Clark, J. S.; Steele, I. A.; Fender, R. P. and Coe, M. J.
PDF (Version of Record)
- Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
|Google Scholar:||Look up in Google Scholar|
We present near IR spectra (0.8–2.5 µm) of the two candidate B[e]/X-ray binary systems CI Cam/XTE J0421+560 and HD34921/1H 0521+37. The spectra of both systems show evidence for a more complex circumstellar environment than those seen in classical Be/X-ray binaries. Strong H I and He I emission is seen, confirming the presence of a dense circumstellar wind; O I, Fe II and [Fe II] emission in CI Cam points to recombination of this wind. He II emission, presumably due to excitation by the compact companion is observed in CI Cam. Finally, emission is seen from Na I and CO, which implies regions of the circumstellar environment with much lower excitation temperatures and higher densities, shielded from direct stellar radiation. Both systems show evidence for continuum emission from circumstellar dust. Neither of these two features has previously been observed in any other classical Be/X-ray binary system. Adopting the classification criteria of Lamers et al. (1998) we suggest identifications of unclB[e] and sgB[e] for HD34921 and CI Cam respectively, making them the first High Mass X-ray Binaries with primaries showing the B[e] phenomenon known.
|Item Type:||Journal Article|
|Copyright Holders:||1999 European Southern Observatory (ESO)|
|Keywords:||stars; circumstellar matter; emission-line; Be|
|Academic Unit/Department:||Science > Physical Sciences
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Users 9108 not found.|
|Date Deposited:||16 Jul 2009 15:48|
|Last Modified:||23 Feb 2016 21:16|
|Share this page:|
Download history for this item
These details should be considered as only a guide to the number of downloads performed manually. Algorithmic methods have been applied in an attempt to remove automated downloads from the displayed statistics but no guarantee can be made as to the accuracy of the figures.