2338
PHYS:CS (GENERAL)
Astrophysics and Cosmology
23546
EXPLORATION OF TRE UNIVERSE, SECOND
ELfTION, Abell, George. New York; Holt, Rinchart, and
Winston (1989, 739.
This book is designed for s one~ or two-semester Course an an
(ntroduction to astranomy and astrophysics No apectal training in
ecience or matiematics is required for an understanding of the
text The book ts Itberally illustrated tn black and white and some
color. (W.D.M)
Cosmic Ray Exposure Ages
23547
DATING OF METEORITES BY THE HIGH-TEMPFRATURE RELEASE OF IODINE-CORRELATED!Xe, Podosek,
FLA. (Univ, of Caltfornia, Berkeley),
Acta; 34: 341-65(Mar 1970},
Geochim. Coamochim,
Correlations between the amounts of "Xe and "Xo released in
atepwine heating of peutron-irradiated meteorites were uted to
determine the initial ratio "1/"?) and hence 2 relative formation
time for the various samples. The formation timea In millions of
years fretative to the L4 chondrite Bjurbdle} of nine specimens
are as follows -3 9 + 0.7 for Karoonda (C4 chondrite); 3.1 4 0.6
and 10.5 + 0 7 for the matrix and chondrules, respectively, of
Chainpur (LL3), 7.5 ¢ 19 for St. Severin (L.L6);
3.942 9 and
23.410 for the matrix and chondrules, reapectively, of Allegan
(45), 3.6 + 0.7 for Pefis Blanca Bpring and 20.8 ¢ 9.5 for Bishop-
sille faubrites), 3.8 + 6.7 for a silicate inclusion of the fron me-
teorite El Taco (Campo del Clelo) No aseumptione were made
about the amount of "Xe in the trapped gas. The correlations for
previously) published data were aleo recalculated in the same way,
with no assumptions about trapped '*Xe. For a group of chondrites
previously reported to be isochronous with a mean simultancity of
25 miflton years, the recalculation confirms this mezn simulta-
neity, but significant differences in formation times are resolved,
An iodine — xenon age of 53 + 9 million yeare (after Byurbole) was
obtained from unpublished data for the achondrite Lafayette. The
re‘iability of iodine - xenon ages of individual meteorites la considered; in particular, the ages of Bishopvilie und Lafayette are
jess reliable than those of most other meteorites studied, cspeclally in view of the anomalous ages reported. The re:evance of
iod:ne xenon dating to theories of nucleosynthesis, earty solar
system chronology, and theories of meteorite parent-body forMation ts discussed (auth) (CK)
Stars
Reter also to abstracts 23762, 23976, 24435, and 24516.
23548
(S¥0-3962-2}) ANNUAL PROGRESS REPORT [ON
AUCLEAR PHYSICS AND NUCLEOSYNTHESIS], {Cameron,
ALG. W.)
Science),
CFsTt.
(Yeshiva Univ,, New York. Belfer Graduate School of
(17 Mar 1970], Contract AT(30-1)-3962, llp. Dep.
Abreef summary is given on the work carried out in the areas
of neutron-star matter, neutron-rich nuclei, the URCA process In
white dwarte, end the nuclear mass formula, (W DM.)
23849
LIGHT VARIATION OF FOUR MAGNETIC VARIABLE
STARS, van Genderen, A.M, (Leiden Observatory}. Astron.
Astrophys,, Suppl, Ser.; 1: 123-7(Feb 1970),
Photoelectric observations of the magnetic variable stars
HD 8441, 2) Per, « Cas, and HD 25 384 are detailed. The first
three stare were ohserved with a red filter only, the fourth one
wan also observed In UAV (auth)
23350
PHOTOELECTRIC OBSERVATIONS OF 323 CYGNI.
Sohansen, K sren T.; Rudkjocbing, J.; Gyldenkerne, K. (Univ,
of Copenhagen Observatory, Brorfelde, Denmark}, Astron,
Astron, Astrophye., Suppl, Ser.z 1: 149+64(Feb 1970).
The tong pertod eclipeing binary 32 Cyg was observed at
Copenhagen Unis eraity Observatory in Brorfeide during the 1959,
1967, and 1985 eclipses. The observations were made with UBV
alandard {tere and several narrow-band filters, and the comhined light curve te disccesed A compartecn tx made with ress hrined ty other observers Atleast the 1965 eclipse
ws
1
tat
cet
meat
wee
tw tital The atmospheric nature of the eclipes ie
ote try the Fact that at a certain phase outside totality
‘. 4 fraction of the B ortar ractietion depends an the
feafregton
footatrvatden
‘auth
2308!
