COMMISSION 27 OF THE I.A.U.
              INFORMATION BULLETIN ON VARIABLE STARS
                           Number 1212

                                             Konkoly Observatory
                                             Budapest
                                             1976 December 2


            COPERNICUS OBSERVATIONS OF THE
          NON-ECLIPSING RS CVn BINARY HR 1099

Photoelectric spectrum scans of the Mg II h&k and Lyman-
alpha emission lines of HR 1099 were obtained in September, 1976
with the ultraviolet spectrometers aboard COPERNICUS (Rogerson
et al. 1973). Both spectral regions were scanned continuously
throughout two complete orbital cycles. The resolution at Lyman-
alpha was 5 m A while that at Mg II was 510 m A.
   Both the Mg II and Lyman-alpha emission features exhibited
marked profile and intensity variations over short time scales
of less than five hours. In addition, multiple Mg II velocity
components (+-200 km/s) were observed to appear and disappear
over similar intervals. The velocity direction of these components 
was correlated to the orbital motion of the secondary star,
that is, they were usually negative when the secondary was 
approaching the observer, and positive when receding. This result
may imply mass transfer from the primary to secondary star in
this system. Since the strongest feature was usually observed
with the same velocity as the primary, this component is likely
the more active star. In addition, Bopp and Fekel (1976) have
found the primary to be the main source of the Ca II H&K and
H-alpha emission observed in HR 1099.
   Although the Lyman-alpha profiles were too noisy in most
cases to allow detection of multiple velocity components, a
good correlation was found between the relative strength of the
emission and orbital phase. Strongest emission was usually 
observed around phase (ORB) 0.35 while weakest emission was 
usually found near phase (ORB) 0.85. The phase of maximum emission
intensity agrees well with that found for the minimum of the
photometric distortion wave (phase (ORB) 0.38) by Bopp et al.
(1977). This result is in good agreement with similar emission-
wave correlations found in other RS CVn binaries by Weiler (1975),
Mulligan and Bopp (1975), and Bopp (1976).
   Hall (1972) has hypothesized that similar photometric 
distortion waves in other RS CVn binaries are produced by starspot
concentrations in preferred longitudes on the active star. This
concept of preferred longitudes of activity has its solar precedent 
as reported by Bumba and Howard (1965) and Dodson and Hedeman 
(1968). The aforementioned correlations support Hall's model
as the plage and flare activity necessary to produce chromospheric 
emission lines would likely be concentrated in similar
longitudes. Extensive and variable chromospheric activity is
also indicated by Owen's (1976) recent observations of solar-
type radio emission from HR 1099.
   Analysis of the current data is continuing and a more 
detailed report of this research and additional studies of UX Ari
will appear elsewhere. This study was conducted as part of an
international project aimed at monitoring chromospheric activity
in HR 1099 and UX Ari. The project consisted of coordinated 
satellite UV spectrophotometry as well as radio, UBV photometry,
H-alpha and Ca II H&K, and polarimetric observations. Analyses of
the combined data set will begin shortly, and any reports of
additional observations of these two systems during 1976 would
be greatly appreciated.
   The satellite research discussed in this note was supported
by the National Aeronautics and Space Administration.


                                   EDWARD J. WEILER

                                   Princeton University Observatory
                                   Peyton Hall
                                   Princeton, New Jersey 08540



References:

Bopp, B.W. 1976, I.B.V.S. 1175
Bopp, B.W., Espenak, F., Hall, D.S., Landis, H.J., Lovell, L.P., and
   Reucroft, S. 1977, Astron. Jour., in press [BIBCODE 1977AJ.....82...47B ]
Bopp, B.W. and Fekel, F. 1976, Astron. Jour. 81, No. 9, 771 [BIBCODE 1976AJ.....81..771B ]
Bumba, V. and Howard, R. 1965, Astrophys. Jour. 141, 1492 [BIBCODE 1965ApJ...141.1492B ]
Dodson, H.W. and Hedeman, E.R. 1968, IAU Symposium No. 35, Structure and
   Development of Solar Active Regions, 56 [BIBCODE 1968IAUS...35...56D ]
Hall, D.S. 1972, Publ.Astron. Soc. Pac. 84, 323 [BIBCODE 1972PASP...84..323H ]
Mulligan, K. and Bopp, B.W. 1975, I.B.V.S. 1075
Owen, F.N. 1976, IAU Circ. No. 2929 [BIBCODE 1976IAUC.2929....2O ]
Rogerson, J.B., Spitzer, L., Drake, J.F., Dressler, K., Jenkins, E.B.,
   Morton, D.C., and York, D.G. 1973, Astrophys. Jour. (letters), 181, L97 [BIBCODE 1973ApJ...181L..97R ]
Weiler, E.J. 1975, I.B.V.S. 1014