Science Abstracts. Section A, Physics Abstracts. Vol. 48, No. 573

T N o / Y f

PHYSICS ABSTRACTS

S E C T I O N A

o f

SCIENCE ABSTRACTS

SECTION A , PH YSICS

SEC TIO N B, E L E G J^ IC A L E N G IN E E R IN G

Edited and Issued M onthly by

THE INSTITUTION OF ELECTRICAL ENGINEERS

In Association with

T H E PH YSICAL SOCIETY T H E A M E R IC A N PH Y SIC A L SOCIETY

T H E A M E R IC A N

IN ST IT U T E OF ELECTRICAL E N G IN E E R S

V O LU M E 48

A B S T R A C T S 2081-2401

SEPTEMBER 1945 N U M B E R 573

TY P E IV COMPRESSOR & VACUUM PI M P

A N A L L - P U R P O S E U N I T F O R E V E R Y L A B O R A T O R Y A N D W O R K S

★ Vacuum 24 in. Hg.

★ P ressure 10 lb.

' k

Displacem ent 3 cubic feet per second

Blowpipes, Spraying A i r o r Gas C irc u latin g

Aspirating, etc.

PRICE COM PLETE AS ILLUSTRATED

£18 :18 : 0

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K A N G L E Y B R I D G E R O A D , L O W E R S Y D E N H A M , L O N D O N , S.E.26 Telephone: SYDenham 7026. Telegrams: Edcohivac, Phone, London

061 A n n u a l r e p o r ts 51 M a th e m a tic s 511 A r ith m e tic 512 A lg e b ra 513 G e o m e try 517 A n a ly sis

.5 F u n c tio n s .9 D iff. e q u a t io n s 518 C a lc u la tio n 519.2 P r o b a b il ity

.4 G r o u p s 52 A s t r o n o m y 523 D e sc rip tiv e

.1 C o sm o lo g y .4 P la n e ts

.7 S u n

.8 S ta rs

526 G e o d e s y 53 P h y sic s

.081 53 0 .1 2

U n its . D im e n sio n s R e la tiv ity

.1 4 5 Q u a n tu m th e o ry 531 M e c h a n ic s o f s o lid s

.7 M e a s u re m e n ts 53 2 M e c h a n ic s o f flu id s

.13 V isco sity .5 H y d ro d y n a m ic s .61 S u rfa c e te n s io n .63/.6S C a p illa rity .69 S u rfa c e a c tiv ity .71 O sm o sis .7 2 D iffu sio n .73/.7S S o lu tio n 533 M e c h a n ic s o f g ases

.6 A e ro d y n a m ic s 5 3 4 A c o u stic s 535 O p tic s

.1 T h e o ry .2 R a d i a tio n .215 P h o to -c le c tric ity .2 4 P h o to m e tr y .31 G e o m . o p tic s

CONTENTS ABSTRACTS 2081-2401

E a g c P a g e

2 33 535 .3 2 R e fr. in d e x 24 7

2 33 .33 S p e c tro s c o p y 24 7

2 33 .338 S p e c tra 2 4 8

233 .34 A b s o r p tio n 248

2 33 .37 F lu o re s c e n c e 2 49

2 33 .375 R a m a n effect 2 49

2 3 4 .41 I n te r f e r e n c e 2 4 9

2 3 4 .43 S c a tte rin g 2 4 9

2 3 4 .6 C o lo u r 249

235 .7 V isio n 25 0

235 .8 I n s tr u m e n ts 25 0

2 3 6 536 H e a t 2 5 0

2 3 6 .7 T h e rm o d y n a m ic s 251

23 6 .8 H e a t e n g in e s 2 5 2

2 3 6 537 E le c tric ity 2 5 2

23 6 .12 E le c tro n s 2 5 2

2 3 6 .2 E le c tro s ta tic s 25 2

238 .2 2 6 D ie le c tric s 253

23 8 .29 E le c tric field s 253

2 3 8 .31 C o n d u c tiv ity 253

2 3 8 .5 D is c h a rg e 25 4

2 3 9 .531 X -ra y s 25 5

2 3 9 .533 N e g . ra y s 255

2 4 0 .5 3 4 P o s . ra y s 25 6

241 .5 6 Io n iz a tio n 257

241 .59 C o s m ic r a y s 25 7

2 4 2 538 M a g n e tis m 259

2 4 2 .1 T h e o r y 25 9

2 4 3 .2 P r o p e r tie s 2 6 0

243 .5 4 E d d y c u r r e n ts 26 0

24 3 .5 6 E lc c tro m a g n . oscill. 26 0

24 3 .6 M a g n e tic fields 260

243 .7 T e r r e s tr . m a g n e tis m 2 6 0

2 4 4 539.13 M o le c u le s 2 6 p

2 4 4 .15 A to m s 261

2 4 4 .16 R a d io a c tiv ity 261

24 5 .17 A to m d is in te g r a tio n 262

245 .185 N e u tr o n s 2 6 2

24 6 .2 S t r u c t u r e o f s o lid s 26 2

2 4 6 .2 6 X - ra y e x a m . 26 4

2 4 6 .3 E la s tic ity 26 4

2 4 7

061.055.1 A L G E B R A — G E O M E T R Y 517.392

061.055.1 : 550.3

see Abstr.

2600 0 6 1.05 5.5 : 550

see Abstr.

2599 061.055.5 : 550.381 J<?e

Abstr.

2604

06 1.22 : 535.42 : 53 7.533.73 : 537.531

see Abstr.

2311

511.23 2081

O n the integral order, (mod

p ).

o f quadratics

x 2 + ax

+

b,

w ith applications to the construction o f m inim um functions fo r

G F(p2),

and to some number theory results. Bo se, R . C ., Ch o w l a, S ., a n d Ra o, C . R .

Bull. Calcutta M ath. Soc.,

36,

pp.

153-174,

Dec.,

1944.— P olynom ials are considered whose coefficients belong to th e rin g o f integers, and

p

is an od d prim e. T h e least positive integer

n

such that

x n =

an integer (m o d

p, x 2

+

ax +

6), is called the in teg ral o rd e r o f

x 2

+

ax

-j-

b,

(m o d

p).

A n u m b er o f theorem s are deduced concerning the integral order. G iv e n

b

# 0, a ll quadratics

x 2

+

ax

+

b

o f a given type and in teg ral o rd e r are fo u n d , an d these are used in constructing m in im u m functions fo r

GF(p2).

Som e k n o w n results concerning these functions are extended. G iv e n

a

# 0 , all quadratics

x 2 + ax + b

o f a given type and in teg ral o rd e r are fo u n d , and necessary and sufficient conditions are investigated un der w h ich the congruence

f„(a ,b )

=

0 (m o d

p)

is solvable, (i) w h en regarded as a congruence in

a,

(ii) w hen regarded as a congruence in

b.

