Disk mass and Halpha EW of zeta Tau
Posted: Mon Mar 07, 2016 4:04 pm
I guess that the majority of the ARAS observers knows the ARAS long-term Halpha monitoring of zeta Tau (http://astrospectroscopy.de/media/files/IBVS-5813.pdf)
Several days ago I got the poster "The Variable and Asymmetric Disk of zeta Tau", presented by Christopher Tycner (Central Michigan University, Mount Pleasant, MI, United States) & Aaron Sigut (The University of Western Ontario, London, ON, Canada) at the IAU meeting last year (http://adsabs.harvard.edu/abs/2015IAUGA..2255073T)
That poster shows among others long-baseline interferometric observations in the optical part of the spectrum of zeta Tau in order to complement spectroscopic observations. Fig. 4 of the poster shows the (interferometric) total disk mass as a function of time since Dec 3, 2003 based on the Halpha emission profile fits.
That Fig. offers an excellent opportunity, to compare our Halpha long-term monitoring for the same time section (see the attached Fig.). We can recognize that the disk mass correlates with the Halpha EW. This is not surprising, because the disk contains mostly ionized hydrogen, which is responsible for the line emission, but a wonderful confirmation of our work, which has been complemented by other methods of the professional astronomy. I try to stay in contact with the researchers.
Ernst Pollmann
Several days ago I got the poster "The Variable and Asymmetric Disk of zeta Tau", presented by Christopher Tycner (Central Michigan University, Mount Pleasant, MI, United States) & Aaron Sigut (The University of Western Ontario, London, ON, Canada) at the IAU meeting last year (http://adsabs.harvard.edu/abs/2015IAUGA..2255073T)
That poster shows among others long-baseline interferometric observations in the optical part of the spectrum of zeta Tau in order to complement spectroscopic observations. Fig. 4 of the poster shows the (interferometric) total disk mass as a function of time since Dec 3, 2003 based on the Halpha emission profile fits.
That Fig. offers an excellent opportunity, to compare our Halpha long-term monitoring for the same time section (see the attached Fig.). We can recognize that the disk mass correlates with the Halpha EW. This is not surprising, because the disk contains mostly ionized hydrogen, which is responsible for the line emission, but a wonderful confirmation of our work, which has been complemented by other methods of the professional astronomy. I try to stay in contact with the researchers.
Ernst Pollmann