Modern Mathematical Models of Time and their Applications to Physics and Cosmology: Proceedings of the International Conference held in Tucson, Arizona, 11–13 April, 1996

384 Pages·1997·7.36 MB·English

by  Halton Arp (auth.)

MODERN MATHEMATICAL
MODELS OF TIME
AND THEIR APPLICATIONS
TO PHYSICS AND COSMOLOGY
Proceedings of the International Conference held in Tucson,
Arizona, 11-13 April, 1996
Edited by
W.G. TIFFf
Department ofA stronomy, University ofA rizona,
Tucson, Arizona, U.S.A.
and
W.J. COCKE
Department ofA stronomy, University ofA rizona,
Tucson, Arizona, U.S.A.
Reprinted from Astrophysics and Space Science
Volume 244, Nos. 1-2, 1996
SPRINGER -SCIENCE+BUSINESS MEDIA, B.V.
A C.I.P. Catalogue record for this book is available from the Library of Congress.
ISBN 978-94-010-6372-2 ISBN 978-94-011-5628-8 (eBook)
DOI 10.1007/978-94-011-5628-8
Printed on acid-fru paper
AH rights reserved
@1997 Springer Science+Business Media Dordrecht
Originally published by Kluwer Academic Publishers in 1997
Softcover reprint ofthe hardcover lst edition 1997
No part of the material protected by this copyright notice may be reproduced or
utilized in any form or by any means, electronic or mechanical,
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TABLE OF CONTENTS
Preface 1
DAY 1 SESSIONS 1-3
Session 1. The Redshift
HALTON ARP / The pair of X-ray sources across NGC 4258, its relation to
intrinsic redshifts, ejection and quantization 9
JACK W. SULENTIC and J. BRETT SMITH / A fresh look at discordant
redshift galaxies in compact groups 23
W.G. TIFFT / Evidence for quantized and variable redshifts in the cosmic
background rest frame 29
W.M. NAPIER and B.N.G. GUTHRIE / Testing for quantized redshifts. I. The
project 57
T.E. NORDGREN, Y. TERZIAN and E.E. SALPETER / The distribution of
galaxy pair redshifts 65
Session 2. Critical Properties of the Universe
LI-ZHI FANG and YI-PENG JING / Density fluctuations on super-Hubble
scales 73
S.A. GREGORY / The challenge of large-scale structure 81
ANTHONY L. PERATT / Electric space: evolution of the plasma universe 89
J.G. LAROS / Gamma-ray bursts: should cosmologists care? 105
Session 3. Statistical Methods
W.M. NAPIER and B.N .G. GUTHRIE / Testing for quantized redshifts. II. The
local supercluster 111
W.I. NEWMAN and Y. TERZIAN / Power spectrum analysis and redshift data 127
W. COCKE, C. DEVITO and A. PITUCCO I Statistical analysis of the occur-
rence of periodicities in galaxy redshift data 143
P.A. STURROCK I Zooming in on the redshift problem 159
DAY 2 SESSIONS 4-5
Session 4. New Approaches to Cosmology
G. BURBIDGE I Two universes 169
JAYANT V. NARLIKARI Anomalous redshifts and the variable mass hypothesis 177
W.G. TIFFT I Three-dimensional quantized time in cosmology 187
Session 5. Gravitation and Time in General Relativity
W.J. COCKE I The stress-energy tensor and the deflection of light in 6-
dimensional general relativity 211
P.C.W. DAVIES I Einstein's greatest mistake? 219
ROGER PENROSE I Time, space and complex geometry 229
D.E ROSCOE I Discrete spatial scales in a fractal universe 231
TOM VAN FLANDERN I Possible new properties of gravity 249
LEOPOLD HALPERN I On the cosmic limits of physical laws 263
MENDEL SACHS I Changes in concepts of time from Aristotle to Einstein 269
METOD SANIGA I On the transmutation and annihilation of pencil-generated
spacetime dimensions 283
DAY 3 SESSIONS 6-7
Session 6. Nuclear and Particle Physics
VINCENT ICKE I Particles, space and time 293
AVSHALOM C. ELITZUR I Time anisotropy and quantum measurement:
Clues for transcending the geometrical picture of time 313
ARI LEHTO I 3-D Period doubling and magnetic moments of particles 321
C. WOLF / Relics of the primordial origins of space and time in the low energy
world 329
L.W. MORROW I Unexplained empirical relations among certain scatterings 347
MARTIN KOKUS I Spherical rotation, particles and cosmology 353
Session 7. Mathematical Models and Methods
CARL L. DEVITO / A Non-linear model for time 357
W.M. STUCKEY / Defining spacetime 371
A.P. PITUCCO / Some elementary geometric aspects of extending the dimen-