H e re

/„(a , b)

=

F n(y — \a , — y — ia )

where

y 2 = i( a 2

— 4 6 ) and

Fn(X, Z )

is the result o f m akin g

Fn(X ),

th e cyclotom ic p o lyn o m ial o f o rd e r

n,

h o m o ­

geneous by in tro d u cin g

Z .

T h e applications to n u m b er th eo ry include th e determ in atio n o f prim es

p,

such th at 2, 3 o r 5 are q u ad ratic residues o f

p,

and the s o lvab ility o f th e cubic congruences

x 2 —

3 x = + 1 (m o d

p), x 2

— 3 * = — 1 (m od

p)

l. s. G.

511.5 2082

E u le r’s three biquadrate proolem. Wa r d, M .

Prac. Nat. Acad. Sci., Wash.,

31,

pp.

125-127,

A p ril,

1945.— T h e pro b lem is w h eth er the d io p h an tin e equa­

tio n x4 + y4 + z4 = cu4 has an y in teg ral solutions.

I t is show n th a t th ere cannot be a solution w ith

co < 10 00 0. l. s . G.

51 1.9 2083

A peculiar g ap-fillin g process fo r powers o f (9 )n . Ka p r e k a r, D . R .

J. Univ. Bombay,

13, p. 1,

M arch,

1945.— B y (9 )„ w e m ean the d ig it 9 repeated « times, and by (9 )"‘ w e m ean the w th po w er o f (9)„. A qu ick m eth o d is given fo r w ritin g d o w n (9 )"'. l. s. g.

512.1 : 621.3.0 14 2084

E lectronic circuits perform m athem atical processes.

Be it m a n, M . N .

Radio News,

33,

pp.

72

and

74,

M ay,

1945.— [A b str. 1875 B (1945)].

512.52 2085

M e th o d o f Lagrang ian curvilinear interpolation.

Ta y l o r, W .

J. J. Res. Nat. Bur. Stand., Wash.,

35,

pp.

151-15 5,

Aug.,

1945.— Describes a sim plified m eth od o f co m p uting Lagran g ian coefficients fo r c u rv ilin e ar in terp o latio n , w h ic h m ay be used w hen tables o f Lag ran g ian coefficients are n o t a v ailab le o r w h en tables are availab le b u t th e coefficients a re n o t tabulated f o r the exact fractio n o f the in terval to w h ich th e in te rp o la tio n is to be m ade.

513.3 : 548.1

see Abstr.

2567 513.563 : 513.734

see Abstr.

2088

513.564.1 2086

O n a problem in solid geom etry. R a o , C . V . H .

Bull. Calcutta M ath. Soc.,

36,

pp.

132-134,

Dec.,

1944.— T h e lengths o f the axes o f a n a rb itra ry plane section o f the general q u ad ric surface are determ ined.

l. s . G.

513.622.11 2087

O n surface area. Ra d o, T .

Proc. Nat. Acad. Sci., Wash.,

31,

pp.

102-10 6,

M arch,

1945.— T h e surface area o f F rec h et surfaces,

S,

o f th e type o f the 2-cell is considered. A q u a n tity a (S ), term ed the lo w er a rea o f

S,

is in tro du ced , using conceptions in the theory o f continuous tran sfo rm atio ns in th e plane. T h e relation ship o f

a(S

) to th e Lcsbesguc area o f

S,

denoted b y

A (S )

is studied, an d conditions are given in o rd e r th a t

a(S)

= /IC S ). l. s. g.

5 1 3 .7 3 4 :5 1 3 .5 6 3 2088

O n scrolls generated by lines whose polars w ith regard to a pencil and a net o f quadrics arc concurrent.

C h a r i a r , V . R .

Bull. Calcutta M ath. Soc.,

36,

pp.

1 2 2-12 4,

Dec.,

1944.— A study is m ade o f surfaces generated by lines,

I,

whose polars w ith respect to a given pencil, Q , o f quadrics intersect. T h e lines,

I,

th ro ug h a given p o in t generate a q u ad ric cone passing th ro u g h the vertices o f the s e lf conjugate tetrahed ro n.

A ls o lines w h ich intersect a given line, A, and whose polars w ith respect to 2 pencils o f quadrics are con­

cu rren t, pencil by pencil, generate a surface, 2, o f o rd e r 8 havin g A as a m u ltip le curve o f o rd e r 4.

A plane 7r th ro u g h A meets 2 residually in 4 straight lines w h ich intersect in pairs in 6 points. A s

tt

varies these 6 points trace o u t a curve o f o rd e r 6 w h ic h is do ub le o n

2 -

V ariou s o th er properties o f

2

are deduced, and it is shown th a t the polars o f a given lin e w ith respect to 3 given quadrics w ill be con­

cu rren t o n ly w h en the lin e is th e g e nerator o f a certain ruled surface o f o rd e r 9. l . s . g .

513.76 ’ 2089

Irre g u la r projective invariants. K a s n e r , E ., a n d D e C i c c o , J.

Proc. Nat. Acad. Sci., Wash.,

31,

pp.

123-12 5,

A pril,

1945.— A b r ie f su m m ary o f the classification o f irre g u lar an alytic elements w ith respect to th e 8-p aram e ter group o f collineations in the. plane. A n irre g u lar elem ent w ith a sim ple cusp possesses 2 relative in varian ts o f the 7th an d 8th

orders. L. s. G.

5 1 3 .7 6 1 .4 :5 1 3 .8 3 20 90

A x io m a tic approach to homology theory'. Eil e n- b e r g, S ., a n d St e e n r o d, N . E .

Proc. Nat. Acad.

Sci., Wash.,

31

, pp.

1 1 7-12 0,

A pril,

1945.— T h e usual approach to th e concept, h o m o log y grou p, in vo lv in g the study o f the co m plex, is here replaced by an a x io m a tic ap proach, w h ich results in greater logical sim p licity an d a broadened p o in t o f view . O n ly a

b r ie f o u tlin e is given. l. s . g.

513.83 : 513.761.4

see Abstr.

20 90

5 1 7 .3 9 2 :5 1 8 .1 2 2091

T a b le o f coefficients fo r num erical in teg ration w ithout differences. Lo w a n, A . N . , a n d Sa l z e r, H . E .

J. M ath. Phys.,

24,

pp.

