1,460 research outputs found
Chemical modeling of the L1498 and L1517B prestellar cores: CO and HCO+ depletion
Prestellar cores exhibit a strong chemical differentiation, which is mainly
caused by the freeze-out of molecules onto the grain surfaces. Understanding
this chemical structure is important, because molecular lines are often used as
probes to constrain the core physical properties. Here we present new
observations and analysis of the C18O (1-0) and H13CO+ (1-0) line emission in
the L1498 and L1517B prestellar cores, located in the Taurus-Auriga molecular
complex. We model these observations with a detailed chemistry network coupled
to a radiative transfer code. Our model successfully reproduces the observed
C18O (1-0) emission for a chemical age of a few 10^5 years. On the other hand,
the observed H13CO+ (1-0) is reproduced only if cosmic-ray desorption by
secondary photons is included, and if the grains have grown to a bigger size
than average ISM grains in the core interior. This grain growth is consistent
with the infrared scattered light ("coreshine") detected in these two objects,
and is found to increase the CO abundance in the core interior by about a
factor four. According to our model, CO is depleted by about 2-3 orders of
magnitude in the core center.Comment: Accepted for publication in A&
Star Formation and Substructure in Galaxy Clusters
We investigate the relationship between star formation (SF) and substructure
in a sample of 107 nearby galaxy clusters using data from the Sloan Digital Sky
Survey (SDSS). Several past studies of individual galaxy clusters have
suggested that cluster mergers enhance cluster SF, while others find no such
relationship. The SF fraction in multi-component clusters (0.228 +/- 0.007) is
higher than that in single-component clusters (0.175 +/- 0.016) for galaxies
with M^0.1_r < -20.5. In both single- and multi-component clusters, the
fraction of star-forming galaxies increases with clustercentric distance and
decreases with local galaxy number density, and multi-component clusters show a
higher SF fraction than single-component clusters at almost all clustercentric
distances and local densities. Comparing the SF fraction in individual clusters
to several statistical measures of substructure, we find weak, but in most
cases significant at greater than 2 sigma, correlations between substructure
and SF fraction. These results could indicate that cluster mergers may cause
weak but significant SF enhancement in clusters, or unrelaxed clusters exhibit
slightly stronger SF due to their less evolved states relative to relaxed
clusters.Comment: 10 pages, 6 figures, accepted for publication in Ap
Using Chemistry to Unveil the Kinematics of Starless Cores: Complex Radial Motions in Barnard 68
We present observations of 13CO, C18O, HCO+, H13CO+, DCO+ and N2H+ line
emission towards the Barnard 68 starless core. The line profiles are
interpreted using a chemical network coupled with a radiative transfer code in
order to reconstruct the radial velocity profile of the core. Our observations
and modeling indicate the presence of complex radial motions, with the inward
motions in the outer layers of the core but outward motions in the inner part,
suggesting radial oscillations. The presence of such oscillation would imply
that B68 is relatively old, typically one order of magnitude older than the age
inferred from its chemical evolution and statistical core lifetimes. Our study
demonstrates that chemistry can be used as a tool to constrain the radial
velocity profiles of starless cores.Comment: 12 pages, 3 figures, to appear in the Astrophysical Journal Letter
First results from the CALYPSO IRAM-PdBI survey. I. Kinematics of the inner envelope of NGC1333-IRAS2A
The structure and kinematics of Class 0 protostars on scales of a few hundred
AU is poorly known. Recent observations have revealed the presence of Keplerian
disks with a diameter of 150-180 AU in L1527-IRS and VLA1623A, but it is not
clear if such disks are common in Class 0 protostars. Here we present
high-angular-resolution observations of two methanol lines in NGC1333-IRAS2A.
We argue that these lines probe the inner envelope, and we use them to study
the kinematics of this region. Our observations suggest the presence of a
marginal velocity gradient normal to the direction of the outflow. However, the
position velocity diagrams along the gradient direction appear inconsistent
with a Keplerian disk. Instead, we suggest that the emission originates from
the infalling and perhaps slowly rotating envelope, around a central protostar
of 0.1-0.2 M. If a disk is present, it is smaller than the disk of
L1527-IRS, perhaps suggesting that NGC1333-IRAS2A is younger.Comment: Accepted for publication in A&A letter
Observation of the critical regime near Anderson localization of light
Diffusive transport is among the most common phenomena in nature [1].
