1,190 research outputs found
Contestation and reconstruction: natural capital and post-conflict development in borderland regions
Though often remote and underdeveloped, borderlands are contested territories. The incorporation of borderlands into the post-conflict state highlights many important land-related paradigms, including the conversion of natural resources for economic, political, and civic purposes. This article explores the relationship between the natural resources of borderlands and their post-conflict development, management, and sustainability. Based on case study data and secondary material drawn from Croatia and Cyprus, the paper seeks to establish how the interplay of cross-border, national, and sub-national interests in post-conflict settings may contribute to the creation of new opportunities for economic development and the reconstruction of borderlands. It considers how the exploitation of natural resources may advance the agendas for the political development and incorporation of previous sites of contestation; and equally how their incorporation may constrain policies of sustainability, potentially giving rise to new conflicts. The paper sheds light on issues such as: the conversion of borderland natural capital to political capital as post-conflict states assert sovereignty claims and consolidate territorial identity; the ways in which the non-monetary value of natural capital is reconceived as commercial use value in post-conflict reconstruction; and the involvement of non-state actors and civil society in promoting environmental agendas, often as a counterbalance to state power
High resolution CO images of Seyfert Galaxies
The CO (J = 1-0) emission of three Seyfert galaxies, NGC 3227, NGC 7469, and NGC 5033 was imaged. The CO emission in NGC 3227 and NGC 7469 appears as compact structures centered on the active nuclei, containing substantial fractions of the single-dish flux. In NGC 3227, 10 percent of the CO flux detected by the interferometer is contained within the ionized narrow-line region. The unresolved molecular gas concentrations in the nucleus of NGC 3227 imply a CO mass of 65 million solar masses concentrated within a diameter less than 50 pc. The CO emission in NGC 5033 is not detected at this resolution, implying a CO structure size of 20 to 60 arcsec. Continuum emission at 2.7 mm is not detected in any of the three galaxies. In the center of NGC 7469, the H2 mass is comparable to the dynamical mass. Kinematic studies of the detected gas reveal a rotational motion of the gas in NGC 3227 and NGC 7469, allowing identification of the gas in NGC 7469 with a nuclear starburst. These data are consistent with the idea that interactions between galaxies cause gas to concentrate in their nuclei thereby feeding starburst and Seyfert activity
Turbulence, Feedback, and Slow Star Formation
One of the outstanding puzzles about star formation is why it proceeds so
slowly. Giant molecular clouds convert only a few percent of their gas into
stars per free-fall time, and recent observations show that this low star
formation rate is essentially constant over a range of scales from individual
cluster-forming molecular clumps in the Milky Way to entire starburst galaxies.
This striking result is perhaps the most basic fact that any theory of star
formation must explain. I argue that a model in which star formation occurs in
virialized structures at a rate regulated by supersonic turbulence can explain
this observation. The turbulence in turn is driven by star formation feedback,
which injects energy to offset radiation from isothermal shocks and keeps
star-forming structures from wandering too far from virial balance. This model
is able to reproduce observational results covering a wide range of scales,
from the formation times of young clusters to the extragalactic IR-HCN
correlation, and makes additional quantitative predictions that will be
testable in the next few years.Comment: 4 pages, 2 figures, CUP conference format. To be published in "IAU
Symposium 237: Triggered Star Formation in a Turbulent ISM", eds. B.
Elmegreen & J. Palou
Interaction of laser generated ultrasonic waves with wedge-shaped samples
Wedge-shaped samples can be used as a model of acoustic interactions with samples ranging from ocean wedges, to angled defects such as rolling contact fatigue, to thickness measurements of samples with non-parallel faces. We present work on laser generated ultrasonic waves on metal samples; one can measure the dominant Rayleigh-wave mode, but longitudinal and shear waves are also generated. We present calculations, models, and measurements giving the dependence of the arrival times and amplitudes of these modes on the wedge apex angle and the separation of generation and detection points, and hence give a measure of the wedge characteristics
The Atomic to Molecular Transition in Galaxies. II: HI and H_2 Column Densities
Gas in galactic disks is collected by gravitational instabilities into giant
atomic-molecular complexes, but only the inner, molecular parts of these
structures are able to collapse to form stars. Determining what controls the
ratio of atomic to molecular hydrogen in complexes is therefore a significant
problem in star formation and galactic evolution. In this paper we use the
model of H_2 formation, dissociation, and shielding developed in the previous
paper in this series to make theoretical predictions for atomic to molecular
ratios as a function of galactic properties. We find that the molecular
fraction in a galaxy is determined primarily by its column density and
secondarily by its metallicity, and is to good approximation independent of the
strength of the interstellar radiation field. We show that the column of atomic
