By Don Freeman
As he and his buddies prepare to rejoice Easter with a different occasion, Corduroy wonders if the Easter Bunny is actual.
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Extra info for Corduroy's Easter Party
L.. . 0 . :- : 88 89 I. +]1- 08 09 80 81 82 83 84 85 86 87 AO Fig. 13. The HR-diagram for B stars according to the Victoria system of spectral classification and absolute magnitude. or less uniformly over a range of some five magnitudes. This material does not define a distinctive main sequence for stars of type 09 to B2. The observed dispersion about a main sequence is less for stars of type B3 and later and corresponds more closely to the dispersion expected according to the uncertainties of the method.
This relation could be put in explicit form by using the relationship derived by UNSOLD (1942b) between W (Ry) and log Pe, but such a relation would have little real meaning, for the generalisations that are made to obtain UnsOld's formula are too sweeping to be valid in all early type stellar atmospheres. More recently PETRIE (1964) has examined anew the problem of calibrating the equivalent width of Hy in terms of absolute magnitude in the case of stars of spectral types 06 to A3. He has assembled a series of homogeneous measurements of W(Hy) in the spectra of 166 early type stars belonging to the Pleiades, the IX Persei cluster, NGC 2244, and to the association I Orionis and that around h and X Persei.
Since it is difficult to obtain accurate distances for distant objects, it is difficult to find standard B type stars of known luminosity. 17 Arjr. 2 magnitude, the distance must be known to within ten per cent. 2 magnitude. Many of the interesting groups of 0 and B stars appear to have distances of 1000 to 2000 parsecs. 2 magnitude, the positions in space of these stars are not known within a matter of some 100 to 200 parsecs. Such uncertainties in distance are not small when one thinks in terms of the diameters of aggregates such as open clusters or even associations.