2,881 research outputs found
Algebraic and combinatorial aspects of sandpile monoids on directed graphs
The sandpile group of a graph is a well-studied object that combines ideas
from algebraic graph theory, group theory, dynamical systems, and statistical
physics. A graph's sandpile group is part of a larger algebraic structure on
the graph, known as its sandpile monoid. Most of the work on sandpiles so far
has focused on the sandpile group rather than the sandpile monoid of a graph,
and has also assumed the underlying graph to be undirected. A notable exception
is the recent work of Babai and Toumpakari, which builds up the theory of
sandpile monoids on directed graphs from scratch and provides many connections
between the combinatorics of a graph and the algebraic aspects of its sandpile
monoid.
In this paper we primarily consider sandpile monoids on directed graphs, and
we extend the existing theory in four main ways. First, we give a combinatorial
classification of the maximal subgroups of a sandpile monoid on a directed
graph in terms of the sandpile groups of certain easily-identifiable subgraphs.
Second, we point out certain sandpile results for undirected graphs that are
really results for sandpile monoids on directed graphs that contain exactly two
idempotents. Third, we give a new algebraic constraint that sandpile monoids
must satisfy and exhibit two infinite families of monoids that cannot be
realized as sandpile monoids on any graph. Finally, we give an explicit
combinatorial description of the sandpile group identity for every graph in a
family of directed graphs which generalizes the family of (undirected)
distance-regular graphs. This family includes many other graphs of interest,
including iterated wheels, regular trees, and regular tournaments.Comment: v2: Cleaner presentation, new results in final section. Accepted for
publication in J. Combin. Theory Ser. A. 21 pages, 5 figure
A Comparative Analysis of Post-Traumatic Stress Syndrome among Individuals Exposed to Different Stressor Events
The purpose of the present study was to compare post-traumatic stress syndrome among persons involved in nine different stressor events: combat in the Vietnam War; rape; serious life-threatening events; divorce; the death of a significant other; critical, near fatal illness of a significant other; family trauma; multiple traumatic events; and no stressful event. To assess the severity of the symptoms which define post-traumatic stress disorder (PTSD), the Impact of Event Scale, the Beck Depression Inventory, the Stress Assessment Scale for PTSD from the Vietnam Era Stress Inventory (Wilson & Krauss, 1980) and the Sensation Seeking Scale were administered to the participants (N=409). A person by situation conceptual model of PTSD was presented from which two major hypotheses were tested. As predicted from the model, the degree of loss of a significant other and life-threat were predictive of syndromespecific symptoms of PTSD. The results of the study strongly support the heuristic value of an interactionist model of PTSD
A computer controlled power tool for the servicing of the Hubble Space Telescope
The Hubble Space Telescope (HST) Pistol Grip Tool (PGT) is a self-contained, microprocessor controlled, battery-powered, 3/8-inch-drive hand-held tool. The PGT is also a non-powered ratchet wrench. This tool will be used by astronauts during Extravehicular Activity (EVA) to apply torque to the HST and HST Servicing Support Equipment mechanical interfaces and fasteners. Numerous torque, speed, and turn or angle limits are programmed into the PGT for use during various missions. Batteries are replaceable during ground operations, Intravehicular Activities, and EVA's
High-sensitivity cardiac troponin concentrations at presentation in patients with ST-segment elevation myocardial infarction
No abstract available
A First Catalog of Variable Stars Measured by the Asteroid Terrestrial-impact Last Alert System (ATLAS)
The Asteroid Terrestrial-impact Last Alert System (ATLAS) carries out its
primary planetary defense mission by surveying about 13000 deg^2 at least four
times per night. The resulting data set is useful for the discovery of variable
stars to a magnitude limit fainter than r~18, with amplitudes down to 0.01 mag
for bright objects. Here we present a Data Release One catalog of variable
stars based on analyzing 142 million stars measured at least 100 times in the
first two years of ATLAS operations. Using a Lomb-Scargle periodogram and other
variability metrics, we identify 4.7 million candidate variables which we
analyze in detail. Through Space Telescope Science Institute, we publicly
release lightcurves for all of them, together with a vector of 169
classification features for each star. We do this at the level of unconfirmed
candidate variables in order to provide the community with a large set of
homogeneously analyzed photometry and avoid pre-judging which types of objects
others may find most interesting. We use machine learning to classify the
candidates into fifteen different broad categories based on lightcurve
morphology. About 10% (430,000 stars) pass extensive tests designed to screen
out spurious variability detections: we label these as `probable' variables. Of
these, 230,000 receive specific classifications as eclipsing binaries,
pulsating, Mira-type, or sinusoidal variables: these are the `classified'
variables. New discoveries among the probable variables number more than
300,000, while 150,000 of the classified variables are new, including about
10,000 pulsating variables, 2,000 Mira stars, and 70,000 eclipsing binaries.Comment: Accepted by AJ; gives instructions for querying ATLAS variable star
database; this new version has nicer lightcurve figure
Constraints on the Progenitor of SN 2016gkg From Its Shock-Cooling Light Curve
SN 2016gkg is a nearby Type IIb supernova discovered shortly after explosion.
