5,292 research outputs found
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.
A survey of HC_3N in extragalactic sources: Is HC_3N a tracer of activity in ULIRGs?
Context. HC_3N is a molecule that is mainly associated with Galactic star-forming regions, but it has also been detected in extragalactic environments.
Aims. To present the first extragalactic survey of HC_3N, when combining earlier data from the literature with six new single-dish detections, and to compare HC_3N with other molecular tracers (HCN, HNC), as well as other properties (silicate absorption strength, IR flux density ratios, C_(II) flux, and megamaser activity).
Methods. We present mm IRAM 30 m, OSO 20 m, and SEST observations of HC_3N rotational lines (mainly the J = 10â9 transition) and of the J = 1â0 transitions of HCN and HNC. Our combined HC_3N data account for 13 galaxies (excluding the upper limits reported for the non-detections), while we have HCN and HNC data for more than 20 galaxies.
Results. A preliminary definition âHC_3N-luminous galaxyâ is made based upon the HC_3N/HCN ratio. Most (~80%) HC_3N-luminous galaxies seem to be deeply obscured galaxies and (U)LIRGs. A majority (~60% or more) of the HC3N-luminous galaxies in the sample present OH mega- or strong kilomaser activity. A possible explanation is that both HC_3N and OH megamasers need warm dust for their excitation. Alternatively, the dust that excites the OH megamaser offers protection against UV destruction of HC_3N. A high silicate absorption strength is also found in several of the HC_3N-luminous objects, which may help the HC3N to survive. Finally, we find that a high HC_3N/HCN ratio is related to a high dust temperature and a low C_(II) flux
Robust autoresonant excitation in the plasma beat-wave accelerator: a theoretical study
A modified version of the Plasma Beat-Wave Accelerator scheme is introduced
and analyzed, which is based on autoresonant phase-locking of the nonlinear
Langmuir wave to the slowly chirped beat frequency of the driving lasers via
adiabatic passage through resonance. This new scheme is designed to overcome
some of the well-known limitations of previous approaches, namely relativistic
detuning and nonlinear modulation or other non-uniformity or non-stationarity
in the driven Langmuir wave amplitude, and sensitivity to frequency mismatch
due to measurement uncertainties and density fluctuations and inhomogeneities
The uniting of Europe and the foundation of EU studies: revisiting the neofunctionalism of Ernst B. Haas
This article suggests that the neofunctionalist theoretical legacy left by Ernst B. Haas is somewhat richer and more prescient than many contemporary discussants allow. The article develops an argument for routine and detailed re-reading of the corpus of neofunctionalist work (and that of Haas in particular), not only to disabuse contemporary students and scholars of the normally static and stylized reading that discussion of the theory provokes, but also to suggest that the conceptual repertoire of neofunctionalism is able to speak directly to current EU studies and comparative regionalism. Neofunctionalism is situated in its social scientific context before the theory's supposed erroneous reliance on the concept of 'spillover' is discussed critically. A case is then made for viewing Haas's neofunctionalism as a dynamic theory that not only corresponded to established social scientific norms, but did so in ways that were consistent with disciplinary openness and pluralism
Warm gas towards young stellar objects in Corona Australis - Herschel/PACS observations from the DIGIT key programme
The effects of external irradiation on the chemistry and physics in the
protostellar envelope around low-mass young stellar objects are poorly
understood. The Corona Australis star-forming region contains the R CrA dark
cloud, comprising several low-mass protostellar cores irradiated by an
intermediate-mass young star. We study the effects on the warm gas and dust in
a group of low-mass young stellar objects from the irradiation by the young
luminous Herbig Be star R CrA. Herschel/PACS far-infrared datacubes of two
low-mass star-forming regions in the R CrA dark cloud are presented. The
distribution of CO, OH, H2O, [C II], [O I], and continuum emission is
investigated. We have developed a deconvolution algorithm which we use to
deconvolve the maps, separating the point-source emission from the extended
emission. We also construct rotational diagrams of the molecular species. By
deconvolution of the Herschel data, we find large-scale (several thousand AU)
dust continuum and spectral line emission not associated with the point
sources. Similar rotational temperatures are found for the warm CO (
K), hot CO ( K), OH ( K), and H2O ( K) emission,
respectively, in the point sources and the extended emission. The rotational
temperatures are also similar to what is found in other more isolated cores.
The extended dust continuum emission is found in two ridges similar in extent
and temperature to molecular mm emission, indicative of external heating from
the Herbig Be star R CrA. Our results show that a nearby luminous star does not
increase the molecular excitation temperatures in the warm gas around a young
stellar object (YSO). However, the emission from photodissociation products of
H2O, such as OH and O, is enhanced in the warm gas associated with these
protostars and their surroundings compared to similar objects not suffering
from external irradiation.Comment: 37 pages, accepted for publication in A&
One step multiderivative methods for first order ordinary differential equations
A family of one-step multiderivative methods based on Padé approximants to the exponential function is developed.
The methods are extrapolated and analysed for use in PECE mode.
Error constants and stability intervals are calculated and the combinations compared with well known linear multi-step combinations and combinations using high accuracy Newton-Cotes quadrature formulas as correctors.
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Water-ice driven activity on Main-Belt Comet P/2010 A2 (LINEAR) ?
The dust ejecta of Main-Belt Comet P/2010 A2 (LINEAR) have been observed with
several telescopes at the at the Observatorio del Roque de los Muchachos on La
Palma, Spain. Application of an inverse dust tail Monte Carlo method to the
images of the dust ejecta from the object indicates that a sustained, likely
water-ice driven, activity over some eight months is the mechanism responsible
for the formation of the observed tail. The total amount of dust released is
estimated to be 5E7 kg, which represents about 0.3% of the nucleus mass. While
the event could have been triggered by a collision, this cannot be decided from
the currently available data.Comment: Accepted for ApJ Letter
Evidence for a chemically differentiated outflow in Mrk 231
Aims: Our goal is to study the chemical composition of the outflows of active
galactic nuclei and starburst galaxies.
Methods: We obtained high-resolution interferometric observations of HCN and
HCO and of the ultraluminous infrared
galaxy Mrk~231 with the IRAM Plateau de Bure Interferometer. We also use
previously published observations of HCN and HCO and
, and HNC in the same source.
Results: In the line wings of the HCN, HCO, and HNC emission, we find
that these three molecular species exhibit features at distinct velocities
which differ between the species. The features are not consistent with emission
lines of other molecular species. Through radiative transfer modelling of the
HCN and HCO outflow emission we find an average abundance ratio
. Assuming a clumpy outflow,
modelling of the HCN and HCO emission produces strongly inconsistent
outflow masses.
Conclusions: Both the anti-correlated outflow features of HCN and HCO and
the different outflow masses calculated from the radiative transfer models of
the HCN and HCO emission suggest that the outflow is chemically
differentiated. The separation between HCN and HCO could be an indicator of
shock fronts present in the outflow, since the HCN/HCO ratio is expected to
be elevated in shocked regions. Our result shows that studies of the chemistry
in large-scale galactic outflows can be used to better understand the physical
properties of these outflows and their effects on the interstellar medium (ISM)
in the galaxy.Comment: 12 pages, 8 figures, accepted for publication in A&
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