b Lyrae is a double in eclipse. The system is formed by two stars bigger than the Sun; a with a superficial temperature of 11.000 C., and therefore, of white blue color, on the other hand, the secondary has a temperature inferior superficiality to the 6.000 C., corresponding to the white color; both turning in 12d. 22h. 22m. The centers of masses of both stars separate in 16,000,000 Kms., one of the other, the total mass of the system is 30 times the sun.
The two globes present strong deformations, being ovoids like consequence of the reciprocal attraction; the diameter of the older star is of 17 million Km. and of 12 the minor, the half distance between the two globes is of only 2 million Kms.
The interaction between the gravitatorial fields of the two stars is such, that a continuous exchange of matter takes place, which it flows through two gas currents that pass touching the neuter point. This matter forms two rings that surround to the globes and lies in the orbital plane, but a part of the gases escapes from the gravitational fields of the System disappearing for the interestelar space, given the rotational speed of the system, it's deduced that this gas disappears in hairspring.
This gas is formed mainly by H excited for the intense ultraviolet radiation of the hottest star; espectropicaly, this gas gives the typical lines of the series of Balmer.
I began to observe b lyrae June 13th of 1984 concluding the study July 1st of the same year, I like consequence of climatological adverse conditions could not carry out the mensurations the days 18, 19 and 24 of June; but it was not obstacle in order to achieve an appreciated curve of light.
b lyrae varies 3.3 4,2 between the magnitudes; when both stars are not eclipsed the combined magnitude is of 3,3; when the main eclipse takes place, one of the two stars remains almost completely occult, and the combined low shine until the magnitude 4,2; on the contrary, when a secondary eclipse takes place, the concealment is partially and the magnitude goes down to the value of 3.7 denominated secondary minimum. There is not neither a single moment in which b Lyrae has the same magnitude and color.
In order to carry out the curve of light me I base on the following stars with their magnitudes like pattern of their curve of light.
g lyrae: 3,3 z lyrae: 4,1 i lyrae: 4,3 h lyrae: 4,5
The more used was g lyrae due to their magnitude since it coincides with the maximum of the variable, and z lyrae by approaching to the main minimum.
The observation of the variable was daily between the 21h.00m. and 21h.30m. U.T.; the used method was the Argelander, simple and effective. Using some primástics Vixen, 7x50mm.
Next I am going to expose the comparisons carried out during the observation.
|INSTR.||Mag. A||Mag. B||A||B||Mv||CM||C||Mag. A||Mag. B||A||B||Mv||CM||C|
Three nigths without observations by clouds. Light of curve apreciate.
1: High comparation
2: Medium comparation
3: Dubte comparation
C: Atmospherical conditions
CURVE OF LIGHT
Masm(Last update 10.17.2003)