332 research outputs found
Massive stars and the energy balance of the interstellar medium. II. The 35 solar mass star and a solution to the "missing wind problem"
We continue our numerical analysis of the morphological and energetic
influence of massive stars on their ambient interstellar medium for a 35 solar
mass star that evolves from the main sequence through red supergiant and
Wolf-Rayet phases, until it ultimately explodes as a supernova. We find that
structure formation in the circumstellar gas during the early main-sequence
evolution occurs as in the 60 solar mass case but is much less pronounced
because of the lower mechanical wind luminosity of the star. Since on the other
hand the shell-like structure of the HII region is largely preserved, effects
that rely on this symmetry become more important. At the end of the stellar
lifetime 1% of the energy released as Lyman continuum radiation and stellar
wind has been transferred to the circumstellar gas. From this fraction 10% is
kinetic energy of bulk motion, 36% is thermal energy, and the remaining 54% is
ionization energy of hydrogen. The sweeping up of the slow red supergiant wind
by the fast Wolf-Rayet wind produces remarkable morphological structures and
emission signatures, which are compared with existing observations of the
Wolf-Rayet bubble S308. Our model reproduces the correct order of magnitude of
observed X-ray luminosity, the temperature of the emitting plasma as well as
the limb brightening of the intensity profile. This is remarkable, because
current analytical and numerical models of Wolf-Rayet bubbles fail to
consistently explain these features. A key result is that almost the entire
X-ray emission in this stage comes from the shell of red supergiant wind swept
up by the shocked Wolf-Rayet wind rather than from the shocked Wolf-Rayet wind
itself as hitherto assumed and modeled. This offers a possible solution to what
is called the ``missing wind problem'' of Wolf-Rayet bubbles.Comment: 52 pages, 20 figures, 2 tables, accepted for publication in the
Astrophysical Journa
BCS pairing in a trapped dipolar Fermi gase
We present a detailed study of the BCS pairing transition in a trapped
polarized dipolar Fermi gas. In the case of a shallow nearly spherical trap, we
find the decrease of the transition temperature as a function of the trap
aspect ratio and predict the existence of the optimal trap geometry. The latter
corresponds to the highest critical temperature of the BCS transition for a
given number of particles. We also derive the phase diagram for an ultracold
trapped dipolar Fermi gases in the situation, where the trap frequencies can be
of the order of the critical temperature of the BCS transition in the
homogeneous case, and find the critical value of the dipole-dipole interaction
energy, below which the BCS transition ceases to exist. The critical dipole
strength is obtained as a function of the trap aspect ratio. Alternatively, for
a given dipole strength there is a critical value of the trap anisotropy for
the BCS state to appear. The order parameter calculated at criticality,
exhibits nover non-monotonic behavior resulted from the combined effect of the
confining potential and anisotropic character of the interparticle
dipole-dipole interation.Comment: 14 pages, 3 figure
Burbot Early Life History Strategies in the Great Lakes
Burbot Lota lota exhibit four previously known reproductive strategies in the Great Lakes region. In this paper we review those strategies and provide evidence for a fifth oneâdelayed deepwater spawning. The four known, shallowâwater strategies are as follows: (1) spawning by selfâsustaining, landlocked populations, (2) spawning in tributaries in winter and the exit of larvae to a Great Lake, (3) spawning by residents in a spawning stream with access to a Great Lake, and (4) spawning on unconsolidated and rocky areas in shallow water in winter in the lake proper. Resident, landlocked populations exist in some Michigan and Wisconsin rivers (e.g., the Muskegon River in Michigan). The evidence for winter tributary spawning is the appearance of newly hatched Burbot in the St. Marys and Bark rivers during AprilâJune. Evidence for Burbot juveniles leaving spawning streams is U.S. Fish and Wildlife Service tributory mouth trap data. The evidence for winter nearshore spawning comes from power plant monthly entrainment studies (Mansfield et al. 1983). Our proposed fifth strategy is spring and summer spawning at deep reefs, where