In over

mining and ordinary machinery points of view, are not fitted to examine and overhaul electrical plant. The question arises as to what constitutes 66 a competent person within the meaning of the Mines Act (Rule 11), and the sooner this is made quite clear and insisted upon the better it will be for all concerned in electrical mining work. the present case, the engineer of the colliery and the " man were entrusted with the machinery in question, and the evidence proves clearly that they were only expected to see that outside and surface connections were all right, and also to open up switch boxes, but any internal faults and so on were not considered to be within their responsibility. Colliery managers must be made to realise that technically trained men should be employed to undertake electrical work in the colliery, and until they do so accidents are bound to occur-the only wonder being that they are not more frequent.

PROF. R. W. WOOD has sent us a description of a series of interesting experiments he has made in the direction of the optical intensification of paintings. Onc of the difficulties an artist has to contend with in depicting scenes in which great contrasts of luminosity occur is the narrow range of luminosity obtainable on canvas with pigments. Aubert states that the whitest paper is but fifty-seven times as luminous as the blackest, and this probably represents about the range obtainable in paintings. The problem is, therefore, how to produce a strong illumination on all high lights of the picture and a feeble illumination on all the shadows. Prof. Wood has obtained good results by taking a photograph of the painting on an orthochromatic plate, preferably a red sensitive plate with a suitable ray filter. A lantern-slide is then made from the negative, and the picture projected in a dark room, not on a white screen, but on the original painting. Any desired effect can be secured by local reduction or intensification of the negative or lantern-slide. If the negative itself is projected upon the painting a most curious effect is obtained. The contrast is lessened, and if the negative is a dense one the contrast may be almost destroyed, making the painting appear a flat wash of chocolate. In taking the negative, care must be taken to have the painting vertical and the camera lens directly in front of the centre of the picture. If after looking for a few minutes at a painting illuminated in the way described the lantern-slide is removed and a uniform illumination allowed to fall on the picture, it appears as if it had not been dusted for ten years; the sunlight leaves it, and everything looks flat. Prof. Wood finds that the effects are very different according to whether the negative is taken on an ordinary or an orthochromatic plate, especially if there is much blue in the painting. He thinks, too, that if the values are correct in the original painting, they will hold under the graded illumination produced by the lantern-slide; if they are not right, the errors will be glaringly magnified.

No. 95 of the Communications from the Physical Laboratory of the University of Leyden contains an account of a series of investigations on the measurement of very low temperatures carried out under the superintendence of Dr. Kamerlingh Onnes, the director of the laboratory. Mr. C. A. Crommelin has compared the readings obtained by a thermoelement of constantin-steel with those given by the hydrogen thermometer. Mr. J. Clay has measured the coefficient of expansion of Jena glass and of platinum between +16° C. and -182° C., and compared the platinum resistance thermometer with the hydrogen and

the gold resistance thermometer, whilst M. C. Braak has made a detailed investigation of the hydrogen thermometer as a means of measuring low temperatures.

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THE transformation, which was first observed by Lallemand in 1870, of orthorhombic sulphur, dissolved in carbon disulphide, into a less soluble amorphous variety under the influence of light, forms the subject of a paper by Mr. G. A. Rankin in the Journal of Physical Chemistry (vol. xi., No. 1). The transformation is brought about by the violet and ultra-violet rays, and is reversible, the conversion of the amorphous form into the orthorhombic crystalline variety taking place when it is kept in darkness. The presence of ammonia or hydrogen sulphide accelerates the latter change and tends to prevent pre-ma cipitation from a carbon disulphide solution even in bright sunlight. Conditions of equilibrium depending on the intensity of the light can be established between the two forms of sulphur present in solution at a constant temperature.

A SECOND edition of Mr. Mervyn O'Gorman's "Motor Pocket Book" has been published by Messrs. A. Constable and Co., Ltd. The book has been revised and enlarged, and its price is 7s. 6d. net.

