Modeling accretion shocks at the disk–envelope interface

Astronomy and Astrophysics, vol. 653, pp. A159

Abstract

Context.As material from an infalling protostellar envelope hits the forming disk, an accretion shock may develop which could (partially) alter the envelope material entering the disk. Observations with the Atacama Large Millimeter/submillimeter Array (ALMA) indicate that emission originating from warm SO and SO2might be good tracers of such accretion shocks. Aims.The goal of this work is to test under what shock conditions the abundances of gas-phase SO and SO2increase in an accretion shock at the disk–envelope interface. Methods.Detailed shock models including gas dynamics were computed using the Paris-Durham shock code for nonmagnetizedJ-type accretion shocks in typical inner envelope conditions. The effect of the preshock density, shock velocity, and strength of the ultraviolet (UV) radiation field on the abundance of warm SO and SO2is explored. Compared with outflows, these shocks involve higher densities (~107cm−3), lower shock velocities (~few km s−1), and large dust grains (~0.2 μm) and thus probe a different parameter space. Results.Warm gas-phase chemistry is efficient in forming SO under mostJ-type shock conditions considered. In lower-velocity (~3 km s−1) shocks, the abundance of SO is increased through subsequent reactions starting from thermally desorbed CH4toward H2CO and finally SO. In higher velocity (≳4 km s−1) shocks, both SO and SO2are formed through reactions of OH and atomic S. The strength of the UV radiation field is crucial for SO and in particular SO2formation through the photodissociation of H2O. Thermal desorption of SO and SO2ice is only relevant in high-velocity (≳5 km s−1) shocks at high densities (≳107cm−3). Both the composition in the gas phase, in particular the abundances of atomic S and O, and in ices such as H2S, CH4, SO, and SO2play a key role in the abundances of SO and SO2that are reached in the shock. Conclusions.Warm emission from SO and SO2is a possible tracer of accretion shocks at the disk–envelope interface as long as a local UV field is present. Observations with ALMA at high-angular resolution could provide further constraints given that other key species for the gas-phase formation of SO and SO2, such as H2S and H2CO, are also covered. Moreover, theJames WebbSpace Telescope will give access to other possible slow, dense shock tracers such as H2, H2O, and [S I] 25 μm.

Authors 4

1. M. L. van Gelder Aachen Leiden Observatory

   Leiden University · Leiden Observatory

   Affiliation as printed

   Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands

2. Benoît Tabone Aachen Leiden Observatory

   Leiden University · Leiden Observatory

   Affiliation as printed

   Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands

3. Ewine F. van Dishoeck Aachen Leiden Observatory

   Leiden University · Max Planck Institute for Extraterrestrial Physics · Leiden Observatory

   Affiliation as printed

   Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands

   Max Planck Institut für Extraterrestrische Physik (MPE), Giessenbachstrasse 1, 85748 Garching, Germany

4. B. Godard

   Centre National de la Recherche Scientifique · Université Paris Sciences et Lettres · Observatoire de Paris · École Normale Supérieure - PSL · Sorbonne Université · Laboratoire d’Etudes du Rayonnement et de la Matière en Astrophysique et Atmosphères · Laboratoire de Physique de l'Ecole Normale Supérieure

   Affiliation as printed

   Laboratoire de Physique de l’École normale supérieure, ENS, Université PSL, CNRS, Sorbonne Université, Université de Paris, 75005 Paris, France

   Observatoire de Paris, Université PSL, Sorbonne Université, LERMA, 75014 Paris, France

   Laboratoire de Physique de l'École normale supérieure, ENS, Université PSL, CNRS, Sorbonne Université, Université de Paris, 75005 Paris, France