Notices of the proceedings at the meetings of the members of the Royal Institution of Great Britain with abstracts of the discourses . the screen,which is the red end of the spectrum; and they remain there uutilwell after the second minimum, as seen on the 26 successive periodicdates, including the date of 6-20, which is 9 hours after the secondminimum. It is not until 17 hours after this minimum that weagain find the spectrum as it was at the first eclipse, viz., a broadbright line divided by a fine dark line, and the other hydrogen and 440 The Rev. Walter Sidgreaves [Jan. 22, helium lines si
Notices of the proceedings at the meetings of the members of the Royal Institution of Great Britain with abstracts of the discourses . the screen,which is the red end of the spectrum; and they remain there uutilwell after the second minimum, as seen on the 26 successive periodicdates, including the date of 6-20, which is 9 hours after the secondminimum. It is not until 17 hours after this minimum that weagain find the spectrum as it was at the first eclipse, viz., a broadbright line divided by a fine dark line, and the other hydrogen and 440 The Rev. Walter Sidgreaves [Jan. 22, helium lines single and dark. This is the second spectral conjunc-tion, and, unlike the first, it is retarded on the stellar conjunction,which of necessity occurs at the time of least light; and the retarda-tion is about 24 hours, between the periodic dates of 7-4 and 7-19. ^Hax vetocify and ~Max fJjbectra/ c?isb(£ -4-cj S -X ^ S2- of £c/if9Scs 7 I jSfef/ar &/J/^ec/ra/Co ri/unc/zon V \ ^fcx velocity *J%a x jff>ec/?cc / a?t\rfe££7ne:rr,f -&fax coTnJsonP^J/^/occ/l/ -f- 4. < Tx * /S7s f/a r COT2yteric/eorz / arte? 2. We have here direct indication of elliptical motion, as may beseen in the diagram projected on the screen. Suppose an elliptic orbitof a star S about another star occupying the focus nearer to Earth, t Kambaut, On the Parallax of the Double Stars/ Monthly Notices, ,vol. 50, p. 305. 190-4.] on Spectroscopic Studies of Astroplujsical Problems. 441 and the major axis inclined, in the plane of the orbit, to our line ofsight, represented by the arrow-headed parallel lines. The lineSL S2 is the line of eclipses, or stellar conjunctions, and the twolines of sight drawn normals to the curve are the two lines ofspectral-conjunction, when the star is moving in the tangent at rightangles to the sight-line. It is obvious that the excentricity of theellipse and the inclination of the axis may be such an to leave nomeasurable time-interval between the stellar and spect
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