1 -2 1 ,

Feb.,

1945.—

v o l. x l v ii i.—a.— 1945. Se p t e m b e r. 233

517.512.2 ANALYSIS, v D I F F E R E N T I A L E Q U A T I O N S 517.945.6

B y in teg ratin g th e L a g ran g ian in te rp o la tio n fo rm u la th e in teg ral o f a fu n ctio n

f ix ) ,

k n o w n fo r

n

eq ually spaced argum ents a t in te rv a l

h,

is given as

r A'o

+sh

■{'Or f{ x ) d x ■

-L'o+r/i

w h ere th e su m m ation extends fro m

i = —

[ ! ( « — 1)]

to

i

= [ i « ] , an d

B \\p )

are po lyn o m ials o f degree

n.

T a b le s a re given o f th e values o f these p o lyn o m ials to 10 d ecim al places, fo r

p

ran g in g fro m — | [ ( n — 1] to [ in ] . F o r

it —

3, 4 an d 5 the ta b u la tio n in terval is O 'O l an d fo r

n

—6 an d 7 th e in terval is O -1 . l . s . g . 5 1 7 .5 1 2 .2 : 548.1

see Abstr.

2568

5 1 7.51 2.4 : 621.396.619.018.41 2092

Tables o f Bessel functions

J „(x )

fo r large arguments.

CORRINGTON, M . S ., AND MlEHLE, W .

J. M ath.

Phys.,

24,

pp.

3 0 -5 0 ,

Feb.,

1945.— T w o tables o f

Jn{ms)

are given, tq five decim al places, fo r

n =

0(1)10 a n d

s —

1(1)20. I n th e first th e range o f

m

is 1(1)10 and in th e second

m — v , 2rr, . . ., 5tt.

T h e tables are convenient fo r use in th e su m m ation o f the S chlom ilch series w h ic h occur in th e th eory o f frequency m o d u la tio n , e.g. the ca lcu latio n o f the h a rm o n ic d is to rtio n term s an d o f the co m b in a tio n frequency am plitud es produced w h en an in terferin g signal is present in freq u en cy-m o d u latio n trans­

m ission. l. s . G.

5 1 7 .5 6 :6 2 1 .3 9 6 .1 1 2093

T h e parabolic cylinder functions. We l l s, C . P ., a n d Sp e n c e, R . D .

J. M ath. Phys.,

24,

pp.

5 1 -6 4 ,

Feb.,

1945.— T h e functions 0Ua(£) an d

cUa(£)

w h ich are solutions o f

cPUa(0id? + (£2 + a)Ua(Q = 0,

are represented in a fo rm suitable fo r the solution o f problem s in vo lv in g standing waves. P o w e r series solutions are given an d th e re la tio n o f

Ua( 0

to the confluent hypergeom ctric fu n ctio n Is exam ined . I n ­ tegral solutions,

(sech

<f>)i

cos { K2 ta n h

<j>

+

\a$}d<i>

Jo

o V„{Q = c2

(sech </>); cos { iC2 ta n h

<f>

+

\a<f>}d<f>

Jo

a re ob tained and also solutions asym p to tic in

a

an d these are useful w h en f is n o t to o m u ch larger th a n

a.

Solutions asym p to tic in £, suitable fo r co m ­ p u tin g the functions w h en £ is large, are given an d the functions are tabulated fo r

a

= ± 1, ± 2, ± 3 over th e range £ = 0- 0 0 (0 -1 )3 - 0 0 . T h e functions occur in th e problem s o f th e prop ag atio n o f electro­

m agnetic waves in p a ra b o lic pipes an d th e vib ra tio n s o f a p a ra b o lic m e m b ra n e [A b str. 170 B (1 9 4 3 )].

l. s. G.

51 7 .5 6 4 .3 /.4 2094

O n certain integrals involving Legendre and Bessel functions. Bose, B . N .

Bull. Calcutta M oth. Soc.,

36,

pp.

125-13 2,

Dec.,

1944.— S om e relation s between Legendre an d Bessel functions are o b tain ed an d used to establish certain defin ite integrals, e.g. integrals o f the type

A

P„( 1 - 2y2)F(y)dy

Jo

w h ere

F(y) — J,„(yz)ym + l

o r J 2,(y z)y 2,” + l o r

I m{ky)K,n{ky)y2m+ 1

are evaluated as a fin ite series w hose term s in volve Bessel a n d G a m m a functions.

I t is show n th a t, fo r a ce rta in range o f values o f

It,

r l sin

( 2 y . z)dy r2

{(1 -

h)2 + 4hy2} i ~

* , ? ( *

— a nd s im ila r integrals are

„ q -zCz 4“ ^ ) ev aluated in closed fo rm , an d also T h e in teg ral,

J z n + i& O 2

+ z 2)* }

(t2

+ z 2) i

dt, J ln + 2 {y if2

+

Z2) t y t 2 + Z2 dr

and

d2n+i{y(l2 + t^K n +iW l1* _dt

-d t

=

T7Z~l J2n+\(yz)

0

(t 2 +

Z2)$

w h ere — 1 <

p <

2 an d 0 <

y

<

b.

I t is fin ally shown th at

' s i n

a(z + t) J 2n+ \(y t)

. -

7 7 + 7

^{7T -}

pro v id e d 0 <

y

<

a.

l. s. g.

5 1 7 .9 1 2 .2 :6 2 1 .3 .0 1 2 .8 2095

N um erical solution o f ordinary and p a rtia l differential equations by means o f equivalent circuits. Kr o n, G .

J. Appl. Phys.,

16,

pp.

172-18 6,

M arch,

1945.—

N u m e ric a l m ethods are developed to solve, certain types o f lin e a r an d n o n lin e a r p a rtia l differen tial equations to an y desired degree o f accuracy w ith the a id o f eq uivalen t electrical netw o rks. T h e m ethods o f so lution o f o rd in a ry d ifferen tial equations fo llo w as special cases. T h re e types o f problem s are con­

sidered: (1) I f th e field qu antities are k n o w n alo n g a surface, th e netw o rks m ay be solved by a straight­

fo rw a rd step-by-step calculatio n. F o r tim e-varyin g problem s new types o f netw o rks are developed in w h ich tim e appears as an ex tra sp atial v a ria b le . (2) F o u r m ethods o f so lu tio n o f bo u n d ary value problem s are given: (a ) th e m eth od o f weighted averages; (6) un ­ balanced currents and voltages; (c) relax atio n m eth o d ;

id )

diffu sion m eth o d , th a t changes th e b o un dary- value p ro b lem in to a n in itia l-v a lu e p ro b lem by ad din g to the o rig in al p a rtia l d iffe re n tia l eq u atio n a tim e va ria b le. (3) C haractcristic-valu e prob lem s.

T h e m ethods o f s o lu tio n are s im ila r to those o f b o u n dary-valu e problem s.

