The Sulfur and Iron Abundance of the Peculiar SDO Star Feige 46: a Crucial Test of the Dust Fractionation Hypothesis CYC4 - Medium

Details The Sulfur and Iron Abundance of the Peculiar SDO Star Feige 46: a Crucial Test of the Dust Fractionation Hypothesis CYC4 - Medium The Sulfur and Iron Abundance of the Peculiar SDO Star Feige 46: a Crucial Test of the Dust Fractionation Hypothesis CYC4 - Medium

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994hst..prop.5319h&link_type=abstract

HST Proposal ID #5319

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Hst Proposal Id #5319 Hot Stars Late Evolution

Scientific paper

Feige 46 is a helium rich, subluminous O star that displays a very peculiar abundance pattern dissimilar to all other sdO stars analysed so far. C and N are almost solar whereas Mg and Si are deficient by a factor of 7 and 50, respectively. Its abundance pattern bears strong resemblence to that found in peculiar post-AGB F stars. Their depletion pattern are qualitatively similar to that found in the interstellar medium and therefore dust fractionation has been proposed as the origin of these pecularities. The same mechanism was recently suggested to explain the C/Si anticorrelation and the Si/Fe correlation found in normal A and Lambda Boo stars. This proposals sets out to test whether the dust fractionation mechanism can explain the abundance pattern of Feige 46. The measurement of the abundance of a volatile element such as Ar, S or Zn is necessary. For Feige 46 only S is accessible to a NLTE analysis at present via its strongest UV line at 1501.8 Angstroem. In addition the Fe/Si ratio shall be derived from UV spectra to check whether the A star correlation is also valid for Feige 46. Existing IUE spectra are of insufficient quality and the GHRS is required to obtain suitable data. If proven Feige 46 would be the first highly-evolved O-type star whose surface composition is governed by the separation of gas and dust.

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