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Theoretical Studies, Astrophysics, and Cosmology In collaboration with the group of mathematicians of Warsaw Technical University, HELLER continued the program on applications of noncommutative geometry to physics. They have made substantial progress in constructing a model unifying general relativity and quantum mechanics. Since the model is based on a finite group, it was possible to compute it in all its details, resulting in clarification of several problems encountered in previous work. HELLER continues to research the status of time in relativistic cosmology and, in particular, in fundamental theories based on noncommutative geometry. In the latter theories, time is not given a priori but emerges out of the primordial atemporal (and aspacial) physics. He is also working on the problems, both technical and conceptual, connected with the Majid program to construct the fundamental physical theory based on the theory of quantum groups. STOEGER and ARAÚJO (Universidade Federal do Rio de Janeiro) are nearing completion of their project of specifying and implementing a detailed procedure for solving the Einstein field equations in observational coordinates with cosmological data functions for general perturbations to Friedmann-Lemaître-Robertson-Walker (FLRW) cosmological models. This includes both the case in which there is just dust (pressure-free matter) and the more difficult case in which there is both dust and vacuum energy (a cosmological constant). STOEGER AND RIBEIRO (Physics Institute, Universidade Federal do Rio de Janeiro) are beginning to extend their completed work, relating galaxy luminosity functions to relativistic energy density and to number counts in the case of Einstein de Sitter cosmologies (flat universe models), to other FLRW cases, including those with a non-zero cosmological constant (vacuum energy). Once that is finished, they will be applying their approach to Lemaître-Bondi-Tolman cosmological models (which are isotropic, but not spatially homogeneous) and to perturbed-FLRW models. They also are beginning to investigate how to include improved models of galaxy number and luminosity evolution in their procedure. Following up on earlier work he did with ELLIS, DUNSBY, and McEWAN (Department of Mathematics, University of Cape Town), STOEGER is continuing his investigations of mixed radiation-vacuum energy epochs in the very early universe, just after the Planck era and just before inflation. This study hopefully will shed further light on the constraints that adequate inflation places on the relative amounts of radiation and vacuum energy at these early times and, therefore, on some of the conditions necessary for inflation itself. Connected with this work, STOEGER is also pursuing research on the very difficult question of how possible Planck-era processes could set the size and the requisite smoothness for the pre-inflationary patch from which our universe evolved. This requires careful consideration of time and causality during the Planck (quantum cosmology) era itself¾issues that are far from resolved in quantum cosmology. Closely connected with these efforts, STOEGER has been participating with ELLIS, MURUGAN, and TSAGAS (Department of Mathematics, University of Cape Town) in working out the details of how an inflationary universe, with a single minimally coupled scalar field having a physically acceptable potential, can begin from an initial asymptotic Einstein static state (without a singularity) and emerge after inflation into a standard hot Big Bang evolutionary phase. It appears that none of the characteristics of the model is at odds with current observational constraints. ELLIS and KIRCHNER (Department of Mathematics, University of Cape Town), with STOEGER, have completed preliminary work on the cosmology of multiverses, which are ensembles of many universes or universe domains. These have received a great deal of attention recently, both as the natural outcome of the originating process that generated our own universe, and as an explanation for why our universe appears to be fine-tuned for life and consciousness. In their work so far, they have carefully considered how multiverses should be defined, stressing the distinction between the collection of all possible universes and ensembles of really existing universes. It is only ensembles of really existing universes that provide a possible resolution to the fine-tuning problem. Furthermore, it is very clear that such realized multiverses are by no means unique. To define them adequately, a proper measure on the space of all really existing universes or universe domains is required, so that probabilities can be calculated. And for each such multiverse a distribution function