Like several other Type IIb events with early-time data, SN 2016gkg displays a
double-peaked light curve, with the first peak associated with the cooling of a
low-mass extended progenitor envelope. We present unprecedented
intranight-cadence multi-band photometric coverage of the first light-curve
peak of SN 2016gkg obtained from the Las Cumbres Observatory Global Telescope
network, the Asteroid Terrestrial-impact Last Alert System, the Swift satellite
and various amateur-operated telescopes. Fitting these data to analytical
shock-cooling models gives a progenitor radius of ~25-140 solar radii with
~2-30 x 10^-2 solar masses of material in the extended envelope (depending on
the model and the assumed host-galaxy extinction). Our radius estimates are
broadly consistent with values derived independently (in other works) from HST
imaging of the progenitor star. However, the shock-cooling model radii are on
the lower end of the values indicated by pre-explosion imaging. Hydrodynamical
simulations could refine the progenitor parameters deduced from the
shock-cooling emission and test the analytical models.Comment: Accepted by ApJ
The Baryonic Tully Fisher Relation
We validate the baryonic Tully Fisher (BTF) relation by exploring the Tully
Fish er (TF) and BTF properties of optically and HI-selected disk galaxies. The
data includes galaxies from: Sakai et al. (2000) calibrator sample; McGaugh et
al. (2000: MC2000) I-band sample; and 18 newly acquired HI-selected field dwarf
galaxies observed with the ANU 2.3m telescope and the ATNF Parkes telescope
from Gurovich's thesis sample (2005).
As in MC2000, we re-cast the TF and BTF relations as relationships between
baryo n mass and W_{20}. First we report some numerical errors in MC2000. Then,
we c alculate weighted bi-variate linear fits to the data, and finally we
compare the fits of the intrinsically fainter dwarfs with the brighter galaxies
of Sakai et al. (2000). With regards to the local calibrator disk galaxies of
Sakai et al. (2000), our results suggest that the BTF relation is indeed
tighter than the T F relation and that the slopes of the BTF relations are
statistically flatter th an the equivalent TF relations. Further, for the
fainter galaxies which include the I-band MCG2000 and HI-selected galaxies of
Gurovich's thesis sample, we calc ulate a break from a simple power law model
because of what appears to be real c osmic scatter. Not withstanding this
point, the BTF models are marginally better models than the equivalent TF ones
with slightly smaller reduced chi^2.Comment: 3 pages, 3 figs, refereed conference proceeding based on an invited
talk at the Structure and Dynamics in the Local Universe, a Sydney workshop
to honour Brent Tully's 60th birthday. To appear in Publications of the
Astronomical Society of Australia, ed. J. Bland-Hawthor
Measuring nickel masses in Type Ia supernovae using cobalt emission in nebular phase spectra
The light curves of Type Ia supernovae (SNe Ia) are powered by the
radioactive decay of Ni to Co at early times, and the decay of
Co to Fe from ~60 days after explosion. We examine the evolution
of the [Co III] 5892 A emission complex during the nebular phase for SNe Ia
with multiple nebular spectra and show that the line flux follows the square of
the mass of Co as a function of time. This result indicates both
efficient local energy deposition from positrons produced in Co decay,
and long-term stability of the ionization state of the nebula. We compile 77
nebular spectra of 25 SN Ia from the literature and present 17 new nebular
spectra of 7 SNe Ia, including SN2014J. From these we measure the flux in the
[Co III] 5892 A line and remove its well-behaved time dependence to infer the
initial mass of Ni () produced in the explosion. We then examine
Ni yields for different SN Ia ejected masses ( - calculated
using the relation between light curve width and ejected mass) and find the
Ni masses of SNe Ia fall into two regimes: for narrow light curves (low
stretch s~0.7-0.9), is clustered near ~ 0.4 and
shows a shallow increase as increases from ~1-1.4; at high
stretch, clusters at the Chandrasekhar mass (1.4) while
spans a broad range from 0.6-1.2. This could constitute
evidence for two distinct SN Ia explosion mechanisms.Comment: 16 pages, 12 figures (main text), plus data tables in appendix.
Spectra released on WISeREP. Submitted to MNRAS, comments welcom
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