517.945.6 = 4 2096

O n a solution o f the telegraphic equations. Pa r o d i, H .

C.R. Acad. Sci., Paris,

21 6,

pp.

6 0 6 -6 0 8 ,

M ay

3, 1943.— T h e equations are

DEIbx + r l + IDIIbt

= 0 ,

b llb x + g E

+

CdE/it

= 0 w h ere

E

and

I

are th e po ten tia l an d cu rren t and

r, I, g

an d c are th e (constant) lin e param eters. T h e so lution is usually d e riv ed b y elim in a tin g one o f the variables b u t in th e ne w m eth od given w e w rite

E = D E j, I —

E L - an d sp lit up each eq uation . Th u s

/

1

th e first eq u atio n becomes

, l E i

234

517.947.5 D I F F E R E N T I A L E Q U A T I O N S — C A L C U L A T I O N — PROBABILITY '519.41

N o w assume th a t th e sum o f the term s in each vertical lin e is zero. A fte r some redu ctio n, the so lution is ob tain ed in th e fo rm

E

=

E i

cosh * 0 —

¡¡S

sinh * Q / = / ] cosh

x Q

— E ^ S s in h x: 0

w here 0

= {(Jp+r)(cp+g)}i, S = (lp+r)l(cp+g)-i

and

p — blbt.

I n p a rtic u la r w h en

E l = E0ea l,

/ [ =

K E 0ea <

th e usual solution is obtained. l. s. o .

51 7.947.5 = 4 2097

A new solution o f the equation A3U =

U.

Hu m­ b e r t, P .

C.R. Acad. Sci., Paris,

21 6,

pp.

6 5 7 -6 5 9 ,

M a y

17, 1943.— T h e eq uation ,

td U I W

A 3C / = ^ 3- + V +

V U

, 5 3( /

— 3:

u

i>z3 ''bxbybz

m ay, by changing th e variables to

X, Y

a nd

Z

where

x = X 2 +

2

YZ, y — Z 2 + 2 X Y

and

z = Y 2 + 2X Z

be w ritte n in th e fo rm

7>3U

i>3

U l 3U b3 U b X 3

+ + j)Z 3 O J Q

Y b Z

= 8 (2(3 + Y 3 +

Z 3

-

3 X Y Z )U

H e r e th e variables m a y be separated by w ritin g

U

=

F (r) G(s)

exp

( X 2

+ 2

YZ)

w here

r

=

2 X - Y — Z

a n d

s

=

( Y — Z ) V

3. I t is fo u n d th a t th e equations giving

F

and

G

are each satisfied b y th e co nfluen t hypergeom etric fu nction , thus

F = l F l {h,- i , - i r 2); G

=

iF y{ - h , i , is 2),

so th e o rig in a l eq uation is solved. l. s. g. 518.12 : 517.392

see Abstr.

2091

518.3 : 533.4

see Abstr.

21 94 518.3 : 534.37

see Abstr.

2208 518.3 : 541.123.7

see Abstr.

2447

5 1 8 .3 : 6 2 1 .3 9 2 .5 = 4 2098

Q uadripole nomograms. T h e ir application to trans­

mission lines, d e Mil l e v il l e, H .

Rev. Gen. ¿ le d .,

54,

pp.

2 2 -2 4 ,

Jan.,

1945.

518.5 2099

A problem -solving scale. Le iv e sl e y, V . W .

J. Jnstn Engrs, Aust.,

17,

p.

65,

M arch,

1945.— M a r k on a straig h t edge a lin e a r scale o f

x 2

an d n u m b e r it in term s o f

x ,

thus prod ucing a square la w scale. T h is m ay be used d irec tly fo r th e usual Pythagorean o p eratio n

a

=

{b2

± c2) i , e.g. by using the scale to set o ff ap p ro p ria te points a lo n g a straight line.

A p p lic a tio n to po w er facto r economics, etc., is noted.

■*' G . F. F.

518.5 : 548.73

see Abstr.

2587

519.21 : 677.3 2100

T h e statistical theory o f the strength o f bundles o f threads. I . Da n i e l s, H . E .

Proc. Roy. Soc. A,

183,

pp.

4 0 5 -4 3 5 ,

June

18, 1945.— T h e strength o f a bundle is th e m a x im u m lo ad w h ich it can support. A study is m ade o f th e p ro b a b ility distrib u tio n o f the strength o f bundles whose constituent threads arc sam pled ra n d o m ly fro m an in fin ite p o p u la tio n o f threads in w h ic h the p ro b a b ility d is trib u tio n o f strength is k n o w n . A n expression is derived fo r th e chance,

B „,

th a t a bu n d le o f

n

threads is o f strength less than a given value.

Bn

is expressed firstly in the fo rm o f a d e term in an t an d then, in 2 ways, as a p o w e r series.

T h e last h a lf o f the paper is devoted to an a n alytical in vestigation o f th e asym ptotic b e h av io u r o f

Bn

as

n

—> 0 0. A l l the threads a re assumed to have the same load-extension curve u p to th e breaking p o int.

I t is fo u n d th a t in th e com m onest cases, as

n - y

0 0, the d istrib u tio n tends to the n o rm a l fo rm . l. s. g.

5 1 9 .2 4 :6 2 1 .3 1 5 .6 2 2101

S tatistic al methods applied to insulator development and m anufacture. Ta y l o r, J. J.

Trans. Amer. Inst.

Elect. Engrs,

64,

pp.

4 9 5 -4 9 9 ,

July,

1945.

519.271.1 2102

T h e distribution o f the m ean o f samples fro m a rectangular population. Iy e r, P . V . K .

Curr. Sci.,

14,

pp.

18 -19,

Jan.,

1945,

519.271.1 2103

A note on H o te llin g ’s

T 2.

Iy e r, P. V . K .

Curr.

Sci.,

14,

pp.

173-17 5,

July,

1945.— [A b str. 2102 (1945)].

519.271.1 2104

M in im u m size o f a sample. Sa l v e k a r, P . M .

J. Univ. Bombay,

13,

pp.

2 - 6 ,

M arch,

1945.— A table is given show ing the m in im u m size required in experi­

m e n ta l w o rk in o rd e r to estim ate th e p o p u latio n m ean w ith a specified degree o f accuracy fo r a specified level o f r e lia b ility . T h e m eth od used in constructing

the ta b le is discussed. l. s. g.

519.272 2105

In teractio n form ulae in analysis o f variance. Ay- y a n g a r, A . A . K .

Curr. Sci., 14, p.

35,

Feb.,

1945.

519.272 2106

F a m ilia l correlations or the m u ltivariate generaliza­

tions o f the intraclass correlation. R a o , C . R . K .

Curr. Sci.,

14

,p p .