is also needed to specify which, and how many of each, possible universes are realized. Physically, this means there must be a cosmogonic process, such as Andrei Linde's “chaotic inflation,” which is capable of generating the really existing multiverse with its given distribution function describing the variety of universes it contains. This indicates that any really existing multiverse we consider must have some common generating mechanism or process. It appears, furthermore, that really existing universes cannot have an infinite number of members, since there are strong philosophical arguments against any realized infinity. Infinity is not a specifiable number that can be concretely instantiated. Finally, ELLIS, KIRCHNER, and STOEGER address the issue of the stability of multiverses. Obviously, they are not directly testable¾we will never be able to observe, or receive information from, other universes. However, though it may seem unlikely, we may be able to confirm their existence indirectly. This is possible if there are cosmological theories relying on the existence of multiverses that enjoy long-term success and fruitfulness, that is, they provide greater and greater well-confirmed intelligibility for our universe and the characteristics it possesses. This would mean, for instance, that we were able to determine that our universe originated by some process, driven by a specific type of potential, that explains the detailed history and physics of our universe¾including its propensity for complexity and life¾and which at the same time would more than likely produce many other universes of different types. Ideas for such potentials have been suggested, but so far none of them are particularly compelling or well constrained. ELLIS, KIRCHNER, and STOEGER are currently preparing another paper focusing in detail on the philosophical issues raised by multiverses. With LISZKA (Swedish Institute of Space Science, Sförs) and PACHOLCZYK (Steward Observatory, University of Arizona), STOEGER is extending and solidifying earlier work on reliable detection and modeling of low-level quasi-periodic and deterministic X-ray variability from quasars and active galactic nuclei (AGN), particularly from Seyfert I galaxies. These phenomena are connected with the presence of supermassive black holes, or clusters of black holes, in the core of these massive systems. Liszka now has several clear X-ray signals from NGC 5548 that could be interpreted as the signature of a bright flare, or flare patch, spiraling into a medium-sized black hole. WHITMAN continued work on his project of exposing the real irreducible representations of real forms of the simple complex Lie algebras. He presented six lectures on this topic to the Clavius Group of Mathematicians (see Conferences, section III. Observatory and Staff Activities). This material is essential for understanding Lie groups, and it is not easily found nor well organized in the literature on this subject. This is the reason that WHITMAN decided to make this material more accessible. Extragalactic Research In their project studying star formation in the local universe, FUNES along with KENNICUTT, AKIYAMA, LEE (Steward Observatory, University of Arizona), and SAKAI (University of California, Los Angeles) have finished the H-alpha imaging of a complete sample of nearby galaxies within the local eleven megaparsec volume (300 galaxies in the northern hemisphere and about 70 galaxies in the southern one). The observations were carried out with the VATT, the Steward Observatory 90-inch Bok Telescope at Kitt Peak, and the Cerro Tololo Inter-American Observatory 0.9-m telescope, Chile. The data have been fully reduced and now analyzed. The survey has the following goals: (1) to construct the local star formation rate (SFR) distribution function as a reference for cosmological look-back studies; (2) to develop new diagnostic measures of the rate and distribution of star formation in galaxy populations; (3) to quantify the role of starbursts in the evolution of low-mass galaxies; (4) to quantify the incompleteness biases in star-formation surveys; (5) to study the environmental dependence of the SFR distribution function; and (6) to provide a reference catalogue and image database for use by workers in the field. Star-forming galaxies in the local universe provide important clues for understanding the evolutionary properties of galaxies and the physical processes that drive that evolution. MINNITI (Pontifical Catholic University of Chile), REJKUBA (European Southern Observatory), and FUNES continue the study of the nearest giant elliptical galaxy NGC 5128 (Centaurus A) in their search for SFR in globular clusters. MINNITI, REJKUBA, FUNES, and KENNICUTT have used images from the Very Large