.
:
tt
lntetetan hn anaced ah VE eee Pals
(FOIb)
shows
:
:
abe aba
of Ps
absorption
lines
of
References and Notes
Summary
Already
beyond doubt that O and BO super-
lengths in §, ¢, and ¢ Orionis.
During four Aerobee flights Stecher
(20) has scanned the spectra of at
atmospheres.
The spectrum
8, T. A. Chubb and E, T, Byram, Astrophys. J.
138, 617 (1963); E. T. Byram, T. A. Chubb,
M. W. Werner, Ann. Astrophys. 28, 594
(1965),
while in Sirius (A1V) the main feature is the Mg II resonance doublet.
On 20 September 1966 Jenkins and
Morton (79) flew an all-reflective //2
spectrograph on an Aerobee rocket,
and obtained spectra of eight stars in
Orion with about 1-A resolution. These
photographs confirmed the earlier results of the wavelength shifts in the
C IV and Si IV absorption lines and
the unexpectedly weak interstellar Lyman-q
lines.
The
wavelength
range
least ten hot stars with 5- and 10-A
resolution longward of 1100 A. He also
has found the C IV and Si IV resonance lines to be in emission with ab-
sorption components to shorter wavelengths in some of the stars. On an
Aerobee launched on 16 March 1967
Carruthers (27) used a windowless image
intensifier to photograph spectra of
some 12 stars from 1030 to 1400 A
with 2- to 3-A resolution. He con-
firmed the shifts of some of these lines
in £ Orionis and found the same phenomenon in ¢ Puppis, y Velae, and
« and « Orionis. Both the spectral data
and photon counters lead him to suggest that the photon flux decreases
shortward of 1150 A even in the
hottest stars.
According to theories of model stellar atmospheres only stars of spectral
types from O to about B3 may be expected to be bright in the ultravioletwavelength region. Observations of the
strong resonance lines between 911.6
and 1900 A will yield new information permitting construction of better
models for the outermost layers of OB
stars. However, an adequate theory of
line-formation, including non-l.t.e. effects, should be used if an accurate
physical representation
it
has
been
is
to
result.
demonstrated
giants are surrounded by expanding
between
1900
and
3000 A is formed chiefly in the same
layers of the star as is the part of
the spectrum observed with groundbased equipment; consequently, groundbased observations can be used to establish an adequate model. With such
a model, observations of the absorption lines due to the first and second
ions of the metals should permit new
and reliable determinations of the abundances of Fe, Cr, Mn, and Ti in B
stars.
The photometric and the spectral observations so far available of O and B
stars do not generally conflict seriously
with the predictions of theory, provided
that we use line-blanketed models for
the comparison and that we correct
for the effects of interstellar reddening
when necessary.
=a
was extended to 1130 A and revealed
absorption lines of N V, Si III, and
C Ialso shifted to shorter wave-
1, A. B. Underhill, Publ, Dominion Astrophys.
Obs. Victoria, B.C. 11 433, 467 (1962).
2, The flux F, per unit wavelength, which is
more relevant to observational procedures,
is cFy/\*; F, in the ultraviolet probably
exceeds that in the visible for types even
later than B4.
3. D. M. Mihalas and D. C. Morton, Astrophys.
J, 142, 253 (1965); C. Guillaume, Bull.
Astron, Inst. Neth, 18, 175 (1966). In the
first paper the detailed shape of the strong
ultraviolet-absorption lines is taken into account: in the second, the line profiles are
represented by rectangles.
4. D. C. Morton, Astrophys. J. 139, 1383 (1964);
141, 73 (1965),
5. C. Guillaume, W. van Rensbergen, A. B.
Underhill, Buil. Astron. Inst. Neth. 18, 106
(1965); C. Guillaume, ibid.. p. 175 (1966).
. E. W. Elst, fbid, 19, 90 (1966).
. E, T. Byram, T. A. Chubb, H. Friedman,
J. E. Kupperian, Astron. J. 62, 9 (1957); J.
E. Kupperian, A. E. Boggess, J. E, Milligan,
Astrophys. J, 128, 453 (1958); E. T. Byram,
T. A. Chubb, H. Friedman, ibid. 139, 1135
Mg I, Mg HU, Si I, Fe I, and Fe II
beiow the earth’s atmospheric cutoff,
(1964).
9, A. M. Smith, Astrophys. J. 147, 158 (1967).
10. J. D. Alexander, P. J, Bowen, M. J. Gross,
D. W. O. Heddle, Proc. Roy. Soc. Ser, A
279, 510 (1964).
11. I. S. Gulledge and D. M. Packer, Astron. J.
68, 537 (1963); personal communication.
12, A. E. Boggess, Ann, Astrophys. 27, 805
(1964); A. E. Boggess and J. Borgman.
Astrophys. J. 140, 1636 (1964).
13. R. D. Bless, A. D. Code, T. E. Houck, J. F.
McNall, D. J. Taylor, Astron. J. 70, 667
(1965).
14. T. P. Stecher and J. E. Milligan, Astrophys,
J. 136, 1 (1962); T. P. Stecher, Astron. J. 70,
643 (1965); Astrophys, J, 142, 1683 (1965).
15. D. C. Morton and L. Spitzer, Astrophys. J.
144, 1 (1966}; D. C. Morton, ibid. 147, 1017
(1967).
16. M. E. Stone and D. C. Morton, ibid. 149,
29 (1967).
17. R. Wilson, Publ. Roy. Obs. Edinburgh 2,
61 (1958),
18. K. G. Henize, L. R. Wackerling, F. G.
O’Callaghan, Science 155, 1407 (1967).
19. E. B. Jenkins and D. C. Morton, Sky and
Telescope 33, 162 (1967); Nature 215, 1257
(1967}.
20. T. P. Stecher, paper presented at Yerkes
meeting of Amer. Astron. Soc., 1967.
21. G. R. Carruthers, Astrophys. J. 148, L141
(1967); ibid., in press.
(6), Delgado (7), MacLean (8), and
others are significant in this connection.
On the other hand,it is surprising that
Causality, Consciousness, and
Cerebral Organization
the physiologists show some reluctance
to teach psychological concepts. More
than a minimum knowledge of the relationship between brain and psychological function is essential for students
in biclogy and medicine, both because
Walter R. Hess
Psychology has been largely, if not
exclusively, regarded as being in the
domain of philosophy, and, until recently, reference to the brain as the
substrate of psychological function was
infrequent. It should be admitted that
regional differences of approach exist;
for example. in the United States psy§ DECEMBER 1967
chological concepts are influenced more
by the natural sciences than they are
in tradition-bound Europe. The works
of Herrick (/), Lashley (2), and Hebb
(3), the publications of the experimentally oriented Canadian neurosurgeon
Wilder Penfield (4), and more recent
noteworthy works of Kliiver (5), Ploog
this function plays a role in the biology of men and the other higher mammals and because such knowledge is
necessary for an understanding of mental illness. For all these reasons, an ef-
fort to survey psychological problems
in biological perspective seems justified.
If a series of events relating to our
past experience comes to our attention,
we feel compelled to look for a causal ~
.
The author is professor emeritus of physfology,
University of Ziirich. Ziirich. Switzeyland: 1779