there is probably cobble or boulder habitat. Our evidence comes from midlake reefs in Lake Michigan and offshore areas of Lake Huron: (1) we collected adult Burbot at midlake reefs in Lake Michigan, (2) we collected many Burbot larvae (many of which were newly hatched) from Lakes Michigan and Huron in JuneâAugust, and (3) we collected a Burbot egg in a PONAR grab in midâJuly from 73 m in southern Lake Huron. An important question remains, namely, which life history strategy provides the highest recruitment success for this species. It may be that adaptability ensures the survival of this important, topâpredator fish during periods of crisis (e.g., encounters with dams, Sea Lamprey Petromyzon marinus predation).Peer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/141895/1/tafs1733.pd
Halpha Morphologies and Environmental Effects in Virgo Cluster Spiral Galaxies
We describe the various Halpha morphologies of Virgo Cluster and isolated
spiral galaxies, and associate the Halpha morphologies with the types of
environmental interactions which have altered the cluster galaxies. The spatial
distributions of Halpha and R-band emission are used to divide the star
formation morphologies of the 52 Virgo Cluster spirals into several categories:
normal (37%), anemic (6%), enhanced (6%), and (spatially) truncated (52%).
Truncated galaxies are further subdivided based on their inner star formation
rates into truncated/normal (37%), truncated/compact (6%), truncated/anemic
(8%), and truncated/enhanced (2%). The fraction of anemic galaxies is
relatively small (6-13%) in both environments, suggesting that starvation is
not a major factor in the reduced star formation rates of Virgo spirals. The
majority of Virgo spiral galaxies have their Halpha disks truncated (52%),
whereas truncated Halpha disks are rarer in isolated galaxies (12%). Most of
the Halpha-truncated galaxies have relatively undisturbed stellar disks and
normal-to-slightly enhanced inner disk star formation rates, suggesting that
ICM-ISM stripping is the main mechanism causing the reduced star formation
rates of Virgo spirals. In other galaxies, the Halpha morphologies are more
consistent with a tidal origin or perhaps outer cluster HI accretion. These
results indicate that most Virgo spiral galaxies experience ICM-ISM stripping,
many experience significant tidal effects, and many experience both.
(abridged).Comment: Accepted by Astrophysical Journal. 16 pages, 15 figures, including 9
in low-resolution jpg format. Higher resolution postscript versions of these
figures are available from http://www1.union.edu/~koopmanr/radfig.htm
The Recent Evolution of the Dwarf Starburst Galaxy NGC 625 from Hubble Space Telescope Imaging
New HST/WFPC2 imaging of the dwarf starburst galaxy NGC 625 is presented.
These data, 80% complete to V and I magnitudes of 26.0 and 25.3, respectively,
allow us to study the recent star formation history of NGC 625. We derive a tip
of the red giant branch (TRGB) distance modulus of 27.95+/-0.07, corresponding
to a distance of 3.89+/-0.22 Mpc, and a location on the far side of the
Sculptor Group. NGC 625 has a well-defined radial stellar population gradient,
evidenced by a central concentration of young MS stars and an RGB/AGB ratio
that increases with galactocentric distance. The prominent AGB is very red, and
RGB stars are detected far from the central star forming regions. Using H Alpha
and H Beta narrow band imaging and previous optical spectroscopy we identify
substantial and varying internal extinction (A_V = 0.0 to 0.6 mag) associated
with the central active star formation regions. To better understand the
effects of internal extinction on the analysis of young stellar populations,
synthetic models are presented which, for the first time, examine and account
for this effect. Using the luminous blue helium burning stars, we construct a
simple model of the recent (< 100 Myr) star formation in which an elevated but
declining star formation rate has been present over this entire period. This is
at odds with the presence of spectroscopic W-R features in the major star
formation region which imply a short duration (<= 5 Myr) for the recent
starburst. This suggests that starbursts displaying W-R features are not
necessarily all of a short duration. Finally, we speculate on the possible
causes of the present burst of star formation in this apparently isolated
galaxy, and compare it to other nearby, well-studied dwarf starburst systems.Comment: 56 pages, including 15 figures (2 in color). Scheduled to appear in
