But, undoubtedly, for the possessor of a moderately good telescope there is no way of viewing the sun’s features comparable to that now to be described, which has been systematically and successfully applied for a long series of years by the Rev. F. Howlett.  To use his own words:  “Any one possessing a good achromatic of not more than three inches’ aperture, who has a little dexterity with his pencil, and a little time at his disposal (all the better if it be at a somewhat early hour of the morning)” may by this method “deliberately and satisfactorily view, measure, and (if skill suffice) delineate most of those interesting and grand solar phenomena of which he may have read, or which he may have seen depicted, in various works on physical astronomy."[15]

The method in question depends on the same property which is involved in the use of the pyramidal box just described, supplemented (where exact and systematic observation is required) by the fact that objects lying on or between the lenses of the eye-piece are to be seen faithfully projected on the white surface on which the sun’s image is received.  In place, however, of a box carried upon the telescope-tube, a darkened room (or true camera obscura) contains the receiving sheet.

A chamber is to be selected, having a window looking towards the south—­a little easterly, if possible, so as to admit of morning observation.  All windows are to be completely darkened save one, through which the telescope is directed towards the sun.  An arrangement is to be adopted for preventing all light from entering by this window except such light as passes down the tube of the telescope.  This can readily be managed with a little ingenuity.  Mr. Howlett describes an excellent method.  The following, perhaps, will sufficiently serve the purposes of the general observer:—­A plain frame (portable) is to be constructed to fit into the window:  to the four sides of this frame triangular pieces of cloth (impervious to light) are to be attached, their shape being such that when their adjacent edges are sewn together and the flaps stretched out, they form a rectangular pyramid of which the frame is the base.  Through the vertex of this pyramid (near which, of course, the cloth flaps are not sewn together) the telescope tube is to be passed, and an elastic cord so placed round the ends of the flaps as to prevent any light from penetrating between them and the telescope.  It will now be possible, without disturbing the screen (fixed in the window), to move the telescope so as to follow the sun during the time of observation.  And the same arrangement will serve for all seasons, if so managed that the elastic cord is not far from the middle of the telescope-tube; for in this case the range of motion is small compared to the range of the tube’s extremity.

A large screen of good drawing-paper should next be prepared.  This should be stretched on a light frame of wood, and placed on an easel, the legs of which should be furnished with holes and pegs that the screen may be set at any required height, and be brought square to the tube’s axis.  A large T-square of light wood will be useful to enable the observer to judge whether the screen is properly situated in the last respect.