|Spect.||:||K0III ; F|
|Bayer $\alpha$ UMa||BD +62 1161||HD 95689||HIP 54061|
|Periastron time (xJD-2,400,000.0)||:||18636.2|
|omega primary (deg.)||:||174.|
|sigma residuals primary||:|
|sigma residuals secondary||:|
|Derived quantities (on the fly, from the above quantities)|
This system is A.D.S. 8035 with Delta m close to 3m. Underhill adopted the orbital elements by H.S. Jones and H.H. Furner (Mon. Not. Roy. Astron. Soc., 98, 92, 1937) with P=44.0y, T=1865.9. She also assumed their values of e and omega and derived K and V0 only. The orbital inclination is 161. deg. The visual orbit by W.D. Heintz (Munchen Veroff., 5, 247, 1963) is now considered superior to that by Jones and Furner although the predictions of the two orbits about radial velocities during the interval of observation are similar. C.D. Scarfe (Astrophys. Space Sci., 11, 112, 1971) has shown that the observed velocities do not agree well with either of these orbits, or even with that derived by P. Couteau (J. Observateurs, 42, 31, 1959). Visual observers are hampered by the very close approach of the two stars at periastron. This is just the time when the radial velocities will be able to give most information, but the next approach, according to Heintz' values of the elements will be about the year 2000. All elements should be considered uncertain until then.