6 6 -6 7 ,

M arch,

1945.

519.272.11 2107

Regression lines and the functional relation. Se a r e s, F . H .

Astrophys. J.,

100,

pp.

2 5 5 -2 6 3 ,

Nov.,

1944.—

I t is freq u en tly requ ired to find the fu n ctio n al relation

Yt — A + B X 1

fro m values

X, Y

o f the variables w h ich are affected by observational errors. A m eth o d is given fo r deriving

A

and

B

free fro m system atic e rro r. R ed u ctio n o f the values

X

to the system o f

Y

is by th e regression lin e o f

Y

o n

X

only in the case o f observations o f equal weight. W h e re th e observations d iffer in precision no single line suffices, b u t an expression depending on

B

an d the m ean e rro r o f

X

is derived fo r th e slope o f th e m ost pro b ab le lin e. T h is re la tio n gives all the charac­

teristic properties o f the regression lines, am on g th em th e fa ct th a t the lines are strictly lin e a r o n ly w hen the frequency d istrib u tio n fo r

X

and

Y

is G aussian, a. h u.

519.283 : [62 + 66] 2108

S tatistic al methods in deciding the efficacy o f a m odification in technical procedure: the use o f the /-te s t to chemists and engineers. Ev a n s, U . R .

Chem. and Ind.,

14

,pp .

106-10 9,

A p ril

7, 1945.

519.283 : 620.11 2109

S tatistical tools fo r controlling qu ality. Ma n u e l e, J., a n d Go f f m a n, C .

Trans. Amer. Inst. Elect. Engrs, 64, pp.

5 2 4 -5 2 8 ,

July,

1945.

519.283 : 677 : 539.216.1

see Abstr.

2836 519.4 : 548.1

see Abstr.

2569

519.41 2110

O n semigroups. Le v i, F . W .

Bull. Calcutta M ath.

Soc.,

36,

pp.

1 4 1-14 6,

Dec.,

1944.— Sem igroups, i.e . systems a d m ittin g an associative m u ltip lic a tio n ,

235

523.12 A S T R O N O M Y 523.841.1

are investigated fro m the po int o f view o f the co m ­ b in a to ria l th eory. O f p a rtic u la r im po rtance are /¡t-semigroups w h ich satisfy the co n d itio n

R

( o f refin em ent). T h is states th at i f

a, c

an d

a', c'

are differen t pairs o f elements such th at

ac

=

a'c'

then there exists a n elem ent

b

satisfying a t least one o f the tw o pairs o f conditions

a’ = ab, c = be'

o r

a — a'b, c'

=

be.

I t is show n th at free semi-group's m ay be defined by axiom s w ith o u t reference to a system o f letters o u t o f w h ich they are fo rm ed as words. T h e representation o f a grou p as a facto rg ro up o f a free

sem igroup is discussed. l. s. g.

5 2 3 .1 2 : 5 3 0 .1 4 5 : 5 3 0 .1 2 2111 K inem atical relativity and the nebular rcd-shift.

Di n g l e, H . , Mil n e, E . A .

Nature, Loud.,

155,,

pp.

5 1 1 -5 1 2 ,

A p ril

28, 1945.— D in g le enquires h o w it is possible in kin em atical re la tiv ity to in terpret the rcd-shift o f the lines in n ebu lar spectra as due to relative m o tio n o f the observer an d the nebula w hen relative velocity can be transform ed aw ay by a suitable change o f rate in the observer’s clo ck. W h e th e r the k in em atic al tim e-scale o r the dynam ical tim e-scalc is used,

ad hoc

causes fo r the observed red-shift m ust ap p aren tly be introduced. In his rep ly , M iln e states th a t the red-shift fo rm u la is a m ath em atical result o f kin em atic al re la tiv ity and affirm s th a t D in g le has not understood this th eo ry. g. c. m c v.

5 2 3 .1 6 :5 3 8 .5 6 .0 2 9 .6 2112

Cosmic static. Re b e r, G .

Astrophys. J.,

100,

pp.

2 7 9 -2 8 7 ,

Nov.,

1944.— N a tu ra lly -o c c u rrin g radio waves reaching the ea rth fro m space are captured by an eq u ato rially -m o u n ted 31 ft. sheet-m etal m irro r o f focal length 20 ft. a t whose focus are a p a ir o f cone antennae tuned to 160 M c /s (1 -8 7 m .) w h ich convert the electrom agnetic energy in to a.c. T h is passes to a 5-stage a m p lifier o f 90 db gain, whose o u tp u t is rectified and drives a pen recorder. A s the earth rotates the (statio n a ry ) m irr o r sweeps o u t a pre­

selected band o f declin atio n and the intensity o f cosm ic static is recorded against rig h t ascension on the ch art. Results fro m 200 charts ob tained du ring 1943, plotted as constant-intensity lines on a celestial globe, o u tlin e the M il k y W a y w ith a m ax. in Sagit­

tarius and m in o r peaks in Cygnus, C assiopeia, Canis M a jo r an d Puppis. L ittle ra d ia tio n em anates fro m points > 3 0 ° fro m the galactic plane, b u t m easurable

am ou nts com e fro m the Sun. a. h u.

523.161 2113

O n the origin o f smoke particles in the interstellar gas. t e r Ha a r, D .

Astrophys. J.,

100,

pp.

2 8 8 -2 9 9 ,

Nov.,

1944.— A th eory is developed to account fo r the fo rm a tio n o f solid particles ( “ sm oke” ) fro m in ter­

stellar gas. A fo rm u la is derived relatin g th e tem ­ p erature o f a sm oke pa rticle to th e n u m b er o f atom s i t contains, assum ing it to be a hetero p o la r crystal.

I f th e gaseous density is less th an a certain charac­

teristic value, th e association o f 2 atom s to fo im a d iato m ic m olecule is determ ined b y th e p ro b a b ility o f rad ia tio n capture. F o r higher densities the fo rm a tio n is analogous to th at o f liq u id drops in supersaturated vapou r. T h e discussion o f the 2 cases shows th at an o p tim u m density (close to the characteristic density) exists fo r sm oke fo rm a tio n . R o u g h estimates fo r the solar neighbourhood, assum ing th a t condensation has proceeded fo r 109y r ., suggest particles o f m ax. size

2000

A,

and to ta l densities o f sm oke particles and o f d iato m ic m olecules w h ich are consistent w ith observa­

tio n. A. HU.

523.165 : 537.591

see Abstr.

2330

523.4 2114

T ita n : a satellite w ith an atmosphere. K u i p e r , G . P.

Astrophys. J.,

100,

pp.

