Basic data (System:307)

C1900.0 :05097-0819
C2000.0 :051432272-08120591
Comp. :B
Magn. : 6.67
Spect. :B9


Identifiers:

Bayer $\beta$ OriBD -08 1063HIP 24436


Orbit

ElementValueStd. dev.
Period (d.):9.860
Periastron time (xJD-2,400,000.0):29633.196
Eccentricity:0.1
omega primary (deg.):10.
K1 (km/s):25.0
K2 (km/s):32.6
V0 (km/s):+19.1
sigma residuals primary:
sigma residuals secondary:
#RV primary:
#RV secondary:
Grade:2.0
Contributor:DAO
Status:PUB
Bibcode:1942ApJ....95..421S
Derived quantities (on the fly, from the above quantities)
a1sini (km):3.37263e+060
a2sini (km):4.39791e+060
m1sin**3 i (sol.mass):0.1092580
m2sin**3 i (sol.mass):0.08378710

Note

Fainter component (BC) of beta Ori (A.D.S. 3823, at least a quadruple system).
Separation from beta Ori A is 9.5" and the pair seems to be a
common-proper-motion pair. This fainter component has been suspected of visual
duplicity (separation always less than 0.2"), but since its two subcomponents
are apparently equal in magnitude, it is difficult to reconcile these
observations with the failure to observe any spectrum of C. Star C cannot be
identified with the star producing the secondary spectrum of the spectroscopic
pair. The bright component, beta Ori A, has been suspected of being a binary
and an orbit was derived by J.S. Plaskett (Astrophys. J., 30, 26, 1909). In
view of the small amplitude (3.8 km/s), however, and the known tendency of
supergiants to display random atmospheric motions, it seems unlikely that this
star is a real binary (see R.F. Sanford, Astrophys. J., 105, 222, 1947).

Plot

Orbit
Encapsulated PostScript file

D.Pourbaix

Valid HTML 4.01 Transitional