hydrogen required to shield a molecular region against dissociation is ~10 Msun
pc^-2 at solar metallicity. We compare our model to data from recent surveys of
the Milky Way and of nearby galaxies, and show that the both the primary
dependence of molecular fraction on column density and the secondary dependence
on metallicity that we predict are in good agreement with observed galaxy
properties.Comment: Accepted to ApJ. 22 pages, 13 figures, emulateapj format. This
version corrects a minor error in the binning procedure in section 4.1.2. The
remainder of the paper is unchange
A Magellanic Origin for the Warp of the Galaxy
We show that a Magellanic Cloud origin for the warp of the Milky Way can
explain most quantitative features of the outer HI layer recently identified by
Levine, Blitz & Heiles (2005). We construct a model similar to that of Weinberg
(1998) that produces distortions in the dark matter halo, and we calculate the
combined effect of these dark-halo distortions and the direct tidal forcing by
the Magellanic Clouds on the disk warp in the linear regime. The interaction of
the dark matter halo with the disk and resonances between the orbit of the
Clouds and the disk account for the large amplitudes observed for the vertical
m=0,1,2 harmonics. The observations lead to six constraints on warp forcing
mechanisms and our model reasonably approximates all six. The disk is shown to
be very dynamic, constantly changing its shape as the Clouds proceed along
their orbit. We discuss the challenges to MOND placed by the observations.Comment: 4 pages, 3 figures, submitted to ApJ Letters. Additional graphics, 3d
visualizations and movies available at
http://www.astro.umass.edu/~weinberg/lm
Gas Rich Dwarf Spheroidals
We present evidence that nearly half of the dwarf spheroidal galaxies (dSph
and dSph/dIrr) in the Local Group are associated with large reservoirs of
atomic gas, in some cases larger than the stellar mass. The gas is sometimes
found at large distance (~10 kpc) from the center of a galaxy and is not
necessarily centered on it. Similarly large quantities of ionized gas could be
hidden in these systems as well. The properties of some of the gas reservoirs
are similar to the median properties of the High-Velocity Clouds (HVCs); two of
the HI reservoirs are catalogued HVCs. The association of the HI with the dwarf
spheroidals might thus provide a link between the HVCs and stars. We show that
the HI content of the Local Group dSphs and dIrrs exhibits a sharp decline if
the galaxy is within 250 kpc of either the Milky Way or M31. This can be
explained if both galaxies have a sufficiently massive x-ray emitting halo that
produces ram-pressure stripping if a dwarf ventures too close to either giant
spiral. We also investigate tidal stripping of the dwarf galaxies and find that
although it may play a role, it cannot explain the apparent total absence of
neutral gas in most dSph galaxies at distances less than 250 kpc. For the
derived mean density of the hot gas, n_0 = 2.5e-5 cm^-2, ram-pressure stripping
is found to be more than an order of magnitude more effective in removing the
gas from the dSph galaxies. The hot halo, with an inferred mass of 1e10 solar
masses, may represent a reservoir of ~1000 destroyed dwarf systems, either HVCs
or true dwarf galaxies similar to those we observe now.Comment: AASTex preprint style, 27 pages including 12 figures. Submitted to
ApJ. See also http://astro.berkeley.edu/~robisha
The Role of a Hot Gas Environment on the Evolution of Galaxies
Most spiral galaxies are found in galaxy groups with low velocity
dispersions; most E/S0 galaxies are found in galaxy groups with relatively high
velocity dispersions. The mass of the hot gas we can observe in the E/S0 groups
via their thermal X-ray emission is, on average, as much as the baryonic mass
of the galaxies in these groups. By comparison, galaxy clusters have as much or
more hot gas than stellar mass. Hot gas in S-rich groups, however, is of low
enough temperature for its X-ray emission to suffer heavy absorption due to
Galactic HI and related observational effects, and hence is hard to detect. We
postulate that such lower temperature hot gas does exist in low velocity
dispersion, S-rich groups, and explore the consequences of this assumption. For
a wide range of metallicity and density, hot gas in S-rich groups can cool in
far less than a Hubble time. If such gas exists and can cool, especially when
interacting with HI in existing galaxies, then it can help link together a
number of disparate observations, both Galactic and extragalactic, that are
otherwise difficult to understand.Comment: 16 pages with one figure. ApJ Letters, in pres
Gender and displacement in Jaffna, Sri Lanka
This report presents the preliminary results of a household survey of internally displaced persons (IDPs) in Jaffna District in Northern Province, one of the areas that still has a large IDP population. The main focus of this survey conducted in October 2020 employing Covid-19 safety protocols was to examine the gendered experiences arising from protracted displacements spanning over three decades. The survey covered 220 households (182 male-headed and 38 female-headed), which accounts for 54.3 per cent of the total IDP households in the Jaffna District.
Among other topics, the survey gathered data on the respondents’ current living conditions, finances, asset ownership, safety and security concerns, access to services, social networks and relationship with other IDPs and the host community, and water, sanitation and hygiene issues they face. It also gathered data on the respondents’ pre-displacement experiences to compare that with their current lives, in order to examine the role of displacement in gendered issues they face
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