THE writer of the article on the "Treatment of Cancer" in NATURE of December 20, 1906, writes to say that he was in error in believing that the injections of the pancreatic enzymes have to be made in the neighbourhood of the growth (January 10, p. 247). He understands that this is not the case, so an objection he raised to the trypsin treatment is removed.

OUR ASTRONOMICAL COLUMN. ASTRONOMICAL OCCURRENCES IN MARCH :March 1.

11h. 42m. Minimum of Algol (8 Persei).
14h. Mercury at greatest elongation, 18° 9' E.
8h. 31m. Minimum of Algol (8 Persei).

22h. 26m. Conjunction of Mars with the moon,
Mars 3° 13' S.

Venus. Illuminated portion of disc=0 639.

16. 3h. Conjunction of Vesta with the moon, Vesta,

24.

0° 7' N.

6h. Sun enters Aries, Spring commences.

7h. 16m. to 8h. 30m.

Moon occults x1 Orionis,

(mag. 4'7).

12h. 30m. to 13h. 25m.

Moon occults x Orionis,

mag. 4.8).

16h. 38m. Conjunction of Jupiter with the moon, Jupiter 2° 32' Ñ.

Ioh. 14m. Minimum of Algol (8 Persei).

27. 7h. 3m. Minimum of Algol (8 Persei).

A NEW FORM OF CELOSTAT TELESCOPE.-One of the chief difficulties encountered in the work of the Mount Wilson Solar Observatory has been the deformation and poor definition of the sun's image, caused by the distortion of the mirrors and by the unsteadiness of the heated atmosphere through which the horizontally projected beams have to pass when reflected from the colostat to the spectroheliograph or spectrograph.

Prof. Hale now proposes to obviate some of the difficulties by having the whole instrument vertical, and in No. 1, vol. xxv. (January), of the Astrophysical Journal he describes and illustrates the form of the proposed instrument. The colostat mirror (diameter 17 inches) is to be mounted on a steel tower some 60 feet high in such a manner that it can be moved to follow the sun without

form, will again reflect the beam on to a 12-inch objectdisturbing its adjustments. A second mirror, elliptical in glass (o feet focal length) mounted directly below it, and

this will focus the image on to the slit of the 30-feet spectroheliograph or that of the Littrow spectrograph; both these instruments will be underground, and will therefore be preserved at a fairly even temperature.

To prevent its distortion, each mirror is to be 12 inches thick, and will be silvered on both sides, and, if necessary, heated on the back by reflected or direct sunlight. An electric motor will drive the photographic plate across the secondary slit of the spectroheliograph, and will by means of a vertical shaft impart a synchronous motion to the 12-inch lens, and hence to the sun's image.

The Littrow spectrograph is to be fitted with an 8-inch plane grating, and will be employed in the study of the solar rotation and in the photography of sun-spot spectra. THE RECENT LARGE GROUP OF SUN-SPOTS.-Another large group of sun-spots visible to the naked eye-of which the solar maximum through which we have just passed has furnished an abnormal number was observed during the former half of the present month.

The first signs of this group appeared on February 6, when two small nuclei were seen on the eastern limb about 15° south of the equator, and these were followed by two similar spots on February 8. On February 9 a larger spot brought up the rear of the group, which then contained a large number of small umbræ. In London,

bad weather prevented the daily observation of the develop ment of the group, but on February 11 it was easily visible to the naked eye, and was seen to have developed a second fairly large spot at its preceding extremity. The accompanying reproduction is from a photograph taken

at

was

oh. 47m. on that date, and it may be seen that the preceding spot was then the largest in the group, and had a peculiar kidney-like shape. The total affected area then roughly rectangular, with a length of about 115,000 miles and a breadth of about 55,000 miles. Naked-eye observations of two groups were possible on February 14. The larger group formed a striking spectacle on the western limb on February 18, but had disappeared from view when the sun was observed on the following day.

