COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                     Number 1676

                                     Konkoly Observatory
                                     Budapest
                                     1979 September 25




  SPECTROGRAPHIC OBSERVATIONS OF THE SUSPECTED DELTA SCUTI
            VARIABLE STAR 2 LYNCIS (HR 2238)



   In a recent paper (Antonello et al., 1978) we have published
the results of eighteen spectrographic observations of the suspected 
variable star 2 Lyn, obtained with the Zeiss prism spectrograph
of the Merate Observatory. The equivalent width (W_lambda) and the radial
velocity (RV) of spectral lines of this star were found to be variable, 
with a period of about 0.04d for the RV, and 0.3d for the W_lambda.
Moreover smaller variations of W_lambda, superimposed on the greater
ones and partially in accordance with the RV were found.
   At the beginning of 1978 thirteen new spectra of 2 Lyn were
taken with the electronic camera of the Astronomical Observatory
of Haute Provence (Reseau holographique, dispersion: 18.7 A/mm;
152 cm telescope). Unfortunately the spectra are slightly under-
exposed. The methods of reduction are the same as in the previous
paper, and the values obtained are listed in Table 1. The Figures 1
and 2 show the new results compared with some of the old ones 
reported in the previous paper.

                     Table 1
       
        J.D.   RV (Km/s)        W_lambda(A)   W_lambda(A)
            MgII lambda4481   MgII lambda4481  H_gamma

2443519.332    -8.3                 0.42       14.11
       .344    15.5                 0.87       14.80
       .359     7.1                 0.62       13.68
       .371   -15.2                 0.48       13.75
       .387     6.7                 0.76       12.61
       .398   - 5.0                 0.50       14.94
       .414   - 0.7                 0.40       12.76
       .426     0.9                 0.46       13.18
       .441     1.7                 -           -
       .457    13.4                 0.41       15.05
       .469   - 3.2                 0.48       12.52
       .484   - 6.7                 0.48       13.25
       .496     2.9                 0.43       14.96


                         [FIGURE 1]

 Fig. 1.  Radial velocities and equivalent widths of H_gamma line
          versus Julian Days.

                         [FIGURE 2]

 Fig. 2.  Radial velocities and equivalent widths of Ca II - K
          and Mg II lambda4481 lines versus Julian Days.


    As regards the short period variations, one can see that
the present results are in agreement with the old ones, both for
RV and for W_lambda. However, these results are not sufficient to
confirm (but neither to exclude) the longer period variation.





           E. ANTONELLO, M. FRACASSINI and L.E. PASINETTI
           Osservatorio Astronomico di Milano - Merate
           Via Brera n. 28, 20121 Milano, Italia





Reference :
Antonello, E., Arienti, F., Fracassini, M., Pasinetti, L.E.,
        1978, Astron. and Astrophys., 66, 37 [BIBCODE 1978A&A....66...37A ]