Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000jgr...10510363e&link_type=abstract
Journal of Geophysical Research, Volume 105, Issue A5, p. 10363-10370
Astronomy and Astrophysics
Astrophysics
19
Solar Physics, Astrophysics, And Astronomy
Scientific paper
Some portion of the interstellar dust entering the heliosphere is a refractory (Ca-Al-Ti-Mg-Si-Fe-Ni-Cr-Co-rich) component either condensed at high temperature from stellar outflows or formed in the interstellar medium (ISM). Condensation sequences for T>1100K, assuming chemical equilibrium, are calculated for stellar outflow gas having (1) solar composition at various Ptot; (2) compositions approaching C/O=0.9, otherwise solar; (3) metallicities reduced by Z/Z0=0.10; and (4) metallicities enhanced by added dust components. Calculated depletions are relatively insensitive to these excursions from the canonical ``cosmic'' abundances. The intragroup similarities of depletions observed for the element groups (Ca-Ti), (Fe-Ni-Cr-Co), and (Mg-Si) reflect the dominant mineralogy calculated for stardust: Ti- and Ca-aluminate phases, metal alloy, and Mg2SiO4 (Mg-olivine). This result suggests that the bulk of the refractory component of ISM dust was condensed in stellar environments.
No associations
LandOfFree
Variations on solar condensation: Sources of interstellar dust nuclei does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Variations on solar condensation: Sources of interstellar dust nuclei, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Variations on solar condensation: Sources of interstellar dust nuclei will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1195376