Telescope (VLT) at the European Southern Observatory in Chile to identify the ionizing source centered on the largest HII region of NGC 5128. This source turns out to be a close pair of bright and blue star cluster candidates. Spectroscopy obtained with the Magellan II telescope (Las Campanas, Chile) confirms that these are massive young clusters, and the radial velocities confirm the physical association with the giant HII region. Dynamical models predict that binary clusters with these properties would merge in a short timescale of a few orbital periods. The discovery of this binary cluster suggests that mergers of young massive clusters could lead to the formation of the most massive globular clusters such as Omega Centauri in our Galaxy and G1 in M31. FUNES, REJKUBA, MINNITI, AKIYAM, KENNICUTT, and THILKER (Johns Hopkins University, Baltimore) are studying star formation in the disk of NGC 5128. Little quantitative progress has been realized in recent years on the issue of NGC 5128’s continuing star formation. Using VLT images of the innermost regions, they identify young stars and blue clusters plus old globular clusters embedded in the dusty regions of the NGC 5128 disk. In addition, H-alpha images are used to derive the HII region luminosity function effectively constraining ensemble characteristics of those clusters formed most recently. The study of satellite galaxies can provide information on the merging and aggregation processes that, according to the hierarchical clustering models, form the larger spiral galaxies. With the aim of testing hierarchical models of galaxy formation, FUNES, GUTIERREZ (Instituto de Astrofísica de Canarias, Spain), PRADA (Instituto de Astrofísica de Andalucía, Spain), and AZZARO (Isaac Newton Group of Telescopes, Spain) have conducted an observational program comprising H-alpha imaging for both the parent and the satellite galaxies, taken from the compilation by Zaritsky et al. (1997) that contains 115 galaxies orbiting 69 primary isolated spiral galaxies. They have observed a sub-sample of 37 spiral and irregular galaxies taken from this compilation. The aim of this study is to determine star formation properties of the sample galaxies. The observations were carried out with the VATT. Preliminary results indicate that interacting satellite galaxies exhibit a higher level of star formation than satellites with no signs of interaction. This work extends to satellite galaxies the idea, established previously for luminous galaxies, that interactions trigger star formation.
In their project on the kinematics and dynamics of disk galaxies, BERTOLA, CORSINI, PIZZELLA (University of Padua), and FUNES continue to obtain spectroscopic data that will allow an accurate investigation of the dark matter distribution within the optical regions of low surface brightness galaxies. OMIZZOLO, in collaboration with CRISTIANI (Astronomical Observatory of Trieste) and GRAZIAN (Rome Astronomical Observatory at Monte Porzio), has completed the low red shift quasar survey needed to determine the quasar luminosity function. The results of this extensive survey were presented in a poster at the General Assembly of the International Astronomical Union in July in Sydney, Australia (see International Meetings, section III. Observatory and Staff Activities), and they have been submitted for publication in the Astronomical Journal. Plans are being made to enlarge the survey with observations at telescopes in the 4-6 meter range to study quasar clustering. In collaboration with BARBIERI (Department of Astronomy, University of Padua), OMIZZOLO is researching the light curves of quasars from data obtained by scans of the photographic plates in the Vatican Observatory’s archives at Castel Gandolfo (see section II. Instrumentation and Technical Services). The first results were presented at the Sydney meeting of the International Astronomical Union in July and at astronomy meetings in Italy. From scans made at the Asiago Observatory, an historical light curve of the quasar 3C 345 has been obtained, and a report was presented at the meeting on active galactic nuclei at Cozumel, Mexico in December. The Galaxy and Galactic Objects The Nearby Stars (NStars) project, to obtain spectra, spectral types, and
basic parameters of the 3600 stars within 40 parsec of the Sun and earlier than M0 spectral
type, continued to make good progress this year. The observational program is now 98% complete,
and the principal collaborators with CORBALLY are GRAY, MCFADDEN (Appalachian State University,
Boone, North Carolina), GARRISON (David Dunlap Observatory, University of Toronto), and
O'DONOGHUE (St. Lawrence University, Canton, New York). They have now turned their full
attention to the analysis of these data. They are using the spectra to provide new, precise
