597 research outputs found
The Photoevaporative Wind from the Disk of TW Hya
Photoevaporation driven by the central star is expected to be a ubiquitous
and important mechanism to disperse the circumstellar dust and gas from which
planets form. Here, we present a detailed study of the circumstellar disk
surrounding the nearby star TW Hya and provide observational constraints to its
photoevaporative wind. Our new high-resolution (R ~ 30,000) mid-infrared
spectroscopy in the [Ne II] 12.81 {\mu}m line confirms that this gas diagnostic
traces the unbound wind component within 10AU from the star. From the blueshift
and asymmetry in the line profile, we estimate that most (>80%) of the [Ne II]
emission arises from disk radii where the midplane is optically thick to the
redshifted outflowing gas, meaning beyond the 1 or 4AU dust rim inferred from
other observations. We re-analyze high-resolution (R ~ 48, 000) archival
optical spectra searching for additional transitions that may trace the
photoevaporative flow. Unlike the [Ne II] line, optical forbidden lines from
OI, SII, and MgI are centered at the stellar velocity and have symmetric
profiles. The only way these lines could trace the photoevaporative flow is if
they arise from a disk region physically distinct from that traced by the [Ne
II] line, specifically from within the optically thin dust gap. However, the
small (~10 km/s) FWHM of these lines suggest that most of the emitting gas
traced at optical wavelengths is bound to the system rather than unbound. We
discuss the implications of our results for a planet-induced versus a
photoevaporation-induced gap.Comment: Accepted for publication in Ap
Turbulent viscosity in clumpy accretion disks II supernova driven turbulence in the Galaxy
An analytical model for a turbulent clumpy gas disk is presented where
turbulence is maintained by the energy input due to supernovae. Expressions for
the disk parameters, global filling factors, molecular fractions, and star
formation rates are given as functions of the Toomre parameter , the ratio
between the cloud size and the turbulent driving length scale , the
mass accretion rate within the disk , the constant of molecule
formation , the disk radius, the angular velocity, and its radial
derivative. Two different cases are investigated: a dominating stellar disk and
a self-gravitating gas disk in direction. The turbulent driving wavelength
is determined in a first approach by energy flux conservation, i.e. the
supernovae energy input is transported by turbulence to smaller scales where it
is dissipated. The results are compared to those of a fully gravitational
model. For Q=1 and both models are consistent with each other. In a
second approach the driving length scale is directly determined by the size of
supernovae remnants. Both models are applied to the Galaxy and can reproduce
its integrated and local gas properties. The influence of thermal and magnetic
pressure on the disk structure is investigated. We infer and
for the Galaxy.Comment: 15 pages with 10 figures. Accepted for publication in A&
A multi-wavelength study of a double intermediate-mass protostar - from large-scale structure to collimated jets
(abridged) We study a previously discovered protostellar source that is
deeply embedded and drives an energetic molecular outflow. The source, UYSO1,
is located close to IRAS 07029-1215 at a distance of ~1 kpc. The
multi-wavelength observations resulted in the detection of a double
intermediate-mass protostar at the location of UYSO1. In addition to the
associated molecular outflow, with a projected size of 0.25 pc, two
intersecting near-infrared jets with projected sizes of 0.4 pc and 0.2 pc were
found. However, no infrared counterparts to the driving sources could be
detected in sensitive near- to far-infrared observations. In interferometric
millimeter observations, UYSO1 was resolved into two continuum sources with
high column densities and gas masses of 3.5 Mo and 1.2 Mo, with a linear
separation of 4200 AU. We report the discovery of a H2O maser toward one of the
two sources. The total luminosity is roughly estimated to be ~50 Lo, shared by
the two components, one of which is driving the molecular outflow that has a
dynamical timescale of less than a few thousand years. The jets of the two
individual components are not aligned. Submillimeter observations show that the
region lacks typical hot-core chemistry. We thus find two protostellar objects,
whose associated circumstellar and parent core masses are high enough to
suggest that they may evolve into intermediate-mass stars. This is corroborated
by their association with a very massive and energetic CO outflow, suggesting
high protostellar accretion rates. The short dynamical timescale of the
outflow, the pristine chemical composition of the cloud core and absence of hot
core tracers, the absence of detectable radio continuum emission, and the very