sion of the space of instants 375
B.R. FRIEDEN / Fisher information as a measure of time 387
THE RED SHIFT
CRITICAL PROPERTIES OF THE UNIVERSE
STATISTICAL METHODS
DAY 1
Rodeway Inn, North
:~ iP1"'r'"''""'li'it,;m;iitlru,iil r.~iitfl!rl!n~ on ModernMathematlCa1 MO(IelS
Applications to Physics and Cosmology_
. April 11-14. 1996 Tucson
Figu.re 1. Sketch art courtesy Janet A. Tifft
THE PAIR OF X-RAY SOURCES ACROSS NGC 4258:
ITS RELATION TO INTRINSIC REDSHIFTS,
EJECTION AND QUANTIZATION
HALTON ARP
Max-Planck-Institut fur Astrophysik
85740 Garching, Germany
Abstract. The chance that the pair of X-ray sources observed across NGC
4258 is accidental can be calculated as 5 x 10-6. The recent confirmation
as quasars, and determination of the redshifts of the pair, at z = 0.40
and 0.65 by E.M. Burbidge enables the final accidental probability of the
configuration to be calculated as < 4 x 10-7. In addition there are a number
of observations which indicate the central Seyfert galaxy is ejecting material
from its active nucleus.
The NGC 4258 association is compared to four other examples of close
association of pairs of X-ray quasars with low red shift galaxies. It is con
cluded that in each of these five cases the chance of accidental association
is less than one in a million. The ejection speed calculated from the red
shift differences of the X-ray quasars is 0.12c. This agrees with the ejection
velocity of O.lc calculated in 1968 from radio quasars associated with low
red shift galaxies. When corrected for ejection velocities the observed red
shift peaks become narrower - simultaneously strengthening the ejection
origin for quasars and the quantization property of their redshift.
1. Introduction
The first associations of high redshift quasars with low red shift galaxies was
made more than 30 years ago (Arp 1966b, 1967, 1968). The most recent,
striking evidence has come from X-ray sources, paired across Seyfert galax
ies, which have turned out to be quasars of considerably higher redshift
than the galaxy (Radecke 1996, Arp 1996). Evidence for smaller intrin
sic redshifts of galaxies has also accumulated (Arp 1994b). The evidence
Astrophysics and Space Science 244:9-22,1996.
© 1996 Kluwer Academic Publishers.
10 HALTON ARP
demonstrates that part of the redshift of these extragalactic objects must
be intrinsic (non-velocity).
The pairs are particularly important in that they allow us to estimate
the ejection velocities necessary to get the quasars out of their parent galax
ies. In the cases available, if the ejection velocities are subtracted from the
component quasar redshifts, the two members have more closely the same
redshift - as if material of the same intrinsic redshift was ejected in oppo
site directions. After correction for the velocity component, the redshifts
also fall closer to the well marked peaks in the redshift distribution (Arp
et. al. 1990). Therefore quantization of the red shifts becomes more clearly
established. The fact of quantization independently reinforces the earlier
result that the quasar redshifts are not primarily due to velocity but to
an intrinsic property of matter. Perhaps most important of all, existence
of quantization represents one of the strongest empirical clues to the phys
ical reason for the intrinsic red shifts of these recently ejected, compact,
energetic objects.
2. Ejection
It has long been accepted that radio galaxies eject material out in roughly
opposite directions to approximately equal distances from their active nu
clei. It has even been possible to study optical emission from material within
these radiolobes (egs. see Fosbury 1984 and Morganti, Robinson and Fos
bury 1984). More recently, as X-ray observations began to accumulate, it
appeared that material which emits high energy X-rays also accompanies
these radio ejections. Some well known examples are X-ray jets within the
strong radio ejections from Virgo A and Cen A (egs. Feigelson et. al. 1981),
the X-ray hot spots within the lobes of Cyg A and the X-ray material
extending far out along the ejection direction in Cen A (Arp 1994a).
