gta
MUCLEAR SCIINCE ARSTRACTS
Vol. 22, to. 3
137° 965) conc: 33 that the detected Morar polarisation signi <2 gither that Lie xredostioe te wyackru. .° radiation of, tf the
Sgalet Gistrfsatie of redisting electrone {e
weivotrepic, et 8
surement procedures used are cutlined. The first
gate for the total vertical steewuation at 59 Ofis a mean valve of 4
dB sed a brightness temperature of approximately 7.690%. (J.28.)
am
4Py IN THE EARLY SOLAR SYSTEM AND CONIRDANT PLUTONIU:
442-4(Now. a, 1967}.
Coscordsst platonfum/nenca and jodine/xepon decay intervala
have bees obtained fo. 2 dozen meteorit-s mostly achondrites.
Plotosiam-344 aad lodine-229 abundances in the early solar ayetem suggest that theee extiact nuclides were synthesized in the
galactic nacleo-asyathesia process, which tasted sevaral billion
years, (auth)
ams
EVIDENCE OF CONTINUUM EMISSION FROM
JUPITER AT 16 Me. Barrow, C. M.; WOliams, J, R. (Florida
State Univ., Tallabeecess). Nature (Loudoa), 316; 462-S(Mov. ¢,
1987).
It was reported earlier that almost continmous ‘burstyradiatian from Jupiter could be detected st lowfregaencise if an asrialsystem of suff;
A
increase tn eralesion Probability at 30.3 Mewas also tamd wateg
the large array at Clark Lake Radio Observatary. Evidesce
presented in this communication of a related effect at 18 Ma a
served on several occasions during the 1966-67 apparition of
Jupiter; this refers to a r
jy ateady
4
appearing as a background to the ‘more sual “bursty” type of
emission, The observations were made with an interferometer
consisting of two ideatical broadside arrays, each consinting of
four whole-wave dipoles, on an E--W bescline of 16 wavelengths.
The event characteristics are tabulated. A total of 17 events out
of 43 observed during the period November 5, 1966 to March 4,
1967 contained evidence of continuum emission. That this effect
waa Bot observed on every occasion presumably indicates thai the
conUncum emissice is either not a frequem occurrence at 18 Mo,
or that ft te sivays present but emuelty of too low invensity to be
recorded (UK
aver
CASE OF THE VANISHED CORRELATION IN STATISTICS OF QUASI-STELLAR OBJECTS,
of Coloredo, Boulder),
1967),
Gamow,G,
(Univ,
Nature (London) 218: 461-2(Nov. 4,
The result of the studies by Longair and Scheuer (Nature 215:
919 (1967}} concerning the possible cor. elation between optical and
radio intensities and red shifte in quasare are discussed. These
authors found that correlation dlasppeared when the effects of rela-
tivietic time dilation were eliminaten An exp‘anation of this disappearance is offered, based on absorption by galaxica. The obeerved
Doppler effect in the absorption lines will correspond not to the
Tecearion velocity of the source, but to that of au iatervening galary. (UD
am
SPECTRA OF SOME BLUE OBJECTS iN HIGH
GALACTIC LATITUDER Dtbat, E, A,; Ealpov, V. F. (Astro~
somical Inst., Moscow}. Sov. Astron. AJ (Engl, Transi,}, 13;
220-3 (Sept-Oct, 1967),
Tranelated trom Astros, Z&., 44: 378~83{(Mar.-Apr. 1967).
A search was made for extragalactic objects among blue slara
in high galactic latiudes, Spectra of Tonantzintla objects 256,
259, 361, 262, 264, 266, 186, 811, 622, and 317 were obtained with
an image tube and'a grating spectrograph at the Cassegrain focus
of the 128-cm reflector. Except for Tom 356, none of the objects
exhibits emission lines. A apectrophotometric study was made of
the quasi-stellar galaxy Tom 256, discovered by Sandage. The
physical parameters of the gapeous envelope are derived from
ths forbiddem-line ineneities. The eimation is found to be similar
to the phenomena observed im Seyfert galaxy suclel, but on 8
larger soske. (math)
am
POSSIBLE POLARIZATION OF BRE MSSTRAMLUNG
X RADIATION FROM SOLAR FLARES. Korchak, A.
Leoatovich, M.A. (net. of Terrestrial Magnetism, lomepheare,
and Radiowsve Propagation, Moaoow}. Dob, Akad. Newk S86K,
173+ 291-4(Mar. 11, 1907), (fe Rtunstan.
