and are now widely distributed across all continents except Antarctica. Until now, no freshwater bivalves of any kind were known to exist in the Early Triassic. Principal Findings: Here we report on a faunule of two small freshwater bivalve species preserved in vertebrate coprolites from the Olenekian (Lower Triassic) of the Burgersdorp Formation of the Karoo Basin, South Africa. Positive identification of these bivalves is not possible due to the limited material. Nevertheless they do show similarities with Unionoida although they fall below the size range of extant unionoids. Phylogenetic analysis is not possible with such limited material and consequently the assignment remains somewhat speculative. Conclusions: Bivalve molluscs re-invaded freshwaters soon after the End-Permian extinction event, during the earliest part of the recovery phase during the Olenekian Stage of the Early Triassic. If the specimens do represent unionoids then these Early Triassic examples may be an example of the Lilliput effect. Since the oldest incontrovertible freshwater unionoids are also from sub-Saharan Africa, it is possible that this subcontinent hosted the initial freshwater radiation of the Unionoida. This find also demonstrates the importance of coprolites as microenvironments of exceptional preservation that contai
Anomalous X-ray Pulsars and Soft Gamma-Ray Repeaters in supernova remnants
Important constraints on the properties of the Anomalous X-ray Pulsars (AXPs)
and Soft Gamma-Ray Repeaters (SGRs) can be provided by their associations with
supernova remnants (SNRs). We have made a radio search for SNRs towards the
AXPs RX J170849-400910 and 4U 0142+61 - we find that the former lies near a
possible new SNR with which it is unlikely to be physically associated, but see
no SNR in the vicinity of the latter. We review all claimed pairings between
AXPs and SNRs; the three convincing associations imply that AXPs are young (<
10 000 yr) neutron stars with low projected space velocities (< 500 km/s).
Contrary to previous claims, we find no evidence that the density of the
ambient medium around AXPs is higher than that in the vicinity of radio
pulsars. Furthermore, the non-detection of radio emission from AXPs does not
imply that these sources are radio-silent. We also review claimed associations
between SGRs and SNRs. We find none of these associations to be convincing,
consistent with a scenario in which SGRs and AXPs are both populations of
high-field neutron stars ("magnetars") but in which the SGRs are an older or
longer-lived group of objects than are the AXPs. If the SGR/SNR associations
are shown to be valid, then SGRs must be high-velocity objects and most likely
represent a different class of source to the AXPs.Comment: 13 pages, 3 embedded EPS figures. Minor alterations following
referee's report; no significant changes. Accepted to Ap
- …