It seems, therefore, that both radio emission and X-ray emission are
characteristic of the material ejected from galaxies. It should then perhaps
not be surprising when the phenomenon of X-ray sources paired across
active galaxies starts to turn up in the same way that pairs of radio sources
were initially discovered across (what later turned out to be) galaxies with
active nuclei. The study of these X-ray pairs and associations will have
to proceed empirically as did the early association of radio pairs. Now,
as then, the first step is to test the statistical significance of associations
and build up a list of secure associations in which to study their empirical
characteristics.
The identification of secure associations must utilize the a priori cri
terion of tendency toward: 1) opposite ejection 2) equal separation and
3) similarity of ejected sources. All these are demonstrated properties of
X-RAY SOURCES 11
accepted ejections and rule out any question of a posteriori probability cal
culations. Since in many of the X-ray cases (as in a number of previous
radio and optical associations) objects of differing redshifts are identified,
one cannot interpret them on the basis of a present theory or understanding
of ejection mechanisms (if indeed it is solely an ejection phenomenon). A
number of cases must be accumulated, studied and a working theoretical
explanation suggested from an inductive analysis.
In order to make the a priori statistical criteria specific we refer to the
early data of pairing of radio sources across active and disturbed galaxies:
The Atlas of Peculiar Galaxies (Arp 1966a) showed numerous cases of ra
dio sources paired across galaxies, particularly in that section containing
galaxies with morphological evidence of ejection. The improbability of these
paired radio sources being accidental resided principally in the closeness of
the sources at their brightness and secondarily in the tendency for the
sources to be aligned across the central galaxy and tertiarily to be equally
spaced across the galaxy (Arp 1967). Although some sources were aligned
to within ±1°, the average over the 26 original associations was 12°.7, of
the order of alignment of radio lobes and knots which are conventionally
believed to have been ejected from active galaxies.
A follow-up analysis of pairs of radio sources in the Parkes Survey (Arp
1968) showed those pairs which had galaxies located between them had sim
ilar properties, demonstrating physical association. Of these radio sources
in pairs, 16 were identified as quasars and disturbances in some of the
central galaxies indicated the time since ejection. This enabled calculation
of ejection speeds for the quasars of O.lc. In an important result of the
present analysis, just this predicted velocity is now calculated directly from
the measured redshifts of the pairs of X-ray quasars across such galaxies as
NGC 4258 as well as in previous associations of pairs of X-ray quasars.
3. The NGC 4258 Configuration
ROSAT X-ray measures of a 20' radius field around the active Seyfert II
galaxy, NGC 4258 revealed a striking pair of X-ray sources aligned across
the center of the galaxy (Pietsch et. at. 1994 and Fig.1 here). The authors
commented: "If the connection of these sources with the galaxy is real they
may be bipolar ejecta from the nucleus" .
Us ing the parameters listed in Tables 1 and 2 of Pietsch et. at. we
construct Table 1 here showing the properties of the two sources. The fluxes
(Fx) are computed in two steps: First the 0.4 to 2.4 keY band counts = B
are obtained from B = s~ss (1+HR1). Then the count-to-energy conversion
factor of 1.4 x lO-l1erg em-2 cts-1 (see Pietsch in Arp 1994a) is used to
compute Fx. This Fx is close to the system of Hasinger et. at. (1993) and we
12 HALTON ARP
0
o
NGC 4258
•
o •
'pSp~·
ROSAT
0.1-2,4 keV , .
.6
(j.
•
.,
.'!'
'0
<>
•
..
•
@
.
•
0 •
.
. .
®.
5 arcmin.
9 ' . , I
•
Figure 1. The pair of X-ray sources across NGC 4258 as discovered by Pietsch et. al.
= =
(1994). #26, with z .65, is to the NE and #8, with z .40, is to the SW. The blue
stellar objects are seen at the center of each source.
can therefore use their log N(> S) - log(S) curve to compute the density
of sources of the strength of #26 and #8 in an average field. That density
comes out to be about 5 and 2 per deg.2 respectively.
TABLE 1. Parameters of X-ray Pair
r p.a. F", (0.4 to 2.4 keY) HR1 ct rate
arc min deg X 10-13 (cgs) xlO-3s-1
Source #26 (NE) 9.66 73.3 0.8 -.4 17.9
Source #8 (SN) 8.57 256.6 1.4 - .2 25.1