Peer-Reviewed Journal Details
Mandatory Fields
Meaburn, J.,O'Connor, J. A.,LÛpez, J. A.,Bryce, M.,Redman, M. P.,Noriega-Crespo, A.
2000
Unknown
Monthly Notices Of The Royal Astronomical Society
The ejecta from the luminous blue variable star P Cygni
Published
()
Optional Fields
318
561
572
Further optical observations have been made with the Manchester Occulting Mask Imager and Manchester Echelle Spectrometer of the inner and outer shells of P Cygni, and of the 7-arcmin long giant lobe projecting from this luminous blue variable star. An image in the light of the fluorescently excited [Niii] 7378-≈ line has revealed the knottiness of the inner shell. Well defined `velocity ellipses' for the position/velocity arrays across the outer shell indicate that its expansion velocity is 160kms-1 which is somewhat lower than the previously reported value. The kinematical behaviour of the giant lobe, both in the vicinity of P Cygni, and further away, emphasizes its strange nature, although close association with P Cygni is again suggested by these new observations. One possibility is that this lobe is a `trail' of collimated ejected material. The observations are compared with a 60-mum IRAS high-resolution map of the region. A variety of possible explanations of the observed phenomena are explored, e.g. radio knots in the outer stellar wind either coalesce or expand to become the [Niii]7378-≈ emitting knots in the inner shell; that a mass-loaded wind overunning slower moving clumps explains the kinematics of the inner shell; that the one-sided giant lobe could be a `trail' of ejected material from P Cygni funnelled through the outer shell.Further optical observations have been made with the Manchester Occulting Mask Imager and Manchester Echelle Spectrometer of the inner and outer shells of P Cygni, and of the 7-arcmin long giant lobe projecting from this luminous blue variable star. An image in the light of the fluorescently excited [Niii] 7378-≈ line has revealed the knottiness of the inner shell. Well defined `velocity ellipses' for the position/velocity arrays across the outer shell indicate that its expansion velocity is 160kms-1 which is somewhat lower than the previously reported value. The kinematical behaviour of the giant lobe, both in the vicinity of P Cygni, and further away, emphasizes its strange nature, although close association with P Cygni is again suggested by these new observations. One possibility is that this lobe is a `trail' of collimated ejected material. The observations are compared with a 60-mum IRAS high-resolution map of the region. A variety of possible explanations of the observed phenomena are explored, e.g. radio knots in the outer stellar wind either coalesce or expand to become the [Niii]7378-≈ emitting knots in the inner shell; that a mass-loaded wind overunning slower moving clumps explains the kinematics of the inner shell; that the one-sided giant lobe could be a `trail' of ejected material from P Cygni funnelled through the outer shell.
0035-87110035-8711
http://adsabs.harvard.edu/abs/2000MNRAS.318..561Mhttp://adsabs.harvard.edu/abs/2000MNRAS.318..561M
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