A Be star with a low nitrogen abundance in the SMC cluster NGC330

Details A Be star with a low nitrogen abundance in the SMC cluster NGC330 A Be star with a low nitrogen abundance in the SMC cluster NGC330

2004-07-13

arxiv.org/abs/astro-ph/0407258v1

Astron.Astrophys. 438 (2005) 265

Astronomy and Astrophysics

Astrophysics

7 pages, 4 figures. Submitted to A&A

Scientific paper

10.1051/0004-6361:20041653

High-resolution UVES/VLT spectra of B12, an extreme pole-on Be star in the SMC cluster NGC330, have been analysed using non-LTE model atmospheres to obtain its chemical composition relative to the SMC standard star AV304. We find a general underabundance of metals which can be understood in terms of an extra contribution to the stellar continuum due to emission from a disk which we estimate to be at the ~25% level. When this is corrected for, the nitrogen abundance for B12 shows no evidence of enhancement by rotational mixing as has been found in other non-Be B-type stars in NGC330, and is inconsistent with evolutionary models which include the effects of rotational mixing. A second Be star, NGC330-B17, is also shown to have no detectable nitrogen lines. Possible explanations for the lack of rotational mixing in these rapidly rotating stars are discussed, one promising solution being the possibility that magnetic fields might inhibit rotational mixing.

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