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X. Self Love.

XI. Love of Popularity.

XII. Caution.

XIII. Benevolence or Gentleness.
XIV. Superstition or Bigotry.
XV. Ardent Expectation.
XVI, Imagination.
XVII. Love of Justice.
XVIII. Firmness.

INTELLECTUAL POWERS.
XIX. Discrimination of Objects.
XX. Discrimination of Forms,
XXI. Discrimination of Bulks.
XXI. Discrimination of Weights.
XXIII. Discrimination of Colours.
XXIV. Discrimination of Localities.
XXV. Discrimination of Method.
XXVI. Discrimination of Time.
XXVII. Power of Calculation.
XXVIII. Discrimination of Sounds.
XXIX. Power of acquiring Languages.

REFLECTIVE POWERS.

XXX. Reasoning or Comparing.
XXXI. Investigation.
XXXII. Wit.

XXXIII. Power of Imitation.

For many curious details, Dr. Spurz beim's Lectures, or his published volume, merit attendance or perusal. The dis tinctions bere enumerated are evidently too numerous. Nature at most designates only the GENERA of natural powers, and not the species of social affections. It is, however, due to Drs. GALL and SPURZHEIM to admit that they have greatly improved our knowledge of the anatomy of the brain; and the credit they have acquired in that particular, entitles their inferences in other respects to the attention of the learned and scientific.

To the Editor of the Monthly Magazine. SIR,

IN

N your Magazine for January, I per ceive that Mr. George Douglas has ready for the press, "A Treatise upon the Light and Heat of the Planets, in

which he purposes to shew that each of them possesses the same degree of light and beat which our earth does."

Amidst the doubts and ignorance which still prevail respecting the nature of light, and the new investigations and experiments which have lately been made by philosophers on this subject, it would, perhaps, be too presumptuous to assert, that it is impossible to prove. the position which Mr. Douglas proposes to support! Without at all pre-judging the result of this gentleman's disquisitions, it may, however, in the mean time, be allowed Ito suggest an objection to one of the arguments brought forward in support of the opinion, "that the planets possess the same degree of light which our earth does." In the notice referred to, it is stated (doubtless as a presumptive argument in favour of his hypothesis) that, "when the planets appear together, Jupiter is but little inferior in brightness to Venus or Mercury, and Venus not inferior to Mercury; the same may be said of Saturn and Mars, which, when each of them is nearest to the earth, are equally bright." On this circum stance, considered as an argument, pers init me to offer the following remarks :—

In the first place, when the heavenly. bodies are viewed in the night time, in the absence of the moon, by the naked eye, though a slight diversity of colour and brilliancy appears among them, the difference of their brightness, when at a considerable elevation above the horizon, is not very great, except in so far as de pends on their apparent magnitudes. The difference, however, in point of brilliancy, between Venus and Saturn, and even between Venus and Jupiter, is quite obvious and striking. But it is presumed that no certain conclusions can be deduced in regard to the degree of light on the surfaces of the respective planets, from their appearance, during night, to the naked eye; for they appear almost like shining points, and present no well-defined surface or disk, to the unassisted sight. A more just and accu rate conclusion may be drawn from their appearance through telescopes of considerable magnifying power, when a large surface is exhibited to the eye. When Jupiter is viewed with a good telescope of considerable power, his surface and margin appear well-defined, and with mild degree of lustre; whereas Venus, at certain times, particularly about the period of her greatest elongation, when viewed with a similar telescope, exhibits such a brisk glaring appearance, that her

2815.] Mr. Dick on the Light and Heat of the Planets.

disk presents an undefined aspect, and her margin, and the boundary between her dark and enlightened hemisphere, cannot be accurately distinguished.Hence it is frequently found necessary to contract the aperture of the objectglass of the telescope, in order to dimi nish the intensity of her light; and, for the same reason, some astronomers, when viewing this planet, have used a smoked glass next the eye; which precautions are never found necessary in viewing Mars, Jupiter, or Saturu. This circumstance, of itself, seems to form a presumptive proof that the degree of light on Venus is greater than that on the surface of Jupiter.

