Halpha observation
Posted: Sun Aug 23, 2015 3:01 pm
Some observations goals of interest around the Halpha area:
Halpha equivalent width:
we can understand the EW of the Halpha line profile (among others) as indicator of the mass lost rate of the M type star into the accretion disk of the B star. The discussion with Phil Bennet about my EW measurements during the last (approx.) 20 years leads to the assumption, that the mass loss rate (EW-scatter out side the eclipse) is of stochastic character (see the attached EW monitoring). During the coming years it is of certain interest, to monitor the EW on short time scales in order to find out any periodicities if there are (one spectrum per week).
V/R variability:
the Halpha profile is devided by a central absorption core. This absorption is caused of the amount of neutral hydrogen gas in the outer (cool) region of the accretion disk around the B star, from the super-giant itself, and from the hydrogen cloud which surrounds the whole system. Because of the orbital movement of the B star and its disk, we have to expect a certain variability of the radial velocity (dependently of the orbit) of the central absorption core.
(see the attached radial velocity plot). That's why we can observe a corresponding variation of the V/R ratio (see the attached V/R montoring).
The question is, is there in addition a further influence on the V/R ratio? There is a statement from a professional astronomer, that the violett component (V-peak) has been always stronger than the red component (R-peak) of the profile. If so, why? A larger density (or temperature) of the accretion disk in the area, which rotates in the line of sight towards us?
Ernst
Halpha equivalent width:
we can understand the EW of the Halpha line profile (among others) as indicator of the mass lost rate of the M type star into the accretion disk of the B star. The discussion with Phil Bennet about my EW measurements during the last (approx.) 20 years leads to the assumption, that the mass loss rate (EW-scatter out side the eclipse) is of stochastic character (see the attached EW monitoring). During the coming years it is of certain interest, to monitor the EW on short time scales in order to find out any periodicities if there are (one spectrum per week).
V/R variability:
the Halpha profile is devided by a central absorption core. This absorption is caused of the amount of neutral hydrogen gas in the outer (cool) region of the accretion disk around the B star, from the super-giant itself, and from the hydrogen cloud which surrounds the whole system. Because of the orbital movement of the B star and its disk, we have to expect a certain variability of the radial velocity (dependently of the orbit) of the central absorption core.
(see the attached radial velocity plot). That's why we can observe a corresponding variation of the V/R ratio (see the attached V/R montoring).
The question is, is there in addition a further influence on the V/R ratio? There is a statement from a professional astronomer, that the violett component (V-peak) has been always stronger than the red component (R-peak) of the profile. If so, why? A larger density (or temperature) of the accretion disk in the area, which rotates in the line of sight towards us?
Ernst
