IBVS - KONKOLY OBSERVATORY, BUDAPEST, HUNGARY - ABOUT THIS DOCUMENT


COMMISSIONS 27 AND 42 OF THE IAU
INFORMATION BULLETIN ON VARIABLE STARS
Number 3337


Konkoly Observatory
Budapest
13 June 1989
HU ISSN 0374 - 0676

SAO 139 174 IS AN ECLIPSING BINARY STAR

R. CASAS (1,2) J.M. GOMEZ-FORRELLAD (1)

(1) Grup d'Estudis Astronomics, Apdo. 9481, 08080 Barcelona, Spain

(2)Instituto de Astrofisica de Canarias, 38200-La Laguna (Tenerife), Spain


SAO139174 (BD -1d2777 = HD 114125) was used as a check star during the observations performed on 18 and 19 March 1988 at Sierra Nevada Observatory in Spain. The star howed brightness variations which suggested that it might be an eclipsing binary (Rodriguez et al., 1988).

During 18 nights, from March 21 to April 22, 1989, SAO 139174 was observed using a solid state photometer attached to the Cassegrain focus of the 0.5 m Mons telescope at Observatorio del Teide (Instituto de Astrofisica de Canarias Canary Islands, Spain).

SAO 139171 was used as comparison 1, and SAO 139131 (48 Vir) as comparison 2, while SAO 139086 (44 Vir), SAO 139139, SAO 139186, and SAO 139196 as check stars.

HY_vir.gif (4411 bytes)
[Fig. 1.]

 

The results of this surveillance program proved that SAO 139174 is an eclipsing binary star with a period close to 2.73 days. The star is a 7.81 magnitude (V) object at the maximum light that fades to 8.10 and 8.05 at the primary and secondary minima respectively. The eclipses last about 6.3 hours. Figure 1 shows the light curve obtained.

From our set of data we computed the tentative ephemeris for the primary minimum:

HJD = 2447240.97128 + 2.73236d E
             +-0.00006 +-0.00002

After a quick first analysis of the light curve using the Russell-Merrill model according to Irwin (1962) we obtained the following elements:

R_s=0.15 L_s=0.423

R_g=0.19 L_g=0.577

i=80.1deg

Additional photometric data are needed in order to compute more precise elements and ephemeris for this new binary system.

We would like to acknowledge the Instituto de Astrofisica de Canarias for allowing us to utilize their facilities. We would like to acknowledge also C. Gallart for her assistance in the observation during some nights, and E. Garcia-Melendo for his help in computing the elements of the system. 

 

References:

Rodriguez, E., Sedano, J.L., Lopez de Coca, P., and Rolland, A. 1988, Inf. Bull. Var. Stars, No. 3174.

Irwin, J.B. 1962, in "Astronomical Techniques", Univ. of Chicago Press, p. 584.