AJ, December, 2003. Full-resolution version may be obtained at
http://www.astro.umn.edu/~Cannon/n625.p
The physics of dipolar bosonic quantum gases
This article reviews the recent theoretical and experimental advances in the
study of ultracold gases made of bosonic particles interacting via the
long-range, anisotropic dipole-dipole interaction, in addition to the
short-range and isotropic contact interaction usually at work in ultracold
gases. The specific properties emerging from the dipolar interaction are
emphasized, from the mean-field regime valid for dilute Bose-Einstein
condensates, to the strongly correlated regimes reached for dipolar bosons in
optical lattices.Comment: Review article, 71 pages, 35 figures, 350 references. Submitted to
Reports on Progress in Physic
Judge Jack B. Weinstein, Tort Litigation, and the Public Good: A Roundtable Discussion to Honor One of America\u27s Great Trial Judges on the Occasion of his 80th Birthday
Local-Group tests of dark-matter Concordance Cosmology: Towards a new paradigm for structure formation
(abridged) Predictions of the Concordance Cosmological Model (CCM) of the
structures in the environment of large spiral galaxies are compared with
observed properties of Local Group galaxies. Five new most probably
irreconcilable problems are uncovered. However, the Local Group properties
provide hints that may lead to a solution of the above problems The DoS and
bulge--satellite correlation suggest that dissipational events forming bulges
are related to the processes forming phase-space correlated satellite
populations. Such events are well known to occur since in galaxy encounters
energy and angular momentum are expelled in the form of tidal tails, which can
fragment to form populations of tidal-dwarf galaxies (TDGs) and associated star
clusters. If Local Group satellite galaxies are to be interpreted as TDGs then
the sub-structure predictions of CCM are internally in conflict. All findings
thus suggest that the CCM does not account for the Local Group observations and
that therefore existing as well as new viable alternatives have to be further
explored. These are discussed and natural solutions for the above problems
emerge.Comment: A and A, in press, 25 pages, 9 figures; new version contains minor
text adjustments for conformity with the published version and additional
minor changes resulting from reader's feedback. The speculation on a dark
force has been added. Also, the Fritz Zwicky Paradox is now included to agree
with the published versio
Fitting the integrated Spectral Energy Distributions of Galaxies
Fitting the spectral energy distributions (SEDs) of galaxies is an almost
universally used technique that has matured significantly in the last decade.
Model predictions and fitting procedures have improved significantly over this
time, attempting to keep up with the vastly increased volume and quality of
available data. We review here the field of SED fitting, describing the
modelling of ultraviolet to infrared galaxy SEDs, the creation of
multiwavelength data sets, and the methods used to fit model SEDs to observed
galaxy data sets. We touch upon the achievements and challenges in the major
ingredients of SED fitting, with a special emphasis on describing the interplay
between the quality of the available data, the quality of the available models,
and the best fitting technique to use in order to obtain a realistic
measurement as well as realistic uncertainties. We conclude that SED fitting
can be used effectively to derive a range of physical properties of galaxies,
such as redshift, stellar masses, star formation rates, dust masses, and
metallicities, with care taken not to over-interpret the available data. Yet
there still exist many issues such as estimating the age of the oldest stars in
a galaxy, finer details ofdust properties and dust-star geometry, and the
influences of poorly understood, luminous stellar types and phases. The
challenge for the coming years will be to improve both the models and the
observational data sets to resolve these uncertainties. The present review will
be made available on an interactive, moderated web page (sedfitting.org), where
the community can access and change the text. The intention is to expand the
text and keep it up to date over the coming years.Comment: 54 pages, 26 figures, Accepted for publication in Astrophysics &
Space Scienc
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