19,581 research outputs found
Aging vs crystallisation dynamics in hyperquenched glasses and a resolution of the water Tg controversy
The possibility of observing a glass transition in water before
crystallisation occurs has been debated vigorously but inconclusively over five
decades [1,2]. For two decades a glass transition at 136K [2,3] was accepted
but this transition has perplexing qualities [4]. Recently it has been
argued[2,5],that this assignment must be wrong. The re-assignment of Tg to
temperatures above the 150K crystallisation was vigorously contested [6]. Here
we use detailed anneal-and-scan studies of a hyperquenched inorganic glass,
which does not crystallize on heating, to interpret the perplexing aspects of
the 136K water phenomenon. We show that it is indeed linked to a glass
transition, though only via a cross-over phenomenon. The thermal history that
gives the same behaviour ("shadow" glass transition) in the inorganic glass is
linked by crossover to a "normal" glass transition 23% higher in temperature.
Thus a Tg is indeed unobservable for water, while the vitreous nature of
hyperquenched glassy water is strongly supported. The shadow Tg is reproducible
in the inorganic glass as it is in H2O. The observed aging dynamics are very
relevant to current glass theory, particularly to dynamical heterogeneity which
is seen to have an energy manifestation.Comment: 23 pages, 4 figure
Reduced-Order Modelling of Parametric Systems via Interpolation of Heterogeneous Surrogates
Implications of Charmless B Decays with Large Direct CP Violation
Based on the most recent data in charmless B decays including the very
recently reported large direct CP violations, it is shown that the weak phase
gamma can well be extracted without two-fold ambiguity even only from two decay
modes pi^+pi^- and pi^+K^-, and its value is remarkably consistent with the
global standard model fit at a compatible accuracy. A fit to all the pi pi, pi
K data favor both large electroweak penguin and color-suppressed tree amplitude
with large strong phases. It is demonstrated that the inclusion of small
SU(3)symmetry breaking effects of strong phases and the inelastic rescattering
effects can well improve the consistency of the data, while both effects may
not be sufficient to arrive at a small electroweak penguin amplitude in the
standard model. It is of interest to notice that large or small electroweak
penguin amplitude becomes a testable prediction as they lead to significantly
different predictions for the direct CP violations for pi^0 pi^0, pi^0 K^0
modes. Clearly, precise measurements on charmless B decays will provide a
window for probing new physics.Comment: 4 pages, 1 figure, 1 table, results updated with the latest data.
conclusions unchanged. Refence added. published versio
Strategic Asset Seeking and Innovation Performance: The Role of Innovation Capabilities and Host Country Institutions
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PSR B1828-11: a precession pulsar torqued by a quark planet?
The pulsar PSR B1828-11 has long-term, highly periodic and correlated
variations in both pulse shape and the rate of slow-down. This phenomenon may
provide evidence for precession of the pulsar as suggested previously within
the framework of free precession as well as forced one. On a presumption of
forced precession, we propose a quark planet model to this precession henomenon
instead, in which the pulsar is torqued by a quark planet. We construct this
model by constraining mass of the pulsar (), mass of the planet
() and orbital radius of the planet (). Five aspects
are considered: derived relation between and ,
movement of the pulsar around the center of mass, ratio of and
, gravitational wave radiation timescale of the planetary system,
and death-line criterion. We also calculate the range of precession period
derivative and gravitational wave strength (at earth) permitted by the model.
Under reasonable parameters, the observed phenomenon can be understood by a
pulsar () with a quark planet
() orbiting it. According to the calculations
presented, the pulsar would be a quark star because of its low mass, which
might eject a lump of quark matter (to become a planet around) during its
birth.Comment: 6 pages, 3 figures, accepted by MNRAS (Letters
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