3 7 8 -3 8 3 ,

Nov.,

1944.— P lu to a n d the largest 10 satellites in th e so lar system w ere exam ined spectroscopically on th e 82 -in . M c D o n a ld reflector, and m any o f th e spectrograms arc repro­

duced. O n ly T ita n has a detectable atm osphere, though T r ito n and P lu to requ ire fu rth e r study.

T ita n ’s atm osphere is sim ila r to th a t o f S atu rn , b u t o f less optical thickness: th e C H4 bands at 6 190

A

and 7 260

A

show w ell, an d the N H3 band a t 6 40 0

A

is suspected. T h e presence o f hydrogen- rich gases on a body w ith so sm all a surface gravity indicates th e ev o lu tio n o f th e atm osphere a fte r co oling o f the satellite. S im ila r conclusions fo llo w , though w ith less force, fo r th e atmospheres o f M a rs ,

Venus and the earth. a . h u .

523.74 : 551.510.535 : 537.311.37

see Abstr.

2301

523.746 2115

Provisional sunspot-numbers fo r Decem ber,

1944,

to February,

1945.

Br u n n e r, W .

Terr. Magn. Atmos.

Elect.,

50

, p.

144,

June,

1945.

523.746 2116

Behaviour o f ultra -vio let and daylig ht rays in the solar cycle. As h w o r t h, J. R .

Nature, Lond.,

156,

p.

115,

July

28, 1945.

523.746 : 550.384

see Abstr.

2606, 2607

523.774 2117

S o la r concentration o f the hydroxyl radical. Dw y e r, R . J.

Astrophys. J.,

100,

pp.

3 0 0 -3 0 1 ,

Nov.,

1944.—

A n outstanding discrepancy betw . th e O H concentra­

tio n calculated fro m the observed strength o f th e O H lines in th e spectrum o f th e so lar disk and the con­

centration calculated th erm o d yn am ically is reduced by using an im proved value ( 4 - 3 4 e V ) instead o f th e previously accepted one (5 ■ 0 e V ) fo r the dissociation

energy o f O H . a. h u.

523.78 : 537.591.1

see Abstr.

2334

523.801 2118

N o te on pressure relations within fluid spheres in equilibrium . Se n, N . R .

Bull. Calcutta M ath. Soc.,

36,

pp.

147-152,

Dec.,

1944.— T h re e theorem s are given concerning the m ean pressure w ith in flu id spheres, these fo llo w in g upon e a rlie r w o rk [A b str.

2416 (1939)]. Som e applications o f th e results to th e th eo ry o f S tellar S tructure are discussed. l. s. g. 523.832 : 523.851.3

see Abstr.

523.84 2119

Observations o f variable stars by the A m erican Association o f V a ria b le S ta r Observers. Ca m p b e l l, L .

Ann. Harv. Coll. Obs.,

110, 7,

pp.

2 1 9 -2 6 0 ,

July,

1944.

523.84 2120

Observations o f variable stars by the A m erican Association o f V a ria b le S ta r Observers. Ca m p b e l l, L .

Ann. Harv. Coll. Obs.,

110, 8,

pp.

2 6 1 -3 2 9 ,

Sept.,

1944.

523.841.1 2121

Fo urth outburst o f N o v a (T ) P yxid is. Ca m p b e l l, L .

Science,

101

, p.

42 9,

A p ril

27, 1945.

236

523.841.37 A S T R O N O M Y 523.852.3

523.841.37 2122

O n the anharm onic pulsations in the pulsation theory o f the Cephcid variable.

Roy,

S. K .

Bull. Calcutta M ath. Soc.,

36,

pp.

109-12 1,

Dec.,

1944.— T h e equa­

tio n s o f m o tio n o f a pulsating star are w ritte n in H a m ilto n ia n fo rm and the 3rd order ap prox. to the so lution is considered. T h e results are com pared w ith those o f R osseland [A b str. 47 (1944)] w h o neglected th e th ird and higher o rd e r term s in the dis­

placem ent. A n ex am in atio n is m ade o f th e fu nd a­

m en tal no de o f os cillation an d the effect o f a sm all o verton e on the fu nd am ental. A com plete solution is

given in a special case.

l . s. g.

52 3.841.9 2123

T h e eclipsing system S X Cassiopciac.

Gaposchkin,

S.

Astrophys. J.,

100

, pp.

2 2 1 -2 2 9 ,

Nov.,

1944.— T h e p h otograp hic light-curve' o f this va ria b le is obtained fro m 2 0 4 6 H a rv a rd p a tro l plates a n d com pared w ith th e visual lig ht-curve. T h e curves indicate different du rations o f eclipse and o f to ta lity , an d also different ellipticities. T h e radius o f the A6 co m p on ent is sm aller a t sh orter wave-lengths. C om parison w ith S truve’s spectroscopic observations [A b str. 1251 (1 944)] suggests th a t the blue co m p on ent is surrounded b y a th ic k asym m etrical atm osphere w h ich pro b ab ly envelops the w h o le system. I t is suggested th at other eclipsing variables show s im ila r effects, and th at m odification s m a y be necessary in o u r views o f stellar ra d ii and thence o f the in tern al co nstitu tion o f stars.

A. HU.

523.841.9 2124

T h e eclipsing system R X Cassiopeiae.

Gaposchkin,

S.

Astrophys. J.,

100

, pp.

2 3 0 -2 4 1 ,

Nov.,

1944.— T h e p h otograp hic (2 0 3 7 observations) and visual (324 observations) light-curves o f this va ria b le are com bined w ith S truve’s spectroscopic results [A b str. 2360 (1 944)] to give relative and absolute dim ensions o f t he system. A lo ng-period in trin sic v a ria tio n o f range O'-46 m ag. an d perio d 5 1 7 -6 days is superposed on the geom etrical v a ria tio n . , A n unprecedented difference o f 0 - 1 6 m ag. exists betw . the m axim a. A s w ith S X Cass [A b str. 2123 (1 9 4 5 )], differen t ra d ii are deduced fro m the p h otograp hic a n d visual curves, and an extensive gaseous envelope is indicated.

a. hu.

523.841.9 2125

Th e W o lf-R a y e t eclipsing variable H V I I 086

= H D 214 41 9.

Gaposchkin,

S.

Astrophys. J.,

100,

pp.

2 4 2 -2 5 0 ,

Nov.,

1944.— T h is star, recently studied as a spectroscopic b in ary [A b str. 2363 (1 944)] is fo u n d fro m 1 7 9 5 H a r v a r d p a tro l plates to be an eclipsing va ria b le w ith a lig h t curve o f

p

L y ra e type.