"But what I consider as still more conclusive, and as forming the principal objection to the opinion now under consideration, is, the different degrees of brilliancy exhibited by the planets, when viewed in the day-time, which is pecularly striking. On this point I beg leave to quote a passage from a communication I some time ago transmitted to Nicholson'sPhilosophical Journal, entitled "Observations on the celestial bodies, made in the day-time, particularly on the planet Venus, with some new deductions in relation to that planet," inserted in the Journal for October 1813. "Though Jupiter, when at, and near, his oppost tion to the sun, appears to the naked eye with a brilliancy nearly equal to that of Venus, yet there is a very striking difference between these two planets, in respect of lustre, when viewed in daylight. Jupiter, when viewed with a high magnifying power, in the day-time, always exhibits a very dull cloudy ap pearance; whereas Venus appears with a moderate degree of splendour. About the end of June, 1813, between five and six in the evening, the sun being nearly three hours above the horizon, having viewed the planet Venus,then within 200 of the sun, aud which appeared with a moderate degree of lustre, I directed the telescope to Jupiter, at that time more than 320 from the sun, when the contrast between the two planets was very striking, Jupiter appearing so faint as to be but just discernible, though his apparent magnitude was more than

195

double that of Venus. In this observa tion a magnifying power of 60 times was used. In his approach towards the sun, about the end of July, I could not perceive him when he was within 25° or 26° of his conjunction with that lumi nary. These circumstances furnish sensible and popular proof, independent of astronomical calculations, that Jupiter is removed at a much greater distance from the sun than Venus, since his fight is so faint as to be scarcely perceptible when more than 200 from the sun, while that of Venus is distinctly seen amidss the full splendour of the solar rays.'

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The observation above referred to was made in the presence of several persons, some of whom were not much accustomed to look through telescopes; they all perceived Venus distinctly, as soon as they applied their eye to the telescope; but it was with some difficulty, and not till after several trials, that they could distinguish Jupiter. I have had several opportunities of making similar observations since that time, and they have uniformly produced similar results. Some weeks after Jupiter's last conjunc tion with the sun, which happened on September 14, 1814, I endeavoured to ascertain how near that luminary he might be seen; but I could not perceive him in the day-time, when he was near the meridian, till October 22, when he was somewhat more than 290 in longitude distant from the sun; and, even then, he appeared extremely faint, though, at the time of observation, he was more than 250 in altitude. December 5, I perceived Venus, when near the meridian,about 40′ past 11,A.M. when her elevation above the horizon was only about 129; and also, on the same day, betwixt 9 and 10 o'clock,A.M. when her altitude was little more than 50; in both cases she appeared more vivid and distinct than Jupiter, on October 22. She was then only about 50 distant from the sun; and, had not the state of the weather prevented further observations, she would probably have beeu seen, when much nearer the sun, notwithstanding her low altitude. In these observations there was no opake body interposed to intercept the direct solar rays. When we consider the difficulty of perceiving the heavenly bodies, when at low altitudes, through the gross vapours near the horizon, the circum

On

Dr. Hooke has observed, "that the

same glass will bear a greater or less apertare, according to the less or greater light of the object. If, for instance, he was viewing the Sun or Venus, he used smaller apertures; but, if he wanted to view the moon by day-light, or Saturn, Jupiter, or Mars, by night, he used a larger Aperture."

* In the paper from which this extract is taken, an observation is stated, in which Venus was distinctly seen when only 29

front the sun's eastern limb,
2C2

stances

same time I may add, that they do not depend on my testimony alone, but some of them could be attested, if requisite, by several respectable characters. That they are not repugnant to the deductions of Mr. Short, who seems to have been among the first who made similar observations, appears from the following extract from his description of the Equatorial Telescope:-" By this instrument most of the stars of the first and second magnitude, have been seen even at mid-day, and the sun shining bright; as also Mercury, Venus, and Jupiter. Saturn and Mars are not so easy to be seen on account of the faintness of their light, except when the sun is but a few hours above the horizon." Methven, near Perth; T. DICK.

