paper

Can Fluffy Dust Alleviate the "Subsolar" Interstellar Abundance Problem?

arXiv:astro-ph/0503564 · doi:10.1086/428038

Abstract

What might be the most appropriate set of interstellar reference abundances of chemical elements (both in gas and in dust) relative to hydrogen has been a subject of much discussion in the past decade. While historically the Sun has been taken as the reference standard, it has recently been suggested that the interstellar abundances might be better represented by those of B stars (because of their young ages) which are just ~60--70% of the widely adopted solar values (``subsolar''). On the other hand, the most recent estimates of the solar carbon and oxygen abundances are also close to those of B stars. If the interstellar abundances are indeed ``subsolar'' like B stars or the newly-determined solar C,O values, there might be a lack of raw material to form the dust to account for the interstellar extinction. In literature it has been argued that this problem could be solved if interstellar grains have a fluffy, porous structure since fluffy grains are more effective in absorbing and scattering optical and ultraviolet starlight than compact grains (on a per unit mass basis). However, we show in this work that, using the Kramers-Kronig relation, fluffy dust is not able to overcome the abundance shortage problem. A likely solution is that the abundances of refractory elements in stellar photospheres may under-represent the composition of the interstellar material from which stars are formed, resulting either from the possible underestimation of the degree of heavy-element settling in stellar atmospheres, or from the incomplete incorporation of heavy elements in stars during the star formation process.

15 pages, 2 figures, 1 table. To appear in The Astrophysical Journal, vol. 622 (the April-01-2005 issue)

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