Seeds of Life in Space (SOLIS). III. Zooming Into the Methanol Peak of the Prestellar Core L1544

Toward the prestellar core L1544, the methanol (CH3OH) emission forms an asymmetric ring around the core center, where CH3OH is mostly in solid form, with a clear peak at 4000 au to the northeast of the dust continuum peak. As part of the NOEMA Large Project SOLIS (Seeds of Life in Space), the CH3OH peak has been spatially resolved to study its kinematics and physical structure and to investigate the cause behind the local enhancement. We find that methanol emission is distributed in a ridge parallel to the main axis of the dense core. The centroid velocity increases by about 0.2 km s−1 and the velocity dispersion increases from subsonic to transonic toward the central zone of the core, where the velocity field also shows complex structure. This could be an indication of gentle accretion of material onto the core or the interaction of two filaments, producing a slow shock. We measure the rotational temperature and show that methanol is in local thermodynamic equilibrium (LTE) only close to the dust peak, where it is significantly depleted. The CH3OH column density, N tot(CH3OH), profile has been derived with non-LTE radiative transfer modeling and compared with chemical models of a static core. The measured N tot(CH3OH) profile is consistent with model predictions, but the total column densities are one order of magnitude lower than those predicted by models, suggesting that the efficiency of reactive desorption or atomic hydrogen tunneling adopted in the model may be overestimated; or that an evolutionary model is needed to better reproduce methanol abundance

VizieR Online Data Catalog: SOLIS. II. L1157-B1 NH2CHO image (Codella+, 2017)

Datacube in fits format of the NH2CHO(41,4-31,3) towards L1157-B1 using the IRAM-NOEMA interferometer (see Fig. 1). The L1157-B1 shock was observed at 3mm with the IRAM NOEMA seven-element array during several tracks in July, October, and November 2015 using both the C and D configurations. The shortest and longest baselines are 19m and 237m, respectively, allowing us to recover emission at scales up to ~17". (2 data files)

VizieR Online Data Catalog: SOLIS. I. OMC2-FIR4 HC3N and HC5N images (Fontani+, 2017)

IRAM-NOEMA Interferometer, 3mm receiver, Widex and Narrow-band correlators. Observations with the IRAM NOEMA Interferometer of HC3N (9-8) and HC5N (31-30), at rest frequencies 81.881468GHz and 82.539039GHz , respectively, towards OMC-2 FIR4 have been carried out over 5 days between the 5th and the 19th of August, 2015. The HC3N line was observed in the Widex band correlator, providing a resolution in velocity of ~7.15km/s, while the HC5N line was observed also in the Narrow band correlator with a resolution in velocity of ~0.57km/s. (2 data files)

3D modelling of HCO+^+ and its isotopologues in the low-mass proto-star IRAS16293−-2422

International audienceIons and electrons play an important role in various stages of the star formation process. By following the magnetic field of their environment and interacting with neutral species, they slow down the gravitational collapse of the proto-star envelope. This process (known as ambipolar diffusion) depends on the ionisation degree, which can be derived from the \hco abundance. We present a study of \hco and its isotopologues (H$^{13}$CO$^+$, HC$^{18}$O$^+$, DCO$^+$, and H$^{13}$CO$^+$) in the low-mass proto-star IRAS16293$-$2422. The structure of this object is complex, and the HCO$^+$ emission arises from the contribution of a young NW-SE outflow, the proto-stellar envelope and the foreground cloud. We aim at constraining the physical parameters of these structures using all the observed transitions. For the young NW-SE outflow, we derive $T_{\rm kin}=180-220$ K and $n({\rm H_2})=(4-7)\times10^6$ cm$^{-3}$ with an HCO$^+$ abundance of $(3-5)\times10^{-9}$. Following previous studies, we demonstrate that the presence of a cold ($T_{\rm kin}$$\leqslant$30 K) and low density ($n({\rm H_2})\leqslant1\times10^4$ cm$^{-3}$) foreground cloud is also necessary to reproduce the observed line profiles. We have used the gas-grain chemical code \textsc{nautilus} to derive the HCO$^+$ abundance profile across the envelope and the external regions where X(HCO$^+$)$\gtrsim1\times10^{-9}$ dominate the envelope emission. From this, we derive an ionisation degree of $10^{-8.9}\,\lesssim\,x(e)\,\lesssim\,10^{-7.9}$. The ambipolar diffusion timescale is $\sim$5 times the free-fall timescale, indicating that the magnetic field starts to support the source against gravitational collapse and the magnetic field strength is estimated to be $6-46 \mu$G

Experimental approach of lessivage: Quantification and mechanisms

International audienceLessivage, also called argilluviation, consists of a substantial vertical transfer of particles less than 2 pm from a superficial departure horizon to a deeper horizon. This process is common in many soil types and responsible for the development of a textural differentiation in soil profiles in the subsurface. However, the mechanisms of lessivage are still poorly understood, and to our knowledge, lessivage has rarely been quantified. We propose here two original experiments of in vitro pedogenesis on soil columns to analyse the mechanisms acting in eluviation and illuviation, the two phases of lessivage, and to quantify these two phases in terms of particle export and fixation. We paid special attention to the experimental conditions, so that the conditions were favourable for lessivage and as close as possible to field conditions. The eluviation experiment showed that the release of particles was not the determining process for lessivage. We also showed that the smectite selectivity of eluviation was not continuous overtime. Both physical and chemical processes were identified as acting on both eluviation and illuviation. Concerning illuviation, experiments showed that from 25 to 90% of the eluviated particles were retained in the deeper horizon. Although large, to our knowledge this range represents the first quantification of illuviation. (C) 2013 Elsevier B.V. All rights reserved

The Chemistry of Phosphorus-bearing Molecules under Energetic Phenomena

For decades, the detection of phosphorus-bearing molecules in the interstellar medium was restricted to high-mass star-forming regions (as e.g. SgrB2 and Orion KL) and the circumstellar envelopes of evolved stars. However, recent higher-sensitivity observations have revealed that molecules such as PN and PO are present not only toward cold massive cores and low-mass star-forming regions with PO/PN ratios >1, but also toward the Giant Molecular Clouds in the Galactic Center known to be exposed to highly energetic phenomena such as intense UV radiation fields, shock waves and cosmic rays. In this paper, we carry out a comprehensive study of the chemistry of phosphorus-bearing molecules across different astrophysical environments which cover a range of physical conditions (cold molecular dark clouds, warm clouds, hot cores/hot corinos) and are exposed to different physical processes and energetic phenomena (proto-stellar heating, shock waves, intense UV radiation and cosmic rays). We show how the measured PO/PN ratio (either >1 as in e.g. hot molecular cores, or <1 as in UV strongly illuminated environments) can provide constraints on the physical conditions and energetic processing of the source. We propose that the reaction P + OH --> PO + H, not included in previous works, could be an efficient gas-phase PO formation route in shocks. Our modelling provides a template with which to study the detectability of P-bearing species not only in regions in our own Galaxy but also in extragalactic sources.Comment: 16 pages, 4 tables, 15 figures, accepted for Ap

Improvement of heat transfer in joule effect tubular heat exchanger by geometrical modifications. Applications to model (milky dessert) and real (whole egg) fluids

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Amélioration des performances thermiques d'un échangeur tubulaire à effet Joule (T.P.C.) par modification géométrique. Application sur des fluides modèle et réel

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