Feb. 2, 1815.

To the Editor of the Monthly Magazine:

Ν

SIR,

stances in which Venus was seen, in the observations now stated, were evident ly very unfavourable; yet neither her proximity to the sun, nor the dense atmosphere through which her rays had to penetrate, could prevent her light from being distinguished. In the month of October last, when Saturn was more than 90% from the sun, he could not be perceived till within half an hour or twenty minutes of sun-set, and even then be exhibited a very faint cloudy appear ance, though his apparent diaineter was as great, and his altitude, at the time of observation, as high, as those of Venus in the above-stated observations. Į have never been able to distinguish this planet, in the day-time, even at the time of its opposition to the sun, except a very short time before sun-setting. His great southern declination, at present, and his consequent low elevation above the horizon, it must be acknowledged, are unfavourable for such observations; but the same circumstances were equally unfavourable in the case of Venus, as noted above,

As the above-stated facts are not so litary instances, but specimens of many similar observations which I have frequently made, they seem to furnish a presumptive proof, that the quantity of light on Venus is considerably greater than that on Jupiter and Saturn; and Consequently that the probability lies against the hypothesis which supposes, that they possess the same degree of light as the earth does." Otherwise,why should Jupiter always exhibit such a dull and cloudy appearance, in the day-time, when compared with Venus? Why should the light of this planet be undis tinguishable by day-light when more than 20° distant from the sun, while that of Venus is distinctly seen when she is within 5, and even when within 30 of the body of that luminary? And why should Saturn be so difficult to be distinguished, even in the most favourable positions, if the light of the superior planets be not inferior in degree to the light of Mercury and Venus? If this is not the conclusion to be deduced, it remains with those who adopt a different opinion to account for the phenomena now described, in another way. Should Mr. Douglas be disposed to question the accuracy of the observations here stated, I can only recommend him to repeat the observations himself, in company with any of his friends, whose quids are not warped by an attachment to a favourite hypothesis; and, at the

IN your Magazine for March, under the

term "Aphorisms," it is maintained that the landed property is mortgaged to the public creditor to the extent of the capital of our debt.-This I deny. There is no law, nor was there any bargain at the different periods when our debt was incurred, from which such an inference can be deduced, 1 know well that it is the firm belief of the monied interest that all lands and property are securities for the principal of the public debt. But the really implied security is not on the principal of all property, nor on land in par ticular, nor even on the income derived from land and other property, but merely and burely on the taxes levied from the income of the nation. I say, this is the implied security of the public creditor, and that only for his interest, and not for the principal. For, consider the progress of a loan. The minister borrows from certain monied persons, at a fixed rate of interest, in perpetuity, but under no obligation to repay the principal. The exceptions to this prove my position; for I recollect that the public creditor (for some part of the four or five per cents.) is bound to accept his principal if the stocks rise to a certain height. Now to meet the interest, which the minister engages to pay for the loan of the principal sum, "Ways and Means" are proposed by different taxes. In all this there is pot the slightest allusion to an engage. ment, or mortgage, for even the interest over the land and property of the country.

Whenever therefore the taxes cannot be brought to meet the interest of the public debt, the public creditor must

submit

1815.]

Security of Public Debt.-Boxing Matches.

submit to a diminution of his interest. And his situation is merely that of a perpetual annuitant, whose annuity depends upon the produce of the taxes.

A. B. C.

To the Editor of the Monthly Magazine. SIR,

IT is

Tis offensive to all persons of delicacy to see whole columns of our newspapers occupied with the disgusting details and low slang of boxing-matches; from which foreigners must conclude it to be a subject of the utmost interest and impor. tance to the British public. Boxing ought never to be connived at or permitted, unless it can be proved to have some useful tendency, (instead of exciting a brutal and quarrelsome disposition;) in which case it ought to be more generally encouraged, and not confined to a few individuals of the lowest description.

