About the B[e] stars
Posted: Sun Oct 09, 2011 11:24 am
Hello,
i'have started a program of observation of some B[e] stars of FS CMa type objects. This new class of objects present strong emission lines and infrared excess. It can be described as a hot star with dust environment. The question is where the dust is coming from ? Some are Binary candidate with a late type star, some other are binary with degenerated star or some are herbig Be star. Principal investigator is Anatoly Miroschnichenko, as primary amateur observation came from IAC80 ( http://gabalou.canalblog.com/archives/2 ... 88732.html ).
Two of this class are V1972 cyg and V2028 cyg easily observable now.
I took an eshell spectra of both star (R11000, thor arg calibrated, flat field and, instrumental response corrected)
The targets are from mag 10.5 to 10.8, but the emission lines are strong. I encouraged every observers to make spectra in low and high resolution, in every spectral domain, specially H alpha, Nir.
Radial velocity monitoring, spectral profiles and transients lines observation would permit a better comprehension of the FS cma object.
As exemple, V2028 cyg:
Merged spectra http://cjoint.com/?AJjntCJkDFq
i'have started a program of observation of some B[e] stars of FS CMa type objects. This new class of objects present strong emission lines and infrared excess. It can be described as a hot star with dust environment. The question is where the dust is coming from ? Some are Binary candidate with a late type star, some other are binary with degenerated star or some are herbig Be star. Principal investigator is Anatoly Miroschnichenko, as primary amateur observation came from IAC80 ( http://gabalou.canalblog.com/archives/2 ... 88732.html ).
Two of this class are V1972 cyg and V2028 cyg easily observable now.
I took an eshell spectra of both star (R11000, thor arg calibrated, flat field and, instrumental response corrected)
The targets are from mag 10.5 to 10.8, but the emission lines are strong. I encouraged every observers to make spectra in low and high resolution, in every spectral domain, specially H alpha, Nir.
Radial velocity monitoring, spectral profiles and transients lines observation would permit a better comprehension of the FS cma object.
As exemple, V2028 cyg:
Merged spectra http://cjoint.com/?AJjntCJkDFq