Structural and chemical alteration of crystalline olivine under low energy He + irradiation
By K. Demyk, P. Carrez, H. Leroux, P. Cordier, A. Jones, J. Borg, E. Quirico, P. Raynal, L. D'hendecourt. 2001
148 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics, Geophysics
View Paper: https://www.semanticscholar.org/paper/b709f94795760690eb66a17b6b182bf1d6ff53d3
How researchers see this paper
The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.
In Astronomy and Astrophysics
- N. Evans II
- C. Dullemond
- E. V. van Dishoeck
- E. Dishoeck
- J. Jørgensen
- A. Boogert
- K. Pontoppidan
- G. Blake
Citations in the corpus
- The Absence of Crystalline Silicates in the Diffuse Interstellar Medium (2004, background): “…several laboratory studies have investigated the effect of ion bombardments on crystalline grains (e.g., Day 1977; Bradley 1994; Wang et al. 1998; Demyk et al. 2001; Carrez et al. 2002; Jäger et al. 2003b; Brucato et al. 2004), measuring the required dose for amorphization as a function of…”
- Ion irradiation of carbonaceous chondrites: A new view of space weathering on primitive asteroids (2017, methodology): “…CCs or terrestrial olivine sample; corresponding to band number 3) exceeds the position of a crystalline olivine with a forsterite number of 0 (no Mg content = 100 % fayalite) [Hamilton, 2010]: this is because Mg loss is also accompanied by amorphization [Demyk et al., 2001; Carrez et al., 2002].”
- The global dust modelling framework THEMIS (The Heterogeneous dust Evolution Model for Interstellar Solids) (2017, background): “For example, photon, ion and electron irradiation can induce changes in the dust chemical composition and structure (e.g., Demyk et al. 2001, 2004), hydrogenation and accretion can drive changes in the grain chemical composition (e.g., Hecht 1986; Sorrell 1990, 1991; Mennella 2008, 2010; Jones…”
- c2d Spitzer IRS Spectra of Disks around T Tauri Stars. I. Silicate Emission and Grain Growth (2005, background): “Enhanced pyroxene-to-olivine abundances were previously observed toward high-mass protostars with ISO and may be explained by He+ sputtering in high-velocity shocks (Demyk et al. 2001 and references therein).”