Those who attend boxing-matches do not reason on the subject, but merely go as to a horse-race for the purpose of betting money; perhaps worse specimens of human nature could not be found than of those who attend such exhibitions. Cockfighting is a most contemptible and cruel amusement; but how much more so is it to hire two human beings, coolly stand. ing by, and barbarously encouraging them to beat and bruise each other, till the "human face divine" is converted in to a hideous piece of deformity, at which humanity shudders! The man who was just before standing erect, in all the pride of his strength, like the " mighty warrior of the race of Fingal," brought by long training to the utmost state of bodily perfection, is in one half hour laid prostrate, fainting with agony, carried away to languish for months on a sick bed, possibly to rise from it no more!

Yet this brutal practice has its advocates; for there is nothing too absurd not to have advocates, particularly if sanctioned by long custom and antiquity. It has even been asserted that bull-baiting is of use to preserve the British character from degenerating and becoming effeminate; but experience has shewn that those people who know nothing of box ing or bull-baiting are quite as brave in the field of battle as those who have been accustomed to practices that are worse than useless, and a national dis VERITAS.

grace.

To the Editor of the Monthly Magazine.

SIR,

REQUEST your readers to believe that I could not say, “I wish we were

197

well rid of the Property Tax, if even at the expence of something as bad or worse.' I know not whether we are not in the wrong of being rid of it on such terms. But, although we often undesignedly change bad for worse, no one wishes such an exchange. It should have been printed, "if not at the expence."

I believe it capable, by reducing to pa litical proportions instead of mere arith metical 10 per cent., wherever it falls, to have received modifications, which may have made it preferable to most other means, perhaps to any, of raising a vast annual sum.

But then Life-Annuities, and, still more, incomes from professions, aud trade or manufactures, ought to have been taxed much more lightly than absolute fixed property, whether real or per sonal; and small property than great. Seeing no prospect of such modifications, I saw no probability of much substantial relief. I think few will say that I was much deceived, or that we are any way near a politic, just, and tolerably-equal system of finance.

Solar Spots.

These are now become conspicuous on each side of the Sun, as it presents itself alternately in about 18 days §.

Apparent Measure of a Degree.

My sight measures the apparent mean diameter of the Sun and Moon at about 6 inches; which I find the Chinese astronomy well corresponds with more than 2000 years back; 100 feet, or tchang, being

100°. This may assist, in a gross estimate, what old Chronicles mean when speaking of Trains of Comets 20 feet or yards long.-Vide Pingré Cometograph, . 1, p. 351, and pp. 572-9. Troston; March 2, 1815.

CAPEL LOFFT.

To the Editor of the Monthly Magazine.

SIR,

N the year 1816 there will be four

I eclipses, two of the O and two of the D. The first is of the on the 27th of May, but invisible in these parts. The second is a total and visible one of the D on the 9th and 10th of June. The third is a large and visible one of the O, which I purpose giving a description of in this paper. The fourth is a partial and visible one of the Don the 4th of December.

The solar eclipse of November 19th will be the largest visible one at London since that of 1764. It will be central

and total in some parts of Europe and Asia, the 's apparent diameter, at its

greatest

.

greatest altitude on the central tract exceeds that of the about 46"; causing an umbrageous tract of one hundred miles, more or lest in breadth, according to the position of the with respect to the horizon.

This eclipse will begin on the O's upper limb at his rising, in lat. 47° 55′ 8" N. long. 10° 51′ 11′′ W., and in a few minutes will be visible over a great extent of country. Before the centre of the enters the earth's disc, the eclipse will be seen at the Azores, Maderias, the British isles, in France, Spain, Germany, &c.

h. m.

