Image linked to itself; Image description: A cartoon of an interstellar dust grain

    Figure: Interstellar dust cartoons and brief explication of interstellar dust

    Image 1 Caption: A cartoon of a model of an interstellar dust grain: sizes down to ∼ 0.0003 microns can occur (Ze-337; HI-371,374). Note, ammonia (NH_3) is spelt wrong in Image 1. Ammonia at room temperatures is a colorless, pungent gas that dissolves easily in water.

    Further explication:

    1. The ices would probably only be present in dense nebulae like molecular clouds and protoplanetary disks??? where it it cold enough for them and they are largely shielded from electromagnetic radiation (EMR) in the ultraviolet band (fiducial range 0.01--0.4 μm)???.

      Image linked to original source; Image description: A model of an interstellar dust grain with a silicate core and an ice mantle

    2. Image 2 Caption: Image 2 A more detailed model of an interstellar dust grain with a silicate core and a mantle of ices:
      1. atomic hydrogen (H) (which is probably just isolated atoms since atomic hydrogen does not form an ice.
      2. ammonia (NH3).
      3. carbon dioxide (CO2) (called dry ice when solid).
      4. carbon monoxide (CO).
      5. formaldehyde (H2CO or CH2O).
      6. methane (CH4).
      7. methanol (CH3OH).
      8. molecular hydrogen (H2).
      9. water (H2O).
      10. organic molecules which are all molecules containing carbon (C).
      Note, cosmic rays and ultraviolet radiation (fiducial range 0.01--0.4 μm) tend to destroy the ice mantle.

    Credit and/or file tracking information follows to the divider line:

    Images:
    1. Credit/Permission: © Ralf Srama et al., 2009 / No permission.
      Image link: Itself.
      Image website: Ralf Srama et al., 2009.
      Placeholder image: alien_click_to_see_image.html.
    2. Credit/Permission: © David Jeffery, 2003 / Own work.
      Image link: Itself.
    Local file: local link: interstellar_dust.html.
    File: Star file: interstellar_dust.html.