However, as predicted by Anderson [2], diffusion may break down due to
interference. This transition from diffusive transport to localization of waves
should occur for any type of classical or quantum wave in any media as long as
the wavelength becomes comparable to the transport mean free path [3].
The signatures of localization and those of absorption, or bound states, can
however be similar, such that an unequivocal proof of the existence of wave
localization in disordered bulk materials is still lacking. Here we present
measurements of time resolved non-classical diffusion of visible light in
strongly scattering samples, which cannot be explained by absorption, sample
geometry or reduction in transport velocity. Deviations from classical
diffusion increase strongly with decreasing as expected for a phase
transition. This constitutes an experimental realization of the critical regime
in the approach to Anderson localization.Comment: 5 pages, 4 figure
Frank's constant in the hexatic phase
Using video-microscopy data of a two-dimensional colloidal system the
bond-order correlation function G6 is calculated and used to determine the
temperature-dependence of both the orientational correlation length xi6 in the
isotropic liquid phase and the Frank constant F_A in the hexatic phase. F_A
takes the value 72/pi at the hexatic to isotropic liquid phase transition and
diverges at the hexatic to crystal transition as predicted by the KTHNY-theory.
This is a quantitative test of the mechanism of breaking the orientational
symmetry by disclination unbinding
Non-collinear magnetism in Al-Mn topologically disordered systems
We have performed the first ab-initio calculations of a possible complex
non-collinear magnetic structure in aluminium-rich Al-Mn liquids within the
real-space tight-binding LMTO method. In our previous work we predicted the
existence of large magnetic moments in Al-Mn liquids [A.M. Bratkovsky, A.V.
Smirnov, D. N. Manh, and A. Pasturel, \prb {\bf 52}, 3056 (1995)] which has
been very recently confirmed experimentally. Our present calculations show that
there is a strong tendency for the moments on Mn to have a non-collinear
(random) order retaining their large value of about 3~. The d-electrons
on Mn demonstrate a pronounced non-rigid band behaviour which cannot be
reproduced within a simple Stoner picture. The origin of the magnetism in these
systems is a topological disorder which drives the moments formation and
frustrates their directions in the liquid phase.Comment: 10 pages, RevTex 3.0, 24kb. 3 PS figures available on request from
[email protected] The work has been presented at ERC
``Electronic Structire of Solids'' (Lunteren, The Netherlands, 9-14 September
1995
First results from the CALYPSO IRAM-PdBI survey - III. Monopolar jets driven by a proto-binary system in NGC1333-IRAS2A
Context: The earliest evolutionary stages of low-mass protostars are
characterised by hot and fast jets which remove angular momentum from the
circumstellar disk, thus allowing mass accretion onto the central object.
However, the launch mechanism is still being debated. Aims: We would like to
exploit high-angular (~ 0.8") resolution and high-sensitivity images to
investigate the origin of protostellar jets using typical molecular tracers of
shocked regions, such as SiO and SO. Methods: We mapped the inner 22" of the
NGC1333-IRAS2A protostar in SiO(5-4), SO(65-54), and the continuum emission at
1.4 mm using the IRAM Plateau de Bure interferometer in the framework of the
CALYPSO IRAM large program. Results: For the first time, we disentangle the
NGC1333-IRAS2A Class 0 object into a proto-binary system revealing two
protostars (MM1, MM2) separated by ~ 560 AU, each of them driving their own
jet, while past work considered a single protostar with a quadrupolar outflow.
We reveal (i) a clumpy, fast (up to |V-VLSR| > 50 km/s), and blueshifted jet
emerging from the brightest MM1 source, and (ii) a slower redshifted jet,
driven by MM2. Silicon monoxide emission is a powerful tracer of
high-excitation (Tkin > 100 K; n(H2) > 10^5 cm-3) jets close to the launching
region. At the highest velocities, SO appears to mimic SiO tracing the jets,
whereas at velocities close to the systemic one, SO is dominated by extended
emission, tracing the cavity opened by the jet. Conclusions: Both jets are
intrinsically monopolar, and intermittent in time. The dynamical time of the
SiO clumps is < 30-90 yr, indicating that one-sided ejections from protostars
can take place on these timescales.Comment: Astronomy & Astrophysics Letter, in pres
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