R e la tiv e and absolute dim ensions are deduced, and th e W co m p on ent is shown to be very sim ila r in physical properties to the W com ponent o f V 444 C yg n i [A b str. 814 (1945)]. Its extended atm osphere, th ro u g h w h ich atom s are co ntinuo usly ejected a t high velocity, renders th e o rd in ary conception o f “ radiu s”

in ap p licab le, an d the observed discrepancy betw.

e x cita tio n and effective tem p erature is ap paren t on ly.

a

.

hu

.

523.84 1.9 2126

T h e eclipsing s ta r A R M onocerotis.

Payne- Gaposchkin,

C .

Astrophys. J., 100, pp.

2 5 1 -2 5 4 ,

Nov.,

1944.— T h e ph o to g rap h ic lig ht-curve o f this /9-Lyrae va ria b le is ob tain ed fro m 1 441 H a rv a rd

plates, and relative elements derived fro m this and a visual curve. T h e m ean ra d ii o f th e com ponents appear to v a ry w ith w avelen gth, the ph otograp hic curve giving a to ta l b u t th e visual o n ly a p a rtial eclipse. A bsolu te dim ensions are fo u n d by using a plausible m ass-ratio, and tem peratures are assumed to derive absolute m agnitudes fo r the com ponents.

A. HU.

523.842 2127

A report on new spcctrographic m aterial o f 13 C eti.

Bauer,

C . A .

Astrophys. J.,

100,

pp.

3 0 2 -3 1 0 ,

Nov.,

1944.— T h is star is a visual do u b le whose brighter co m p on ent A is a one-spectrum spectroscopic binary.

F r o m 108 spectrograms taken a t Y erkes betw . 1928 and 1944 th e systemic velocity o f A is shown to v a ry w ith th e relative ra d ia l velocity o f the fa in te r co m ­ p o nent B w ith respect to A , th e c o rrela tio n giving masses

M A

= 1 -8 ,

M B —

0 - 6 in so lar units. N o significant variation s in the spectrum are fo un d, but th e spectroscopic perio d is im proved.

a. hu.

523.842.3 2128

T h e spectroscopic orbit o f A R M onocerotis.

Sahade,

J.,

and Cesco,

C . U .

Astrophys. J.,

100,

pp.

3 7 4 -3 7 7 ,

Nov.,

1944.— F ro m 29 spectrograms ta ken on the 82-in. M c D o n a ld telescope over 3 consecutive cycles in 1944 the spectroscopic elem ents arc deduced by ap p ly in g Schlesinger’s least-squares m eth od to a p re lim in a ry o rb it. A t p rim a ry eclipse the K 0 co m ­ p o ne nt, whose spectrum is th e o n ly one observed, is in fro n t. T h e C a I I lines appear in em ission and share the velocity variation s o f th e K 0 co m ponent;

th ey presum ably arise in an extended atm osphere

a ro u n d the K0 star.

a. hu.

523.842.3 2129

T h e W o lf-R a y e t type spectroscopic binary H D 152 271).

S tru ve,

O .

Astrophys. J.,

100,

pp.

3 8 4 -3 8 7 ,

Nov.,

1944.— T h is is th e first W C star to be discovered as a spectroscopic binary. Its em ission lines are b road and show an expansion velocity o f a b o u t 2 0 0 0 km ./sec. -T h e blended em ission featu re a t 4 6 4 7 -4 686 A . ( C III? C I V , H e I I ) shows a n oscilla­

tio n in w avelength o f period 8 -8 2 days. T h e central absorptions o f the H lines v a ry in the same period but in opposite phase, and m ay arise fro m the second co m p on ent o f th e system, w h ich w o u ld then .b e o f ab sorption O type. A p p ro x . o rb ita l elements are

derived.

a. hu.

5 2 3 .8 5 1 .3 :5 2 3 .8 3 2 2130

T h e rad ia l velocity o f the Pleiades.

Smith,

B .,

and S tru ve,

O .

Astrophys. J.,

100,

pp.

3 6 0 -3 7 3 ,

Nov.,

1944.— F r o m 237 spectrogram s o f 69 m em bers o f this cluster (d o w n to ap paren t m agn itu de 9 - 0 ) the m ean ra d ia l velocity is fo u n d to be + 4 - 0 8 km ./sec.

A large system atic difference o f ra d ia l velocity betw.

m em bers o f h igh an d those o f lo w ro ta tio n a l velocity is unexplained. O n ly 2 spectroscopic binaries are fo u n d , th ou gh 8 m o re are suspected. T h e sm all difference fo un d betw . external and in ternal m ean errors in th e velocities confirm s th a t in tern al m otions are sm all. N o evidence is fo u n d th a t th e velocities depend up on position in th e cluster. T h e results are co m p ared w ith o th e r recent determ ination s, b u t no e x p lan atio n is offered fo r appreciable discrepancies.

a

.

hu

.

523.852.3 : 523.874

see Abstr.

2133, 21 34 237

5 2 3 .8 7 2

523.872 2131

R ela tio n between colour index and effective wave­

length from the observations o f H ertzsprung and V anderlinden. Se a r e s, F . H . , a n d Jo y n e r, M . C .

Astrophys. J.,

100,

pp.

2 6 4 -2 7 8 ,

Nov.,

1944.— T h e relations ob tained by H ertzsp ru n g an d by V a n d e r­

lin d e n betw . effective w avelength and c o lo u r index are recalibrated to the revised in te rn a tio n a l co lo u r system, and co m p ared w ith th e theoretical relatio n co m p uted fo r b lack-bo dy radiators in a previous p a p er [A b str. 343 (1944)]. T h e regression fo rm u la e are given so th a t o th e r extensive observations on the Pleiades an d Praesepe by these authors m a y be reduced to th e in te rn a tio n a l system. T h e agreem ent is satisfactory, and co m p uted effective w avelengths can th erefo re o rd in a rily be used. a. h u.

5 23.872 2132

A change in the spectrum o f 39e C apricorn!. St r u v e, O ., a n d D e u t s c h , A . J.

Astrophys. J.,

100,

p.

390,

Nov.,

1944.— T h e sharp ab sorption cores o f the H lines in the spectrum o f this B 5

pe

star disappeared d u rin g Sept., 1944, and a t present th e appearance is th a t o f an o rd in ary B 3/m star. T h e ab sorption lin e o f M g I I at 4 481

A

also belongs to th e va ria b le shell spectrum an d has disappeared. a . h u . 523.872 : 539.153.4 : 53 7.228.5

see Abstr.

2297, 2298

523.874 : 52 3.852.3 2133

R ed shift in the anagalactic nebulae. Sh n e l d e r o v, A . J.

Nature, Loud.,

155,

pp.

