three seconds in length or breadth) will be more readily detected than by any other method,” see Plate 7; “as also will any faculae, mottling, or in short, any other phenomena that may then be existing on the disc.”  “Drifting clouds frequently sweep by, to vary the scene, and occasionally an aerial hail- or snow-storm.”  Mr. Howlett has more than once seen a distant flight of rooks pass slowly across the disc with wonderful distinctness, when the sun has been at a low altitude, and likewise, much more frequently, the rapid dash of starlings, which, very much closer at hand, frequent his church-tower.”

An eclipse of the sun, or a transit of an inferior planet, is also much better seen in this way than by any other method of observing the solar disc.  In Plate 7 are presented several solar spots as they have appeared to Mr. Howlett, with an instrument of moderate power.  The grotesque forms of some of these are remarkable; and the variations the spots undergo from day to day are particularly interesting to the thoughtful observer.

A method of measuring the spots may now be described.  It is not likely indeed that the ordinary observer will care to enter upon any systematic series of measurements.  But even in his case, the means of forming a general comparison between the spots he sees at different times cannot fail to be valuable.  Also the knowledge—­which a simple method of measurement supplies—­of the actual dimensions of a spot in miles (roughly) is calculated to enhance our estimate of the importance of these features of the solar disc.  I give Mr. Howlett’s method in his own words:—­

“Cause your optician to rule for you on a circular piece of glass a number of fine graduations, the 200th part of an inch apart, each fifth and tenth line being of a different length in order to assist the eye in their enumeration.  Insert this between the anterior and posterior lenses of a Huygenian eye-piece of moderate power, say 80 linear.  Direct your telescope upon the sun, and having so arranged it that the whole disc of the sun may be projected on the screen, count carefully the number of graduations that are seen to exactly occupy the solar diameter....  It matters not in which direction you measure your diameter, provided only the sun has risen some 18 deg. or 20 deg. above the horizon, and so escaped the distortion occasioned by refraction.[16]

“Next let us suppose that our observer has been observing the sun on any day of the year, say, if you choose, at the time of its mean apparent diameter, namely about the first of April or first of October, and has ascertained that” (as is the case with Mr. Howlett’s instrument) “sixty-four graduations occupy the diameter of the projected image.  Now the semi-diameter of the sun, at the epochs above mentioned, according to the tables given for every day of the year in the ‘Nautical Almanac’ (the same as in Dietrichsen and Hannay’s very useful compilation) is 16’ 2”, and consequently his mean total diameter is 32’ 4” or 1924”.  If now we divide 1924” by 64” this will, of course, award as nearly as possible 30” as the value in celestial arc of each graduation, either as seen on the screen, or as applied directly to the sun or any heavenly body large enough to be measured by it.”