spectral types and basic physical parameters (Teff, log g, [M/H]). In addition they are
In the continuing investigation with STRAIZYS and collaborators (Vilnius, Lithuania) of heavily reddened stars in clusters and of peculiar stars, CORBALLY and O'DONOGHUE have included the Aquila Rift dark clouds in a spectroscopic observing program that complements initial Vilnius 7-color photometry and classification. They also finished observing with the Steward Observatory 2.3-m telescope some 20 stars in the Aries dark cloud. The spectroscopy is being used to determine precise spectral classes, luminosities, and any peculiarities, so that a distance and extinction study can be completed. It is thus hoped to understand better the star forming regions within the Gould Belt. RUEGER (Diocese of Brooklyn), with the help of CORBALLY, continues to process UBVRI observations obtained with the VATT of two fields in the North Galactic Pole. BOYLE, with STRAIZYS, KAZLAUSKAS, SPERAUSKAS, LAUGALYS, CERNIS (Vilnius University, Lithuania) and PHILIP (Union College, Schenectady, New York), has been pursuing an observational program to calibrate the Strömvil Photometric System by observations of 1000 stars at the Steward Observatory 1.5-meter telescope on Mt. Lemmon. The Chretien Grant awarded to STRAIZYS provides travel support to the Lithuanian astronomers. The portable photometer built at Vilnius achieves very precise magnitude measurements in the seven filter system. To date they have made three observing runs over the years 2000 to 2003, each run of about a three month duration. The calibration involves observing stars having already known astrophysical quantities, e.g., temperature, luminosity, and atmospheric metallacities. The calibration consists in the correspondence of these quantities with the color indices derived from the new photometry. The work is almost completed for the stars of solar metallicity, but further observations are planned for other stars. BOYLE and PHILIP have been observing galactic and globular star clusters in this same Strömvil System with the CCD camera at the VATT. Photometric calibration of these observations will follow from using standard stars observed photoelectrically in the previously mentioned program. They are paying close attention to the precise calibration required from flat fielding the CCD observations. JANUSZ (University School Ignatianum, Kraców, Poland) has developed a “CommandLog” software product to automate with precision the processing of the CCD data. They are now obtaining quality one percent photometry needed for classifying the stars observed. SPERAUSKAS with BOYLE and UPGREN (Yale and Wesleyan Universities) is carrying out other observational work also related to stellar statistics in our Galaxy. With his Coravel type spectrometer, he is measuring the radial velocities of several hundred stars. This requires many nights at the following University of Arizona telescopes: 1.5-meter on Mt. Lemmon, 1.54-meter on Mt. Bigelow, and 2.3-meter Bok Telescope on Kitt Peak. The team seeks to obtain radial velocities for a full dynamical picture of more than one thousand nearby stars of which some two-thirds have been observed. After many nights of observing at the VATT from 1995 to 1999 by CROTTS, TOMANEY, UGLESICH (Columbia University, New York) and BOYLE, the program devised by CROTTS in search of MACHOS (Massive Compact Halo Objects) in the neighboring galaxy M31 is now producing results. The search for these mysterious massive objects is now strongly suggesting that a significant fraction of the dark matter halo of M31 is composed of roughly stellar-mass objects. Planetary Sciences Lunar Science · Magma Ocean Modeling: The most commonly
accepted proposal for the origin of the Moon posits a Mars-sized planetesimal (often called “Theia”)
impacting the Earth. According to the most recent simulations, the bulk majority of the material
that went into forming the Moon from this impact would have been derived from the surface of the
impactor, Theia, and not from the Earth. For this material to be depleted in iron and siderophiles,
Theia itself must have already been differentiated into a core and mantle.
In a paper at the 2003 Lunar and Planetary Science Conference, CONSOLMAGNO
argued this model implies that the Moon’s starting material must have been already chemically
processed at least once before being remelted during lunar accretion. And if the Moon’s material
represents only the upper portions of the impactor, then it is presumably enriched in elements
likely found in the crust, and depleted in mantle material, compared to cosmic abundances. If so,
its lithophile incompatibles could be enriched by as much as a factor of 10 compared to chondrites.