3 3 2-33 3,

M arch

17, 1945.— A p h o to n e m itted by a d istan t nebu la has a mass w h ic h is acted up on by th e g rav itatio n al field o f th e G a la x y . I n o rd e r to satisfy th e requirem ents o f th e la w o f gravitation , o f th e th e o ry o f re la tiv ity a n d o f th e conservation o f energy, th e observed freq u en cy m ust d iffe r fro m th e em itted frequency, th e velocity being k e p t const, by a wavelength adjust­

m en t so as to com pensate fo r th e v a ria tio n due to the acceleration. T h is sh ift o f w avelength increases w ith distance a n d is id en tified w ith the observed red-shift o f th e “ expan din g universe.” a. h u.

5 2 3 .8 7 4 :5 2 3 .8 5 2 .3 2134

Red shift in the anagalactic nebulae. De a c o n, E . L ., a n d Ed g e w o r t h, K . E .

Nature, Load.,

155,

pp.

6 9 9 - 70 0,

June

9, 1945.— T h e th e o ry o f S hneiderov [A b str.

2133 (1 945)] is critic ized o n th e grou nd th a t an e m ittin g n ebu la w o u ld exert o n a p h o to n a grav ita­

tio n a l effect opposite a n d presum ably n e a rly eq ual to th a t o f th e G a la x y . T w o a ltern ative explan ations are offered: one reverses S hneiderov’s m echanism and assumes th a t th e G a la x y is sm aller th an m ost nebulae;

th e o th er suggests a change o f frequency due to ab sorption in in tergalactic space. a. h u.

523.877 ' 2135

The generalized C ow ling model. Ha r r i s o n, M . H .

Astrophys. J.,

100,

pp.

3 4 3 -3 4 6 ,

Nov.,

1944.— T h e C o w lin g m odel is generalized b y considering stars in w h ic h th e convective core a n d th e point-source envelope have differen t m ean m o lec u la r weights

p,

th e ra tio

p j f i c

v a ryin g fro m 1 (th e stand ard C o w lin g m o d e l) to 2. A s th e ra tio increases, the convective core encloses less an d less o f th e mass an d radius, w h ile th e to ta l radius an d lu m in osity o f th e co nfigura­

tio n increase. a. h u.

523.877 2136

A n approxim ate solar model on B eth e’s la w o f e n e r g y g e n e r a tio n . Se n, N . R ., a n d Bu r m a n, U . R .

Astrophys. J.,

100,

pp.

3 4 7 -3 5 4 ,

Nov.,

1944.— T h e s tellar equations o f eq u ilib riu m are used in con­

ju n c tio n w ith B e th e ’s la w in its strict e xpon en tial fo rm to investigate th e ce n tral density fo r a n assigned co m p osition a n d ce n tral te m p era tu re. T w o central densities are fo u n d outside w h ic h th e energy transfer is e ith e r p u re ly ra d ia tiv e o r pu re ly convective.

Betw . th e m a convective-rad iative tran sfer satisfies th e b o u n d ary co nd ition s o n ly fo r a un iq u e central density. A s te lla r m o d e l o f th e la tte r type using a ce n tral tem p erature o f 20 X 106°C . and a H co ntent o f 3 5 % (H e co ntent = 0 ) gives a lu m in o s ity closely eq u al to th a t o f th e sun, a mass 7% larger an d a

radiu s 14% larg e r. a . h u .

523.877 2137

O n the radiative equilibrium o f a stellar atmosphere.

I V . Ce s c o, C . U . , Ch a n d r a s e k h a r, S ., a n d Sa h a d e, J.

Astrophys. J.,

100

, pp.

3 5 5 -3 5 9 ,

Nov.,

1944.— T h e p ro b lem o f lin e fo rm a tio n discussed in a previous p a p e r [A b s tr. 829 (1 945)] is solved n u m e ric ally in the first 3 a p p ro xim atio n s, and tables fo r th e resid ual in ten sity a re given. T h e so lu tio n is co m p ared w ith th e stand ard M iln e -E d d in g to n a p p ro x im a tio n , a. h u.

526.7 2138

T h e international g rav ity form ula. La m b e r t, W . D .

Anxer. J. Sei., 243-A, pp.

3 6 0 -3 9 2 , 1945.

D a ily Vol

.—

T h e g rav ity fo rm u la is developed fro m th e constants o f th e In te rn a tio n a l S ph ero id o f reference; then the fo rm u la resulting fro m an assum ption o f a flu id spheroid o f reference o f mass eq u al to th a t o f the In te rn a tio n a l S pheroid is developed an d discussed.

T h e conclusion th a t th e d e p artu re fr o m th e results o f th e In te rn a tio n a l F o rm u la w o u ld be slight is illu strated by nu m e ric al exam ples. T h e B runs te rm a n d th e controversy occasioned by H o p fn e r ’s reviv al o f B ru ns’ ideas are discussed.

A

lo ngitud e te rm is developed by means o f spherical harm on ics. H y p o ­ theses advanced by geodesists are stated and the im plicatio ns discussed.

527 : 53 8.7 (0 9 )

see Abstr.

2361

53 2139

Physics in 1944. Os g o o d, T . H .

J. Appl. Phys.,

16,

pp.

61—76,

Feb.,

1945.— A review o f research in Physics in 1944, the subjects discussed being X -ra y s , cosm ic rays, n u cle ar disin teg ratio n , atm ospheric showers, th e o ry o f counters, a rtific ia l disintegration, m agn etic lens sp ectrom eter [A b str. 265 (1 945)] and N e w to n ’s rings [A b str. 1201 (1 944)]. l. s. g. 53 : 541.64

see Abstr.

2523

53.081.7 2140

P reparation and physical constants o f acetylenie compounds. He n n e, A . L . , a n d Gr e e n l e e, K . W .

J. Amer. Chem. Soc.,

67,

pp.

4 8 4 -4 8 5 ,

M arch,

1945.

53 .089 .6 : 531.718

see Abstr.

2157

530.1 2141

U nification o f the physical fields. Sa x b y, F . R .

Nature, Land.,

155

, pp.

6 0 9 -6 1 0 ,

M a y

19, 1945.— T h e a u th o r’s th eo ry o f in d eterm in ate space tim e is dis­

cussed in re la tio n to E d d in g to n ’s th e o ry a n d some recent rem a rk s by S chröd ing er [A b str. 86 (1945)].

530.12 : 530.145 : 523.12

see Abstr.

2111

5 3 0 .1 2 :5 3 0 .1 4 5 .6 2142

O n the theory o f the particle o f spin 3/2. G in s - b u r g, V .

J. Phys., USSR,

7, 3,

pp.

1 1 5-12 8, 1943.—

530.12 A S T R O N O M Y — PHYSICS. PRINCIPLES

238