Basic data (System:226)

Identifiers:

Orbit

Note

This system has attracted attention since its discovery as a flaring radio
source (R.M. Hjellming and C. Wade, Nature, 242, 250, 1973). Orbital elements
were published nearly simultaneously by R. Rajamohan and M. Parthasarathy
(Pramana, 4, 153, 1975, Kodaikanal Preprint, No. 74), S.C. Wolff and R.J.
Wolff (Publ. Astron. Soc. Pacific, 86, 176, 1974) and the authors cited in the
Catalogue. Older observations (J.F. Heard, Astrophys. J., 87, 72, 1938, W.E.
Harper, Publ. Dom. Astrophys. Obs., 4, 309, 1930 and J.B. Cannon, Publ. Dom.
Obs., 1, 285, 1911) were included by Hill et al. in their discussion of the
long-period orbit. Since the publication of the Seventh Catalogue a further
study of the short-period orbit has been published by H.W. Duerbeck and A.
Schettler (Acta Astron., 29, 225, 1979). Their results confirm those of Hill
et al. and they also find the systemic velocity to be roughly in agreement
with expectations from the long-period orbit. Their photometric observations
show the short-period system to be an ellipsoidal variable. There is a
possibility that the third body eclipses the primary star. Only one spectrum
is visible and Duerbeck and Schettler did not find any effects of blending in
the hydrogen lines, as were suspected by Hill et al.. Duerbeck and Schettler
suggest that the secondary is an F5 subgiant. Rotational broadening of the
only visible spectrum makes accurate measurement of velocities difficult.

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