Such a lunar composition may also be more compatible with the seismic velocities than more
traditional models are. The composition of a primordial magma varies with the size of the source planet,
the amount of iron or sodium present, and other factors. Eucrites (presumably derived from the
small asteroid Vesta) are roughly 40% plagioclase, while the proportion of plagioclase in the
lunar Fra Mauro basalts can range up to 65%, implying that they have seen a wider range of source
region initial pressures or compositions. If this trend holds for the Mars-sized impactor Theia,
its initial crustal material (and hence the initial lunar composition) should have been even
richer in plagioclase. Lunar primordial magmas, formed by remelting this crustal material from Theia
under different lunar conditions, should produce basalts whose composition would exhaust pyroxene
before plagioclase. Thus further melting would result in the production of anorthosites (instead
of the orthopyroxenites seen in the Martian and Vesta meteorites). This mechanism provides a more
geophysically reasonable way to make anorthosites than the problematic “floating anorthosite crust”
first proposed for the Moon thirty years ago. Further developments of this model hold promise to explain anomalies in both
the Apollo-era lunar seismic data, and the compositions of outcrops in the South Pole-Aiken
basin measured by the Lunar Prospector and Clementine missions. · Lunar Meteorite Trace Elements: As
mentioned above, one of the spurs to re-evaluating origin models for the Moon is recognition
that certain meteorites in our collections are lunar samples delivered to Earth by impacts on
the surface of the Moon. Unlike Apollo samples, we do not know exactly where on the lunar
surface these lunar meteorites came from, but almost certainly they sample more areas than
the narrow region of flat, equatorial, near-side plains that Apollo and Luna landers visited. Several such lunar meteorites, first discovered in the Sahara desert, have
been donated to the Vatican Observatory collection in recent years. These include samples of
Dar al Gani 400, Northwest Africa 482, and Dhofar 081. All three are chemically similar to
highland anorthosites (rocks dominated by calcium-rich plagioclase, called anorthite). From
the Apollo samples, we know that such rocks are are among the oldest on the Moon. But since
being formed, these meteorites have all been severely reworked by extensive shocks, presumably
due to impacts including (but not limited to) the cratering event that launched the samples
off the Moon’s surface. Because of these shocks, at present the rocks consist of a very dark
fine-grained matrix surrounding small white glassy or microcrystalline veins and clasts. In the past year RUSSELL and JEFFRIES (Natural History Museum, London)
have done extensive measurements of major and trace element abundances of fragments from
these samples. In collaboration with them, CONSOLMAGNO has used these data to calculate
the bulk mineralogy that the clasts and matrix had before the mineral structure was
destroyed by shock. From knowing how the trace elements, especially the Rare Earth Elements
(REE), partition themselves between any given mineral and the magma from which the mineral
is crystallizing, it is then possible to calculate the likely composition of the melt from
which these rocks first formed. One significant finding is that small relict grains of pure anorthite
in the clasts have REE patterns that would be in equilibrium with a primordial melt whose
REE abundances are unfractionated but uniformly enriched to 10 times chondritic values.
Such a composition is a good candidate for a primordial lunar melt. The REE patterns of
the other clasts lie between the anorthite grains and this model liquid, and may represent
a mixture of the anorthite and the melt. Meteorite Physical Properties As described in last year’s Annual Report, CONSOLMAGNO along with WEIDENSCHILLING
(Planetary Science Institute, Tucson) and BRITT (University of Central Florida, Orlando)
are examining the way in which dust in the solar nebula became lithified into dense,
essentially unporous meteorite rocks. A key ingredient in the mix of necessary physical
processes appears to be the shock produced by impacts in the early nebula, strong enough
to lithify the dust but not so strong as to totally disrupt the sample. One difficulty is
that the rapid compression of highly underdense material by even low degrees of shock will
lead to temperatures elevated high above those experienced by the meteorites themselves.
Thus a multi-stage scenario of initially slow compression by weaker impacts may be necessary.