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THE SPECTROSCOPIC BINARY A ANDROMEDÆ.-From number of spectrograms of λ Andromeda, taken with the Mills spectrograph, 1897-8-9, a set of elements for the orbit of the binary has been computed by Mr. Burns, of the Lick Observatory. On comparing these elements with those determined from more recent spectrograms, taken with the re-mounted Mills spectrograph, it is seen that there are material differences which can only be reasonably accounted for by the supposition that the orbit itself has been modified. The discrepancy, if established, will probably be found to be due to a third body in the system of this star (Lick Observatory Bulletin, No. 105).

THE GROWTH OF MICRO-ORGANISMS.1 THE author, early in the past year, began to make experiments on the origin-of-life question, with various saline solutions containing ammoniacal salts.. After a time he found the best results were to be obtained with one or other of two solutions, one of which contained small quantities of sodium silicate, ammonium phosphate, and dilute phosphoric acid in distilled water, and the other a simple solution of sodium silicate with liquor ferri pernitratis in distilled water. It was found, also, that with the use of these saline solutions exposure of the experimental vessels to diffuse daylight, with even a mean temperature of only 60° F. to 65° F., favoured the appearance of microorganisms quite as much as, or even more than, darkness associated with an incubator temperature of 95° F.

The solutions were placed in previously superheated tubes, which, after being hermetically sealed, were heated again in a calcium chloride bath to 239° F. (115° C.), 248° F., 257° F., or 266° F. (130° C.), for ten to twenty minutes. In all these tubes, after the process of heating, a small deposit, either of silica alone or of silicate of iron, was thrown down. The tubes were subsequently exposed either to diffuse daylight or else in the incubator, and mostly for periods varying from five weeks to four months. When opened, the tubes were found to contain, in varying abundance, one or more kinds of microorganisms, photographs of which were shown..

One point of much interest in connection with these experiments is the fact that no carbon was ostensibly contained in the solutions, though its close chemical ally, silicon, was always present.

It had previously been determined that such solutions proved excellent nourishing media for the growth of microorganisms, and this fact led to trials whether any evidence was to be obtained tending to show that such solutions could also actually engender living units. On examination of the contents of the tubes after their prolonged periods of exposure to light or in the incubator, the organisms were always found, after careful search, on or within the substance of the flakes of silica, while the fluid above remained perfectly clear.

Many organic compounds have been discovered by chemists in which silicon wholly or in part replaces carbon, and it is contended that there is good prima facie evidence from these experiments tending to show that silicon is capable of entering into the composition of protoplasm itself -that is, wholly or in part taking the place of carbon.

In regard to the major question, concerning the origin of life itself, the facts to be borne in mind are these:— If a few hours after the heating of the tubes one or more of them be opened as control experiments and the sediment carefully examined, no organisms of any kind are to be found, but, after suitable periods of exposure, organisms may be found, in more or less abundance, in the sediment taken from other similar tubes. Here, then, is evidence that the organisms are living; they have appeared and multiplied within sealed tubes, though at earlier dates none is to be found.

Then again, it is important to bear in mind (1) that, apart from "". spores " of bacilli, no micro-organisms can

resist an exposure of two or three minutes in boiling water, this being lethal for bacteria, vibriones, micrococci, torulæ, and moulds; and (2) that all ordinary spores of bacilli are killed by a similar exposure for a minute or two to 115° C. (239° F.).

It is concluded, therefore, that the bacteria, bacilli, vibriones, micrococci, torulæ, and moulds which have been taken from hermetically-sealed tubes previously heated to 115° C., 120° C., 125° C., and 130° C. for ten to twenty minutes must have been engendered de novo within these vessels.

The organisms that arise de novo are presumed by the author to assume well-known forms, for precisely the same reason that the various representatives of the crystalline world, when they originate, invariably fall into their own specific shapes, and with surfaces always inclined to one 1 "On the de-novo Origin of Bacteria, Bacilli, Vibriones, Micrococci, Torula and Moulds in certain previously superheated Saline Solutions contained within hermetically sealed Tubes." By Dr. H. Charlton Bastian, F.R.S. Read before the Royal Medical and Chirurgical Society on January 22.

another at angles that never vary for each particular species of crystal. The forms in each set of cases-in organisms and in crystals alike-may be regarded as the necessary resultants of the molecular constitution of their initial units in the particular media and surroundings in which they occur.