PHOTOELECTRIC OBSERVATIONS OF EARLY A
STARS, Johsnern, Karen T.; Gyidenkerne, K, (Univ. of Copene
hagen Observatory, Brorielde, Denmark). Astron. Astrophys.,
Suppl, Ser.; i: 165-8 Feb 197,
Photoelectric observations of the £ index and of indices atmilar
to those af the Strdmgren uvby system were made for 437 Cald
stars and for a number of stacs te the Coma Berenices, Praeaspe,
NGC 6633, and NGC 1662 clusters, Of the field stars, 377 are
AO— A2 atars north of dociination ~8° with V « 4.0; in the clustera
mostly A stars were observed. The night-to-night correction
method is described and the transformation of the observed
indices to the uvby and § standard syatems js discussed in dotatl,
auth)
7
23582
CATALOGUE OF PROPER MOTIONS FOR 487 A
STARS, Olsen, Ht. J. Fogh (Univ. of Copenhagen Observatory,
Brorfelde, Denmark), Astron, Astrophys, Suppl. Ser.; 2; 189-
97(Feb 1970).
Proper motions and radial velocities are given for 437 A stars
observed photoelectrically by Johansen and Gyidenkarne. Most of
the proper motions are improved GC motions transformed to the
FK4 systenr. (auth)
23883
NARROW-BAND PHOTOMETRYOF LATE-TYPE
STARS, Heeggkvist, L.; Oje, T. (Uppsala Astronomical Observetory). Astron, Astrophys., Suppl. Ser.; 1: 199-232(Feh
2970).
The distribution of stare in the direction perpendicular to the
galactic plane {a investigated. It le limited to late-type stars,
which are studfed by means of interference filters; the break at
the G band and the cyanogen absorption are measured, The catalog
includes al! late-type etars brighter than V = 5 north of declination —10° and those brighter than V = 4 north of galactic latitude +
60°. The relation between the two-dimensional classification
establihed for the G and K stars and the MK classification la
studied. It te shown that the giants and the dwarfs are wel! separated from each other and that the separation can be made complete ff the criteria ate complemented by the B-V color, It is
also found that the M gianta can be classified quite accurately by
‘means of the same criteria
The connection hetween the spectro-
photometric criteria and the intringic colors In the UBV system
1a Investigated, and ft is found that different relations hold for the
and the giants. The mean errors of typical B-V color
e derived from the criterta and B—V are about +0 02 for
the dwarfs and 49.03 to 40 03 for the giants. The absolute magnitudes of the late-type giants are discussed and a relation between the mean absolite magnitude in a volume of space and the
epectrophotometric criteria is derived from astrometric data
only (trigonometric parallaxea and proper motions in combination
with radial velocities). The diapersion of the sbsciute magnitudes
ls about 406. (auth)
23854
CASE B OF MASS EXCHANGE IN SYSTEMS 4+ 3.2Mo
AND 441.6Mg. Harmanec, Petr (Astronomical Inst., Ondrejov,
Czech.). Astrophys. Space Sct , 6: 497-503(Mar 1970)
Two examples of caze A of masa exchange ure computed to
estimate the effect of bagic initia! perameters on the course and
the results of mase exchange. It seems that the resulting mass ~
of the original primary 19 independent of the initial mass ratio,
the resulting orbital period 1a Independent of Initial mase of the
primary, and surface hydragen content 1s independent of both of
these parameters
(auth)
23858
ONE EXAMPLE OF MASS EXCHANGE IN CASE AB
Crech.)
Astrophys Space Sel., 6: 492-6{Mar 1970)
IN SYSTEM 5MQ + 4M>.
Hora, J
(Astronomical Inet , Ondrejov,
Evolution af a binary system with masses of 5Mo end 4M,
reapectively, and with orbital period of 1.41 days is studied by
means of
'y model
under
of conservation of total masa and total orbital angular momentum
of the system. Asa result of mase exchange between the components a binary with masees of 8.46 and 0.54 Mo is obtained
Phyalcal parameters of the final product indicate possthle conthe end af mses exchange, (ath)
33856)
DEVELOPMENT OF A COCOON STAR. Davideon,
Kris (Corneil Untv., Ithaca, N. Y.). Astrophys. pace Sc1.; 6:
422-34(Mar 1970},
A beowly fortied masaive star le Likely to be surrounded by
dense gas and dust sa {tt approaches the main sequence Radiation
preseure must push some of the ianer material outward hefore