This theoretical modeling continues. In attempting to learn how meteorites are initially lithified, how their
fabric evolves with time, and how their transport from the asteroid belt to the Earth’s
surface biases our understanding of meteorite structure, STRAIT (Alma College, Alma,
Michigan) and CONSOLMAGNO have used meteorite porosity to constrain the internal structure
of asteroid parent bodies. To do this, they use a computerized point-counting system to
measure void spaces visible in Scattering Electron Microscope images of ordinary chondrite
meteorite thin sections and then compare these data with reported hand-sample porosity
measurements. Although questions about microcrack porosity in meteorite samples have
been resolved (as described in previous Annual Reports), other questions have arisen as a
consequence of these porosity measurements. Are shock-induced microcracks emplaced during
the event that ejects the meteorite from the parent body, or during the impact of the
meteorite with the Earth (either with its atmosphere, or on hitting the ground)? How does
the porosity in meteorites on Earth compare with that of the material while it is still
in its parent body? One way to address these questions is to measure the microcrack porosity of
terrestrial basalt. This is material similar in nature to meteoritic material, but it has not
experienced ejection from a parent body, transportation through space, atmospheric entry, and
impact on the surface of the Earth. When measurements of the microcrack porosity of terrestrial
basalts are compared to those of meteoritic basalts, the data show similar porosities. This
supports the idea that porosity measured for meteorites on Earth is a good indication of their
porosity while still on their asteroidal parent bodies. Another way to address these questions would be to study samples collected
in situ from a body where we also have samples that have experienced ejection, transport,
entry, and impact onto Earth. Samples that would fit this category unequivocally are Apollo
moon rocks and lunar meteorites. Preliminary work is encouraging, but this question will
need to be more extensively studied with a broader range of samples. Meteorite Physical Properties · Asteroid Satellites and the Pluto-Charon System:
The astrometric method to detect asteroid satellites is based on the search for the reflex effect
on the primary object due to the orbital motion of a possible satellite. As reported previously
by KIKWAYA, working with THUILLOT and BERTHIER (Paris Observatory), the astrometric signature of
a satellite of 146 Lucina may reach several milliarcseconds, indicating it may have a satellite.
Spectral analysis of the observed positions of this asteroid compared against its computed orbit
might then detect the signal with a good signal/noise ratio, given high quality astrometric
measurements and extensive coverage by different observation sites. However, the astrometric method cannot be applied to all binary systems of
asteroids. Its applicability depends strongly on the mass ratio of the two bodies and on the
distance between them. The Pluto-Charon system provides a good test of this method. Previous
work based on direct imaging of Charon show that its period is 6.357 days and the mass ratio
is 0.122, putting this system in the range that can be observed by the astrometric method. Using archived photographic observations (1914-1995) and CCD observations
from U.S. Naval Observatory, Flagstaff Station (1995-1998), Bordeaux Observatory (1996-1997),
and McDonald Observatory (1997), the position of Pluto is being analyzed to see if its wobble
effect due to Charon (which should provide an amplitude of around 95 milliarcseconds) can be
detected and if the orbital period of Charon can be recovered through spectral analysis of
Pluto’s observed position compared to its computed orbit. If successful, this detection would
confirm the ability of the astrometric method to find asteroid satellites. In addition, KIKWAYA is collaborating with MERLINE (Southwest Research
Institute, Boulder) to predict possible mutual events (such as eclipses and occultations) of
known binary asteroids. These predictions can then be used to suggest possible observations
of the light curves of these asteroids, to provide a more precise set of orbital elements
for the satellites, and ultimately to obtain a better measure of their masses and densities. · Kuiper Belt Objects: TEGLER
(Northern Arizona University, Flagstaff), ROMANISHIN (University of Oklahoma, Norman),
and CONSOLMAGNO continued their BVR photometric survey of Kuiper Belt Objects (KBOs) at
the VATT, along with observations at the Keck I 10-m telescope on Mauna Kea, Hawaii, and
the University of Arizona 2.3-m Bok Telescope on Kitt Peak. These objects, irregular lumps
of ice and rock orbiting at or beyond the orbits of Neptune and Pluto, appear to represent
some of the most primordial material in our Solar System and may be the source of at least
one class of comets. In examining the data to date, certain dynamical classes of KBOs are now
seen to exhibit very distinctive surface colors. Seventeen of 20 objects on large-inclination
and large-eccentricity orbits with aphelion distances larger than 70 AU (a dynamically hot
population) exhibit gray, B-R < 1.5, surface colors. In contrast, 21 of 21 classical KBOs
on small-inclination and small-eccentricity orbits with perihelion distances larger than
40 AU (a dynamically cold population) exhibit red surface colors, B-R > 1.5. In addition,
22 Centaurs observed to date divide into two very different color populations, gray and