low protostellar luminosity argue for an extremely early evolutionary stage.Comment: 10 pages, 10 figures, accepted for publication in A&A; minor changes:
typos corrected, revised argument in Section
High angular resolution mm- and submm-observations of dense molecular gas in M82
Researchers observed CO(7-6), CO(3-2), HCN(3-2) and HCO+(3-2) line emission toward the starburst nucleus of M82 and have obtained an upper limit to H13CN(3-2). These are the first observations of the CO(7-6), HCN(3-2) and HCO+(3-2) lines in any extragalactic source. Researchers took the CO(7-6) spectrum in January 1988 at the Infrared Telescope Facility (IRTF) with the Max Planck Institute for Extraterrestrial Physics/Univ. of California, Berkeley 800 GHz Heterodyne Receiver. In March 1989 researchers used the Institute for Radio Astronomy in the Millimeter range (IRAM) 30 m telescope to observe the CO(3-2) line with the new MPE 350 GHz Superconductor Insulator Superconductor (SIS) receiver and the HCN(3-2) and HCO+(3-2) lines with the (IRAM) 230 GHz SIS receiver (beam 12" FWHM, Blundell et al. 1988). The observational parameters are summarized
Optimization of glycolipid synthesis in hydrophilic deep eutectic solvents
Glycolipids are considered an alternative to petrochemically based surfactants because they are non-toxic, biodegradable, and less harmful to the environment while having comparable surface-active properties. They can be produced chemically or enzymatically in organic solvents or in deep eutectic solvents (DES) from renewable resources. DES are non-flammable, non-volatile, biodegradable, and almost non-toxic. Unlike organic solvents, sugars are easily soluble in hydrophilic DES. However, DES are highly viscous systems and restricted mass transfer is likely to be a major limiting factor for their application. Limiting factors for glycolipid synthesis in DES are not generally well understood. Therefore, the influence of external mass transfer, fatty acid concentration, and distribution on initial reaction velocity in two hydrophilic DES (choline:urea and choline:glucose) was investigated. At agitation speeds of and higher than 60 rpm, the viscosity of both DES did not limit external mass transfer. Fatty acid concentration of 0.5 M resulted in highest initial reaction velocity while higher concentrations had negative effects. Fatty acid accessibility was identified as a limiting factor for glycolipid synthesis in hydrophilic DES. Mean droplet sizes of fatty acid-DES emulsions can be significantly decreased by ultrasonic pretreatment resulting in significantly increased initial reaction velocity and yield (from 0.15 ± 0.03 μmol glucose monodecanoate/g DES to 0.57 ± 0.03 μmol/g) in the choline: urea DES. The study clearly indicates that fatty acid accessibility is a limiting factor in enzymatic glycolipid synthesis in DES. Furthermore, it was shown that physical pretreatment of fatty acid-DES emulsions is mandatory to improve the availability of fatty acids
The CHESS survey of the L1157-B1 shock: the dissociative jet shock as revealed by Herschel--PACS
Outflows generated by protostars heavily affect the kinematics and chemistry
of the hosting molecular cloud through strong shocks that enhance the abundance
of some molecules. L1157 is the prototype of chemically active outflows, and a
strong shock, called B1, is taking place in its blue lobe between the
precessing jet and the hosting cloud. We present the Herschel-PACS 55--210
micron spectra of the L1157-B1 shock, showing emission lines from CO, H2O, OH,
and [OI]. The spatial resolution of the PACS spectrometer allows us to map the
warm gas traced by far-infrared (FIR) lines with unprecedented detail. The
rotational diagram of the high-Jup CO lines indicates high-excitation
conditions (Tex ~ 210 +/- 10 K). We used a radiative transfer code to model the
hot CO gas emission observed with PACS and in the CO (13-12) and (10-9) lines
measured by Herschel-HIFI. We derive 20010^5 cm-3. The CO
emission comes from a region of about 7 arcsec located at the rear of the bow
shock where the [OI] and OH emission also originate. Comparison with shock
models shows that the bright [OI] and OH emissions trace a dissociative J-type
shock, which is also supported by a previous detection of [FeII] at the same
position. The inferred mass-flux is consistent with the "reverse" shock where
the jet is impacting on the L1157-B1 bow shock. The same shock may contribute
significantly to the high-Jup CO emission.Comment: 7 pages, 9 figures, accepted for publication in Astronomy and
Astrophysic
Incorporation of stochastic chemistry on dust grains in the PDR code using moment equations
Unlike gas-phase reactions, chemical reactions taking place on interstellar
dust grain surfaces cannot always be modeled by rate equations. Due to the
small grain sizes and low flux,these reactions may exhibit large fluctuations
and thus require stochastic methods such as the moment equations.
