COMMISSION 27 OF THE I.A.U.
                 INFORMATION BULLETIN ON VARIABLE STARS
                             Number 2989

                                                       Konkoly Observatory
                                                       Budapest
                                                       23 February 1987

                                                       HU ISSN 0374 - 0676


            SPECTROSCOPIC DISCOVERY OF AN ERUPTIVE AND
          TWO PROBABLE LATE-TYPE EMISSION-LINE VARIABLES

The following stars, of presumed interest to variable star
observers, were discovered on 75 minute exposure (baked Kodak IIIa-J
emulsion) objective-prism plates (1360A mmE-1 at H_gamma) taken for the Case
Low-Dispersion Northern Sky Survey (see Pesch and Sanduleak, 1983).

  1. alpha = 10h52m18s.9, delta = +37d15.8' (1950). On a plate taken on
5 May 1981, the spectrum is that of a 14th magnitude, moderately blue
early-type star with very weak hydrogen absorption lines. However,
inspection of the Palomar Sky Survey (POSS) prints shows only a 19th
magnitude stellar image at this position. Thus, this would appear to
be some type of eruptive variable which underwent at least a 5 mag.
outburst.

  2. alpha = 10h45m16s.9, delta = +52d34.4' (1950). On 14 Jan. 1983, the
spectrum is that of a late K or early M-type star with strong Balmer
series emission seen down to at least H_epsilon and a very strong ultraviolet
continuum. The star seems to have a comparable apparent magnitude of
B ~16.5 on both the objective-prism plate and the POSS O print. The
image diameters on the POSS O and E prints yield an estimate of
B-V ~+1.0. Such stars are only rarely noted in our survey; the
only other case (involving a flare star) was reported by Sanduleak
(1983). Not a known proper motion star.

  3. alpha = 16h30m33s.0, delta = +53d33.6' (1950). Involved here is a
physical double (~3 arc seconds separation) of two comparable brightness 
(B ~16 mag.) late K or early M-type stars. The easternmost
and slightly fainter component (to which the above coordinates apply)
alone displays, on a plate taken 23 May 1984, the H and K Lines of Ca II
in emission with extraordinary strength, i.e. the strongest yet seen at
this dispersion by these observers. Neither star shows evidence of the
Balmer series in emission nor any indication of an abnormally strong
uv continuum. This pair does not appear to have been detected in proper
motion surveys.


                       PETER PESCH
                       N. SANDULEAK

                 Warner and Swasey Observatory
                Case Western Reserve University
                   Cleveland, Ohio, U.S.A.


References:

Pesch, P., and Sanduleak, N. 1983, Ap. J. Suppl., 51, 171. [BIBCODE 1983ApJS...51..171P ]
Sanduleak, N. 1983, I.B.V.S., No. 2433.