The commencement of the central tract will be at 9 34 53, in lat. 66 18′ N. long. 0° 5' F. passing over some parts of Norway, and along the coast of Sweden near the Cattegat, it crosses the Baltic and the island of Bornholm, and, after leaving lat. 54° 32', long. 15° 23′, it will enter Pomerania about 40' after nine, a little to the N. E. of Colberg, continuing its course to lat. 51 14, long. 19° 38' in Prussian Poland; at 46m. after nine it will be very near the town of Cracow; entering Hungary, the central tract will pass over lat. 48° 3', long. 23° 21' to lat. 45° 57', long. 26° 38, where it will leave that country, and enter European Turkey about 55 after nine, cross the Danube near Silistria, and at ten o'clock it will have reached the coast of the Black Sea in lat. 43° 51', long, 29° 10′. The will be centrally eclipsed at noon in lat. 43° 23' 43 long. 29° 42' 30", which happens in the Black Sea, about one hundred and fifty miles N. N. E. of Constantinople; the tract passes over lat. 41° 58', long. 310 25', and enters Asiatic Turkey about 6' after ten; and, in crossing that country, its position will be lat. 40° 8', long. 330 10′, lat. 38° 40′, long. 35° 1', lat. 370 22', long. S7 1', lat. 36° 15', long. 380 56', lat. 35° 7', long. 40° 47', lat. S40 B', long. 42° 39', and lat. 33° 22', long 44° 19' leaving Turkey close to the eity of Bagdad, it enters Persia, at 40m. after ten, near the borders of Arabia. In crossing Persia, the curvature of the central tract will be very considerable. It will pass over lat. 32° 38', long, 46 13, lat. 32o 5', lung. 48° 18', lat. $10 23', long. 50° 32', lat. 31° 6', long. 520 40', lat. 30° 50', long. 55° 28', lat. 300

40', long. 58° 27', lat. 30° 58', long,
62° 11', and lat. 31° 43', long. 66° 41';
quitting Persia at 22 after eleven, it
will enter the northern part of Hindos-
tan, passing over lat. 39°6′, long. 73
S1', and at about 26 after eleven will
reach the extensive empire of China.
Entering the great desert of Cobi, the
central eclipse leaves the earth with the
setting in lat. 35° 54′ 59′′ N. long.
85° 9' 57" E. at 27' 49" after eleven,
A.M. Hence the line joining the cen
tres of the and will describe a
curve on the earth's surface not less
than 4650 geographical miles in 1 52
56. But, owing to the globular form of
the earth, and its diurnal motion on its
axis, combined with the motion of the
in her relative orbit, the increments of
the curve will be very unequal, making
a difference between those at the ingress
and in the middle of nearly 190 geogra
phical uniles in a minute.

The eclipse will finally leave the earth in lat. 13° 19' 43" N. long. 73° 26′ 26′′ E., which happens in the Arabian sea, near the coast of Malabar. It will be visible to all Europe, the N.E. part of Africa, as far as the line, and the northwestern parts of Asia. The duration will be 4 31 12, beginning at 8 13 45 and ending at 12 46 57.

B.

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As this eclipse will not only be total along the central tract, but for several miles on each side of it, and the umbra will pass over some places of note, both in Europe and Asia, it is to be hoped curiosity will induce some persons to communicate their observations on such an interesting phenomenon. It has ge nerally happened, that the great solar eclipses at London have been annular ones, which was the case in 1748, 1764, 1793, 1804, and will be again in 1820; so that it very rarely happens that the umbra it more desirable in the present instance, passes over Europe, which makes when an opportunity offers in this quarter of the globe, to have a correct ac count of the circumstances attending the apparent extinction of the great light of

Heaven.

I shall now give the elements for constructing this eclipse, from which many curious deductions may be obtained:

The Elements for Constructing the great Solar Eclipse of 1816.
Semi-diameter of the Earth's disc (60′ 16′′.5-8".9).
O's declination (south)

D's true latitude, north, decreasing

The angle which the relative orbit makes with the ecliptic

Apparent time of the true ♂ of the and D, Nov. 19, at

1° 0′ 7′′.6 19° 30' 43"

-50′ 46":8 5° 35' 34".2

m. 8,1

10 22 43 A.M. Horary

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