An examinatios lp presested of the method of analyzing the
Polarization of hard eolar-flare x radiation inorder to determine
tyrcneosree, Compeoa), Spectfioally, Dolaa's (Astr. Phys. J., 70:
bea
ss
eecond possibility
Oreats
che, ts meaipca in arontor deol hommeenk
as
ot
beams would be mest probable in the
ours of euler fares. Bremeboth for the case
<= paralelebectron tou na well
a tho cone wher fe sec
troae are cagtared in the reaguetie field aad an arquiar velocity
otribution is established. 2 ie concluded that W the exergy
spectrem of electrons accelerated 1» « flare extents inio teBoo
regica, the
wil
both the Comptoa and synchrotros radiation. The degree tock
Lurely dietat from each other in terme of the energy epoctram.
Ty)
we
ON THE NATURE OF THE INFRARED NEBULA iN
Hartrosna, William K. (Univ. of Arison, Tucson).
reraeareing J., 149: LS87-S0qSegt. 1967).
# recently discovered infrared asbuia in Orion is interpreted
ae = preso-caster with 1 to 10! masaive atara imbedded in an
opaque dust cloud. Sollapes 1sshowt to be ur has been reversed,
aad lifetimes of sich objects is the cheerved states are expected
bakep-vepyinre emmanin
(onthe
see
WEGATIVE RESULTS IN A SEARCH FOR RADIO
EMISSION FROM IFRARED AMD T TAURI STARS. Comalls, J.
(Cornell Univ., Arecivo, Pusrto Rico),
MSazt. 1967).
Astrophys. J., 14% LS1-
Tesults were obtained in & search for radio emission
fromthe
the following infrared and T Tauri stare: two objects in
Cygnus sod Taurus, T Teo,
RYTes, aad & Nos. The 1950 0 onordinates, frequeacios of observation, ms! nuvabers of observations
a2 each frequency for cach are tabulated. Al! the obeervations
wers made with the Arecibo 1000-¢¢ telescopes aad Dicke-switched
radiometers. (W.0.M.)
sen
INFRARED RADIATION FROM UPSLLON SAGITTARII.
, Thomas A.; Nariat, Kyofi (Univ, of Arizona, Tucson,
Tokyo Astronomics! Observatory, Mitaka). Astrophys. J., 149-
‘L93-5(Sept. 1967).
Infrared photometry of » Gigr waa undertaken with the hops thet
it would reveal the sature of the secondary componr’.
omen
Tagoitude and colors from three UBVRI observation? 27 th oe
JAKL obeervations are given along with « comparison uf to
colors of » Sgr with those of standard stars. (WD.M.'
soe3
INFRARED OBSERVATIONS OF THE PLANE! >
NEBULA NGC 7027,
Gillett, F.C.
Diexo); Low, F. J.; Stein, W. A,
{Sept. 1987).
(Univ, of Cailforois, n>
Astrophys. J., 149: 97 10
Observations of NGC 7027 were made in May and June 1947
at the Catalina observing station in an attempt to detect en in’
red line of 54+ at A= 10.59 4. Age result of the ooamrvall uk
there was some in(ioation of the detection of the predy ted fine.
Howevertt war discovered that there was a mesmurable conGmmm flux from NGC 7027 in the wavelength range from 7 § to
14 y that compared in value with the strength of stellar radiation
from a Lyr{AC) at about 94. (W.D. mM.)
2m
OBSERVATIONS OF AZ 29. Wampler, F. Joseph
(Univ. of California, Santa Crus), Astrophys. J., 149 Liti-3
Sept. 1967).
Burbidge, Burbidge, aad Hoyle (10@7) beve argued that 7.79
considered by Greenstelo aad Matthows (1967) to be a white dvarl
with a belicm spectrum, may be a tadio-quiet, quasi-stellay ott
Recently Smak (1967) hax reported that the magnitude of H7 7)
vartatle with a period of 16 mia and an amplitude of 6 92 may
th an effort to obtaln additional data, photoe.ectric scan of RZ 19
were obtained usiag the Lick prime~foone scamser at the 120-in
telescope. (WD.M.)
So08
PHYSICAL CONDITIONS IN SCO X-1, Tucker, W. H.
(Cornell Univ,, ithaca, N. ¥.). Astrophys, J.,149: L105-9
Gept, 1967).
Some restrictions on the purametere charecteriziag Sco X-1
are discussed, and 6 model fing Sco X-1 and other x-ray ecurces
{8 euggested. The basic seeumptions are: (1) the x-ray firx 9°
werved tn the 2- tu 30-ke¥ range te due to bremestrah)s ng freon
fe optically thin plasma with s temperature T= 6 < 10", asd
a he gan bas the comic abundances gtrem by Aller (19¢1).
-D.M)