Grain destruction in interstellar shock waves

  title={Grain destruction in interstellar shock waves},
  author={B. Draine},
  journal={Astrophysics and Space Science},
  • B. Draine
  • Published 1995
  • Physics
  • Astrophysics and Space Science
Interstellar shock waves can erode and destroy grains present in the shocked gas, primarily as the result of sputtering and grain-grain collisions. Uncertainties in current estimates of sputtering yields are reviewed. Results are presented for the simple case of sputtering of fast grains being stopped in cold gas. An upper limit is derived for sputtering of refractory grains in C-type MHD shocks: shock speedsvs≳ 50 km s−1 are required for return of more than 30% of the silicate to the gas phase… Expand

Figures from this paper

The Physical and Chemical Effects of C-Shocks in Molecular Outflows
The bow shocks which are observed in jets associated with low-mass star formation probably have C-shock characteristics over at least part of their extent. We show that ion-neutral streaming inExpand
Destruction of Interstellar Dust
Interstellar dust is an important component of the interstellar medium. Dust grains are the dominant opacity source and thus regulate the radiative transfer in the interstellar medium. Besides theExpand
Parametrization of C-shocks. Evolution of the sputtering of grains
Context. The detection of narrow SiO line emission toward the young shocks of the L1448-mm outflow has been interpreted as a signature of the magnetic precursor of C-shocks. In contrast with the lowExpand
Monte Carlo Calculations of the Sputtering of Grains: Enhanced Sputtering of Small Grains
The sputtering of a small grain embedded in a plasma or hot gas in the interstellar medium (ISM) is calculated using a Monte Carlo binary collision code. This technique is used to describe theExpand
Evaporation of grain-surface species by shock waves in proto-planetary disk
Recent ALMA (Atacama Large Millimeter/submillimeter Array) observations of young protostellar objects detected warm SO emission, which could be associated with a forming protostellar disk. In orderExpand
Chemical evolution of the gas in C-type shocks in dark clouds
A magnetohydrodynamic model of a steady, transverse C-type shock in a dense molecular cloud is presented. A complete gas–grain chemical network is taken into account: the gas-phase chemistry, theExpand
Intergalactic medium metal enrichment through dust sputtering
We study the motion of dust grains into the intergalactic medium (IGM) around redshift z = 3, to test the hypothesis that grains can efficiently pollute the gas with metals through sputtering. We useExpand
We present a model in which the 22 GHz H2O masers observed in star-forming regions occur behind shocks propagating in dense regions (preshock density n 0 ~ 106-108 cm–3). We focus on high-velocityExpand
Bow shocks, bow waves, and dust waves – II. Beyond the rip point
Dust waves are a result of gas-grain decoupling in a stream of dusty plasma that flows past a luminous star. The radiation field is sufficiently strong to overcome the collisional coupling betweenExpand
Ion Interactions with Solids: Astrophysical Applications
Energetic plasma ions and electrons can significantly alter surfaces in the solar system and the interstellar medium (ISM) and produce observable gas-phase atoms and molecules. In order to understandExpand


Disruption and sputtering of grains in intermediate-velocity interstellar clouds
We present numerical models of grain sputtering and disruption by grain-grain collisions in intermediate-velocity (50--120 km s/sup -1/) interstellar clouds. The grain's gyromotion about the magneticExpand
Grain destruction in shocks in the interstellar medium
Destruction of interstellar dust occurs predominantly in supernova shock waves in the warm neutral/ionized medium (density approximately = 0.25/cu cm, temperature approximately = 10(exp 4) K). RecentExpand
Refractory grain destruction in low-velocity shocks.
Recent abundance determinations in intermediate-velocity clouds near the Orion association have shown that silicon abundances may be nearly cosmic even in clouds with a velocity as low as 40 to 50 kmExpand
Destruction mechanisms for interstellar dust
Destruction rates are estimated for interstellar dust grains as a function of size and composition of the grains, and the type of region in which the grain is located. Several idealized models of theExpand
The physics of grain-grain collisions and gas-grain sputtering in interstellar shocks
Grain-grain collisions and ion sputtering destroy dust grains in interstellar shocks. An analytical theory is developed for the propagation of shock waves in solids driven by grain-grain collisions,Expand
Grain disruption in interstellar hydromagnetic shocks
The observed abundance variations of Ca, Fe, Si, and Ti in intermediate-velocity interstellar gas suggest that grains have been disrupted in clouds with velocities as low as 20--50 km s/sup -1/. InExpand
The structure of the time-dependent interstellar shocks and grain destruction in the interstellar medium
A new theoretical analysis of the structure of interstellar shocks and the grain dynamics of these shocks is presented. The basic hydrodynamic equations for J-shocks in interstellar gas are given inExpand
Magneto-Hydrodynamic Shock Waves in Molecular Clouds
The fluid dynamics of MHD shock waves in magnetized molecular gas is reviewed. The different types of shock solutions, and the circumstances under which the different types occur, are delineated.Expand
Infrared emission from dust in shocked gas
The cooling effects of dust in shock-heated gas, and the resulting infrared emission spectra, are computed for a realistic two-component (silicate and carbon) model for interstellar dust with theExpand
Theory of Interstellar Shocks
The interstellar medium is intermittently disturbed by violent events­ supernova explosions being but one example-which cause large increases in the local pressure. As the result of the pressureExpand