IV.—On a method of comparing the light of the sun with that of the fixed stars
One of the most ingenious contributors to the Transactions of our Society in the last century, the Rev. John Michell, in a paper intituled “An inquiry into the probable parallax and magnitude of fixed stars, &c*.” has proposed it to astronomers, as an object worthy their attention, to determine what proportion the light, afforded us separately by each fixed star, bears to the light which we receive from the sun; since, from our inability to measure the annual parallax of those very remote bodies, such a comparison is the best, perhaps the only method within our reach, of obtaining, though not certain, yet probable estimates of their distances; and thus forming reasonable conjectures concerning the extent of the visible universe. In order that we may judge, with the least chance of error, of the mean distance of those stars which are the nearest to the earth, he directs us to compare the light of the brightest stars with that of the sun, and next to calculate how far the sun must be removed, to make the light that we should then receive from him, not more than equal to the mean light of the stars chosen for comparison. Mr. Michell made, as he says, some rude experiments for determining the comparative brilliancy of certain principal stars; but has not suggested any contrivance for comparing a star with the sun. He states, however, so distinctly the great object of such a comparison, and the inferences which an industrious observer would thence be entitled to draw, concerning the distances of those stars whose light he might succeed in measuring, that it is surprising that no astronomer has been incited by these remarks to devise a method of making the requisite observations, and that now, so many years after Mr. Michell’s suggestion was made public, so much remains to be effected in this branch of photometry.