We evaluate the formation rates of H2, HD and D2 molecules on dust grain
surfaces and their abundances in the gas phase under interstellar conditions.
We incorporate the moment equations into the Meudon PDR code and compare the
results with those obtained from the rate equations. We find that within the
experimental constraints on the energy barriers for diffusion and desorption
and for the density of adsorption sites on the grain surface, H2, HD and D2
molecules can be formed efficiently on dust grains.
Under a broad range of conditions, the moment equation results coincide with
those obtained from the rate equations. However, in a range of relatively high
grain temperatures, there are significant deviations. In this range, the rate
equations fail while the moment equations provide accurate results. The
incorporation of the moment equations into the PDR code can be extended to
other reactions taking place on grain surfaces
Spatially Resolved Spitzer-IRS Spectral Maps of the Superwind in M82
We have mapped the superwind/halo region of the nearby starburst galaxy M82
in the mid-infrared with . The spectral regions covered include
the H, [NeII], [NeIII] emission lines and PAH features. We
estimate the total warm H mass and the kinetic energy of the outflowing
warm molecular gas to be between M and
erg. Using the ratios of the 6.2, 7.7 and 11.3
micron PAH features in the IRS spectra, we are able to estimate the average
size and ionization state of the small grains in the superwind. There are large
variations in the PAH flux ratios throughout the outflow. The 11.3/7.7 and the
6.2/7.7 PAH ratios both vary by more than a factor of five across the wind
region. The Northern part of the wind has a significant population of PAH's
with smaller 6.2/7.7 ratios than either the starburst disk or the Southern
wind, indicating that on average, PAH emitters are larger and more ionized. The
warm molecular gas to PAH flux ratios (H) are enhanced in the outflow
by factors of 10-100 as compared to the starburst disk. This enhancement in the
H ratio does not seem to follow the ionization of the atomic gas (as
measured with the [NeIII]/[NeII] line flux ratio) in the outflow. This suggests
that much of the warm H in the outflow is excited by shocks. The observed
H line intensities can be reproduced with low velocity shocks ( km
s) driven into moderately dense molecular gas (
cm) entrained in the outflow.Comment: 19 pages and 12 figures; accepted in MNRA
Directional Radiation and Photodissociation Regions in Molecular Hydrogen Clouds
Some astrophysical observations of molecular hydrogen point to a broadening
of the velocity distribution for molecules at excited rotational levels. This
effect is observed in both Galactic and high redshift clouds. Analysis of H_2,
HD, and CI absorption lines has revealed the broadening effect in the
absorption system of QSO 1232+082 (z_{abs}=2.33771). We analyze line broadening
mechanisms by considering in detail the transfer of ultraviolet radiation (in
the resonance lines of the Lyman and Werner H_2 molecular bands) for various
velocity distributions at excited rotational levels. The mechanism we suggest
includes the saturation of the lines that populate excited rotational levels
(radiative pumping) and manifests itself most clearly in the case of
directional radiation in the medium. Based on the calculated structure of a
molecular hydrogen cloud in rotational level populations, we have considered an
additional mechanism that takes into account the presence of a
photodissociation region. Note that disregarding the broadening effects we
investigated can lead to a significant systematic error when the data are
processed.Comment: 14 pages, 10 figure
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