PROPERTIES OF ALLOYS.1

THE research described in the report was carried out by the authors with the cooperation of the Broughton Copper Co., Manchester, and the British Aluminium Co.,

chiefly those very rich in copper. At this end of the series the limit of serviceable alloys must be placed at 11 per cent. At the other end of the series the limit is even smaller. Among the specifically light alloys rich in aluminium the limit is probably not higher than 4 per cent. of copper. Between 11 per cent. and 96 per cent. of aluminium (exclusive) the alloys do not appear to be of any practical promise.

(b) But if the range of serviceable alloys is narrow, their quality is certainly high in several instances. This statement holds for certain of the rich copper alloys containing between 7 per cent. and 10 per cent. of aluminium. It is not going too far to say that in certain respects the

After a short ar.nealing.

Quer.ched from 900° C. in water. aluminium.

Milton, who furnished respectively the best commercial copper and aluminium for making the alloys, undertook the rolling and drawing of the materials, and made special castings where necessary.

The salient points of the report are stated as follows:(a) The number of alloys that have been found of any industrial and technical promise is small. Such alloys are

1 Abstract of the Eighth Report to the Alloys Research Committee: On the Properties of Alloys of Aluminium and Copper. By Prof. H. C. H. CarJnter and Mr. C. A. Edwards, of the National Physical Laboratory, Read at the Institution of Mechanical Engineers on January 18

9'90

best of them equal, and even surpass, high-quality steels of the same general character.

The following summary refers only to the rich copper alloys :

(c) Four features of the results of the tensile stress tests of outstanding interest merit a special comment.

(1) In view of the doubt which exists at the present time as to whether copper and its alloys possess true yield-points, it is important to record that from o per cent. to 9 per cent. of aluminium the alloys possess clearly marked yield-points.

(2) It has been recently shown by Messrs. Stanton and Bairstow (Proceedings of the Institution of Civil Engineers, 1906) that the primitive yield-point of a rolled or forged steel is usually an artificial figure, and is due to a stiffening caused by this mechanical treatment. Such is not the case with these alloys. Their primitive yield-point is the

true one.

or

(3) The ductilities (considered as a product of the percentage elongation and reduction of area) of alloys containing from 0.1 per cent. to 7.35 per cent. of aluminium are very high and practically constant, even although the tenacity increases markedly with rise of aluminium. (4) The tenacity and ductility of the widely-known "aluminium bronze " gold," containing 10 per cent. of aluminium, have been found to be as good in the form of small chill castings as in the rolled bar, where an So per cent. reduction of area of the original ingot has been effected. So far as the authors have been able to learn, this result has no parallel. At their request, therefore, independent tests were instituted at the Broughton Copper Works, and these have confirmed the above result, which may have important practical consequences.

(d) The research has brought to light several striking instances of the profound influence of a small quantity of aluminium upon copper, notably in the tension tests, but especially in the torsion and electrical conductivity experiments. One-tenth of 1 per cent. raises the angle of twist of copper in torsion 90 per cent.; it lowers the electrical conductivity 23 per cent.

(e) The behaviour in torsional stress of the alloys containing from 0.1 per cent. to 7.35 per cent. of aluminium is one of the outstanding features of the report.

(f) The alloys containing from 5 per cent. to 10 per cent. of aluminium have come well out of the dynamic stress tests. The particular merit of alloys Nos. 9 and 13 when tested in alternating stress is the close approximation of the maximum stress under which they will bear an unlimited number of reversals to the stress at the elastic limit as determined in a tensile test. In this respect they are markedly superior to the iron and steel specimens hitherto investigated.

