9,427 research outputs found
Mechanics of thermally fluctuating membranes
Besides having unique electronic properties, graphene is claimed to be the
strongest material in nature. In the press release of the Nobel committee it is
claimed that a hammock made of a squared meter of one-atom thick graphene could
sustain the wight of a 4 kg cat. More practically important are applications of
graphene like scaffolds and sensors which are crucially dependent on the
mechanical strength. Meter-sized graphene is even being considered for the
lightsails in the starshot project to reach the star alpha centaury. The
predicted strength of graphene is based on its very large Young modulus which
is, per atomic layer, much larger than that of steel. This reasoning however
would apply to conventional thin plates but does not take into account the
peculiar properties of graphene as a thermally fluctuating crystalline
membrane. It was shown recently both experimentally and theoretically that
thermal fluctuations lead to a dramatic reduction of the Young modulus and
increase of the bending rigidity for micron-sized graphene samples in
comparison with atomic scale values. This makes the use of the standard
F\"oppl-von Karman elasticity (FvK) theory for thin plates not directly
applicable to graphene and other single atomic layer membranes. This fact is
important because the current interpretation of experimental results is based
on the FvK theory. In particular, we show that the FvK-derived Schwerin
equation, routinely used to derive the Young modulus from indentation
experiments has to be essentially modified for graphene at room temperature and
for micron sized samples. Based on scaling analysis and atomistic simulation we
investigate the mechanics of graphene under transverse load up to breaking. We
determine the limits of applicability of the FvK theory and provide
quantitative estimates for the different regimes.Comment: to appear in npj 2D Materials and Application
Scaling behavior and strain dependence of in-plane elastic properties of graphene
We show by atomistic simulations that, in the thermodynamic limit, the
in-plane elastic moduli of graphene at finite temperature vanish with system
size as a power law with , in
agreement with the membrane theory. Our simulations clearly reveal the size and
strain dependence of graphene's elastic moduli, allowing comparison to
experimental data. Although the recently measured difference of a factor 2
between the asymptotic value of the Young modulus for tensilely strained
systems and the value from {\it ab initio} calculations remains unsolved, our
results do explain the experimentally observed increase of more than a factor 2
for a tensile strain of only a few permille. We also discuss the scaling of the
Poisson ratio, for which our simulations disagree with the predictions of the
self-consistent screening approximation.Comment: 5 figure
DASCH 100-yr light curves of high-mass X-ray binaries
We analyzed the 100-yr light curves of Galactic high-mass X-ray binaries
using the Harvard photographic plate collection, made accessible through the
DASCH project (Digital Access to a Sky Century at Harvard). As scanning is
still in progress, we focus on the four objects that are currently well
covered: the supergiant X-ray binary Cyg X-1 (V1357 Cyg), and the Be X-ray
binaries 1H 1936+541 (BD+53 2262), RX J1744.7-2713 (HD 161103), and RX
J2030.5+4751 (SAO 49725), the latter two objects being similar to gamma Cas.
The star associated with Cyg X-1 does not show evidence for variability with an
amplitude higher than 0.3 magnitude over a hundred years. We found significant
variability of one magnitude with timescales of more than 10 years for SAO
49725, as well as a possible period of 500-600 days and an amplitude of 0.05
magnitude that might be the orbital, or super-orbital period of the system. The
data is insufficient to conclude for HD 161103 but suggests a similar long-term
variability. We thus observe an additional characteristic of gamma Cas-like
objects: their long-term variability. This variability seems to be due to the
slow evolution of a decretion disk around the Be star, but may be triggered by
the presence of a compact object in the system, possibly a white dwarf. This
characteristic could be used to identify further similar objects otherwise
difficult to detect.Comment: Accepted for publication in Proceedings of Science (INTEGRAL 2012),
Eds. A. Goldwurm, F. Lebrun and C. Winkler, based on a presentation at the
9th INTEGRAL Workshop "An INTEGRAL view of the high-energy sky (the first 10
years)", October 15-19, 2012, Paris, Franc
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