red. In all cases, the odds that these trends are merely random fluctuations of a uniform
color distribution (as seen by applying the Dip Test and Student’s T Test) are less than
one part in several thousand. These observations are consistent with a primordial origin of KBO
surface colors based on their original heliocentric distance. During their formation,
objects that formed closer to the Sun, at warmer temperatures, may have incorporated
methane in the form of methane clathrate, a mixture of roughly seven parts water to
one part methane. Loss of methane from such a surface by sublimation or UV photolysis
would result in a gray water ice “lag” deposit. By contrast, in the colder outer reaches
of the solar nebula, methane could condense directly as an ice on the KBO surfaces,
where it could be turned into more complex hydrocarbons (typically red) by the action
of ultraviolet and cosmic irradiation. The gray objects that formed closer to the Sun would be orbiting in
regions subject to orbital perturbations by an outward migrating Neptune; this would
result in dynamically “hot” orbits. Red objects formed farther from the Sun would be
only partly perturbed by Neptune (contributing to the Centaur population). The
farthest objects (red surfaces, cooler orbits) would remain unperturbed. The reddest of these objects have a color previously only seen on few
inner solar system objects, most notably the asteroid (or perhaps extinct comet nucleus)
5145 Pholus. However, recent observations have suggested that the extreme red color seen
on Pholus 10 years ago may be changing; if so, this might represent outgasing of material
from its interior. VATT observations of Pholus by TEGLER and CONSOLMAGNO are being
analyzed to see if this change can be confirmed. | ||||
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History and Philosophy of Science; Interdisciplinary Studies CARUANA continues to engage in research in three main areas. The more long-term project involves the study of how the scientific mentality may affect the ethical dimension of human beings; the results will eventually be published as a book entitled Science and Virtue. The second project involves research on the impact of Albert Einstein’s special theory of relativity on some central issues in philosophy of religion. The resulting paper will be published in the 2005 special issue of the journal Revista Portuguesa de Filosofia to commemorate the centenary of Einstein’s 1905 paper on special relativity. The third project involves the preparation of 10 hours of advanced lectures on philosophy and cognitive science scheduled for 2004 within the Science and Philosophy specialization currently being offered at the Pontifical Gregorian University. CASANOVAS continues his research in the history of astronomy, especially on the Gregorian reform of the calendar and on spherical astronomy. In preparation for an International Forum on Science, Religion, and Consciousness, CORBALLY reflected on the effect that an encounter with extraterrestrials of superior intellect might have on organized religions. He considered how an understanding of the physical cosmos, presumably shared by terrestrials and by extraterrestrials, leads to insights into the nature of the Creator. Hence he concluded that humanity's fundamental ideas of God would not change in such an encounter. Hopefully, though, there might result some continued purification of religion from “error and superstition,” a task for science suggested in a Message of Pope John Paul II (Physics, Philosophy, and Theology: A Common Quest for Understanding, ed. R.J. Russell, W.R. Stoeger, S.J., and G.V. Coyne, S.J. Vatican: Vatican Observatory Publications 1997, 3rd Edition, pg. M13). COYNE served as a consultant to the John Templeton Foundation on the evaluation of the proposal for the “Science, Theology, and the Ontological Quest” program of three Pontifical Universities in Rome: Gregoriana, Lateranense and Regina Apostolorum. He continues to serve on the Advisory Council for that program. OMIZZOLO in collaboration with BERTOLA (Department of Astronomy, University of Padua) has organized a second series of seminars on interdisciplinary themes in science, philosophy, and theology. He has also been actively involved in these themes at the University of Brescia and in Venice. STOEGER has extended his research on divine action, theology of creation, the science and philosophy of causality, and on reducibility and emergence. |
providing measures of the chromospheric activity of these stars. Recent results of this program
include the basic physical parameters of stars with exoplanets. They conclude that stars with
planets have a mean metallicity that is similar to that of the Sun. However, this mean is
significantly higher than the metallicity for the general run of solar neighborhood,
solar-type stars (see graph). They have also discovered stars with high levels of chromospheric
activity; are making a refinement of the stellar census within 40 parsec of the Sun; and are
finding the possible presence of a significant population of “Maunder Minimum” dwarfs in the
solar neighborhood. Observed and derived data from this project are being released on the
project's website http://stellar.phys.appstate.edu. 
The reddest KBOs have a color similar to that of the asteroid 5145 Pholus. By coincidence, during
observations at the VATT, the asteroid passed near the galaxy NGC 5964, and Consolmagno and Tegler
took its picture (boxed area). Pholus moved between exposures and appears as a streak of light.