66

Alloys Nos. 6, 9, and 13 stood up well when repeatedly stressed beyond the yield-point in Arnold's test. In fact, Prof. Arnold has informed the authors that Alloy No. 9 constitutes a record in its capacity of resisting alternations.""

(g) At about 15 per cent. of aluminium the alloys are entitled to rank with quenched steels in hardness. Thus the hardness number of No. 17 (15.38 per cent.) in the cast state (untreated) is 539, which is about that of a 0-45 per cent. carbon steel quenched in water at 20° C.. (68° F.), and is only slightly lower than that of a 0.66 per cent. carbon steel similarly treated.

(h) In the corrosion tests, which were purposely made as severe as possible, alloys containing from 1 per cent. to 10 per cent. of aluminium have shown themselves to be practically incorrodible by sea-water, whether alone or bolted to a plate of mild steel. In these tests they showed themselves superior both to Muntz metal and naval brass, which corroded appreciably. In tap water of medium temporary hardness the positions were exactly reversed.

(k) In view of the discussion in the previous report as to the trustworthiness of temperatures measured with a protected thermo-junction, the exact influence of the jacket (a fire-clay tube 1/16th inch in thickness) between temperatures of about 1100° C. and 550° C. (2012° F. and 1022 F.) has been determined. It has been found to cause a lowering of not more than 3° C. (5°4 F.) at the higher, and 9° C. (16°.2 F.) at the lower temperature, and above Soo C. (1472° F.) comes within the experimental

errors and uncertainties of the method.

(1) Finally, a special comment must be made on the truly extraordinary similarity in physical and mechanical qualities between alloy No. 13, which consists of 90.06 per cent. of copper +9.90 per cent. of aluminium, and Swedish Bessemer rolled steel of about 0.35 per cent. of carbon and thirty-eight tons per square inch ultimate tensile

stress.

A PROPOSED INTERNATIONAL ATTACK ON THE SIDEREAL PROBLEM.

1

N a brochure written by Prof. J. C. Kapteyn, of the Groningen Astronomical Laboratory, the author outlines the chief points of a very comprehensive attack, which he proposes should be made as soon as possible, on the main problems concerning the structure of the sidereal universe.

Whilst the "Carte du Ciel," parts of which are now approaching completion, gives us the relative projected positions of all the stars down to the eleventh magnitude, and will, by duplication after a number of years, afford material for the accurate determination of proper motions, it leaves untouched the extremely important question as to the distribution of different stellar types in actual space. Prof. Kapteyn proposes to supplement this enormous work by the preparation of a Durchmusterung which shall contain all the necessary data for a preliminary discussion of the structure of the universe. In fact, he proposes that in the same way that the geological has supplemented the geographical study of the earth, so shall an astrological supplement our astrographical study of the heavens; but it is obvious that to attempt a scheme like this for the whole of the heavens at once would be to court failure. The plan would probably die of senile decay ere it showed sufficient results to have justified its existence. For this reason, and acting on the advice of eminent astronomers who favour the idea of such a survey, Prof. Kapteyn limits his proposals to a number of selected areas of the sky. This would reduce the work immensely, and would probably lead to a first approximation of the truths which it is hoped to educe.

The general scheme is based on the method of gauging as carried out by the Herschels, only that now, instead of considering simply the numbers of stars, every ascertainable fact in regard to the objects studied must be considered. The chief data to be obtained, as enumerated by the proposer of the scheme, are visual magnitudes, photographic magnitudes, spectral types, astronomical proper motions, radial velocities, and parallaxes, to which list he adds the determination of the amount of light received from different parts of the sky, as being a subject of great importance to the problem under consideration.

As Prof. Kapteyn points out, there are already sufficient data for the brighter stars, partially excepting parallax and photographic magnitudes, to allow of a fairly thorough statistical treatment, but much of this data needs a great amount of arrangement and classification ere it can be included in a homogeneous attack. The great need in such an inquiry as that proposed is the international study of the fainter stars. Work already completed, or now in hand, will take us down to the seventh or eighth magnitude for most of the elements named, but it is self-evident that, in any attempt to solve the riddle of sidereal structure, the Milky Way is an all-important feature, and, therefore, far fainter magnitudes than this must be included.

Put into its briefest form, the scope of Prof. Kapteyn's proposals is :-" For 206 areas regularly distributed over the sky, and for another less extensive series of particularly interesting regions, to obtain astronomical data of every kind for stars down to such faintness as it will be possible to get in a reasonable time." The 206 areas first named come under the designation of "the systematic plan, and are again divided into two classes, the first of which would comprise 118, and the second eighty-eight These are so arranged that the first class might be completed independently of the second, and would furnish sufficient data for a first approximation. Then, if there were evidence that this could be executed in reasonable time, the second class might be intercalated without interfering with the other, except to provide further data which would, in all probability, enhance the value of the final

areas.

1 "Plan of Selected Areas." By Prof. J. C. Kapteyn. (Groninge, 1906.

results to an extent incommensurable with the extra labour involved.

The 206 areas would include 400 square degrees of the sky, and this full scheme would entail the following labours-The determination of the rough positions and sharply defined photographic magnitudes of some 200,000 stars; visual magnitudes for the same 200,000; the determination of the accurate proper motions, to within o".01 in each coordinate, of some twenty thousand of these objects. For the same twenty thousand, parallaxes are necessary, and for as many of them as is possible the class of spectrum and the radial velocities must be determined. Finally, the determination of the total amount of light received from different parts of the sky would complete a set of homogeneous data from which undreamt-of additions to our knowledge of the sidereal universe might

accrue.

66

In addition to this " systematic plan," Prof. Kapteyn, after much correspondence and discussion with a number of eminent astronomers, has decided on a scheme for the elucidation of 'special areas. This scheme includes forty-six areas, such as those in the Milky Way which show intense variations of star-density, the rifts and branches of the Milky Way, and extra-galactic areas where nebulæ or strong contrasts in star-density are preponderant.

Many interesting devices to further the plan are discussed by Prof. Kapteyn, e.g. the determination of colour, and hence the probable spectrum class, from the comparison of the photographic and visual magnitudes in the cases where the stars are so faint that these features cannot be determined by the usual methods; again, the determination of proper motions and parallaxes from plates exposed a second time after an interval of some years. Possibly Prof. Wolf's stereo-comparator method of determining proper motions would materially curtail the interval necessary between the two exposures.

Considering a few details, it is seen that the scheme includes (1) 9710 exposures on 2620 plates, in addition to the plates for the determination of the radial velocities of three or four standards in each area. (It is intended that the bulk of the radial velocities shall, if possible, be determined by one of the wholesale prismatic-camera methods such as those proposed by Herr Orbinsky, Prof. E. C. Pickering, and Prof. Comstock.) (2) Visual observations of 3024 standard magnitudes, the determination of the magnitudes and positions of 200,000 stars, and the meridian observations of some 2600 stars for propermotion standards. (3) The measuring of nearly 1 million images.

Prof. Kapteyn, with all his experience, is quite ready, should the essential funds be forthcoming, to undertake a greater part of the measuring work, and could, at present, undertake to perform half his proposed share. A number of other well-known astronomers, as may be seen from the letters which he publishes at the end of his brochure, are definitely and enthusiastically in favour of the project, and are willing to grant what aid is in their power, so that the scheme cannot be looked upon as immature or as entailing insuperable difficulties.

UNIVERSITY AND EDUCATIONAL
INTELLIGENCE.

OXFORD.-At a meeting of members of convocation in Magdalen College on February 23, which had been summoned by the Vice-Chancellor to consider the election of a Chancellor of the University, there seemed to be a majority in favour of the nomination of Lord Curzon.

The published accounts of the common university fund for 1906 show that the income for that year was 69371., and the expenditure 63951., of which sum 35771. was devoted to scientific objects.

CAMBRIDGE.-The Smith's prizes have been awarded for "Fluorescence, G. R. Blanco- . the following essays:White; The Systematic Motions of the Stars," A. S. Eddington; "The Bending of Waves Round a Large Opaque Sphere and some Associated Problems,' J. W. Nicholson; "The Variation of the Absorption Bands in the Spectrum of a Crystal under the Action of a Magnetic 4 Field," W. M. Page. The names are arranged in alpha-d betical order. The essay on "Some Problems on the Diffraction of Electric Waves," by H. J. Priestley, is awarded honourable mention.

Accepting for the moment that the plan, in its entirety, is feasible, the possibilities attached to the discussion of the results are obviously infinite. In some fifty or a hundred years, the "Carte du Ciel," if repeated, will probably afford a series of definitive proper motions which can then be discussed from the sidereal structure standpoint, but of the spectral layers in the visible universe it would leave us in almost total ignorance. On the other hand, the results from Prof. Kapteyn's plan would probably afford all the information attainable by human effort of the sidereal strata, or groups, or drifts, or a thousand and one other features.

As an earnest of what might accrue from such a discussion, one may cite the remarkable result recently derived by Mr. Eddington from the analysis of the relatively meagre data of the Greenwich-Groombridge proper motions (see NATURE, No. 1938, p. 182, December 20, 1906), a result first derived, in a qualitative form, by Prof. Kapteyn himself from a discussion of the Bradley proper motions. W. E. ROLSTON.

H. R. Hassè has been elected to the Isaac Newton studentship, tenable from April 15, 1907, to April 15, 1910. The student will carry on a course of research in physical optics.

W. Spens has been elected fellow at Corpus Christi College, and has also been appointed director of natural science studies in the college.

Zoology, announces the receipt of a cast of a skeleton of Dr. Harmer, the superintendent of the Museum of Diprotodon australis, presented by Dr. E. C. Stirling, F.R.S., director of the South Australian Museum at Adelaide. Dr. Harmer also records the gift of a valuable consignment of some nine skeletons and forty skulls and skins of mammals, mostly antelopes, from tropical Africa, presented by Mr. C. B. C. Storey, of Clare College.

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The Cavendish Laboratory Extension Syndicate has proposed plans for the new laboratory running along Free School Land, which will cost between 7000l. and 8300l. Towards defraying the cost of this building there is available Lord Rayleigh's gift of 5000l. out of the Nobel prize, and Prof. Thomson is able to find 2000l. from the labor- our atory funds.

The recommendation of the general board of studies d that a university lecturer in pathology be appointed, in dist connection with the special board for medicine, with an cul annual stipend of 100l. payable out of the common university fund, will be brought before the Senate on 'March 9.

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It is proposed to nominate Prof. A. Thomson to be a ve member of the board of electors to the professorship of ed anatomy; Sir E. C. Perry, a member of the board of a electors to the Downing professorship of medicine; Prof. Graham Kerr, an elector to the professorship of zoology; Dr. Anderson, an elector to the chair of physiology; Prof. Middleton, an elector to the Drapers' professorship of in agriculture; and Prof. Langley, to that of botany.

The local examinations and lectures syndicate has ad appointed E. A. Parkyn and D. H. S. Cranage as delegates at the International Congress on School Hygiene to be held in London in August.

Mr. J. J. Lister has been appointed a manager of the Balfour fund until June, 1909, in succession to the late Sir Michael Foster.

Mr. F. A. Potts has been nominated to occupy the University table at the laboratory of the Marine Biological Association at Plymouth for one month during the ensuing Easter vacation.

THE Mercers' Company has made a donation of fifty guineas, and the Grocers' Company one of ten guineas, to the South-Eastern Agricultural College.

AT the South-Western Polytechnic on March 15 the Lord Alverstone, G.C.M.G., Lord Chief Justice of England, will present prizes and certificates to students of evening classes and of the day college.

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28 10