6,292 research outputs found
Magnetic field enhanced structural instability in EuTiO_{3}
EuTiO_{3} undergoes a structural phase transition from cubic to tetragonal at
T_S = 282 K which is not accompanied by any long range magnetic order. However,
it is related to the oxygen ocathedra rotation driven by a zone boundary
acoustic mode softening. Here we show that this displacive second order
structural phase transition can be shifted to higher temperatures by the
application of an external magnetic field (increased by 4 K for mu_{0}H = 9 T).
This observed field dependence is in agreement with theoretical predictions
based on a coupled spin-anharmonic-phonon interaction model.Comment: 4 pages, 4 figure
Lattice and polarizability mediated spin activity in EuTiO_3
EuTiO_3 is shown to exhibit novel strong spin-charge-lattice coupling deep in
the paramagnetic phase. Its existence is evidenced by an, until now, unknown
response of the paramagnetic susceptibility at temperatures exceeding the
structural phase transition temperature T_S = 282K. The "extra" features in the
susceptibility follow the rotational soft zone boundary mode temperature
dependence above and below T_S. The theoretical modeling consistently
reproduces this behavior and provides reasoning for the stabilization of the
soft optic mode other than quantum fluctuations.Comment: 8 pages, 4 figure
Low albedos of hot to ultra-hot Jupiters in the optical to near-infrared transition regime
The depth of a secondary eclipse contains information of both the thermally
emitted light component of a hot Jupiter and the reflected light component. If
the dayside atmosphere of the planet is assumed to be isothermal, it is
possible to disentangle both. In this work, we analyze 11 eclipse light curves
of the hot Jupiter HAT-P-32b obtained at 0.89 m in the z' band. We obtain
a null detection for the eclipse depth with state-of-the-art precision, -0.01
+- 0.10 ppt. We confirm previous studies showing that a non-inverted atmosphere
model is in disagreement to the measured emission spectrum of HAT-P-32b. We
derive an upper limit on the reflected light component, and thus, on the
planetary geometric albedo . The 97.5%-confidence upper limit is <
0.2. This is the first albedo constraint for HAT-P-32b, and the first z' band
albedo value for any exoplanet. It disfavors the influence of large-sized
silicate condensates on the planetary day side. We inferred z' band geometric
albedo limits from published eclipse measurements also for the ultra-hot
Jupiters WASP-12b, WASP-19b, WASP-103b, and WASP-121b, applying the same
method. These values consistently point to a low reflectivity in the optical to
near-infrared transition regime for hot to ultra-hot Jupiters.Comment: accepted for publication in A&
A search for double beta decays of tin isotopes with enhanced sensitivity
A search for the various double beta decay modes of 124Sn and 112Sn has been
performed on 75 kg.days of data. New half-life limits for excited states in
124Sn have been obtained including a lower limit for the decay into the first
excited 2+ state of 124Te of T_half > 0.87e20 yrs (90% CL) and into the first
excited 0+ state of T_half > 1.08e20 yrs (90% CL). Ground state and excited
state transitions of 112Sn have also been experimentally explored. A limit for
the 2 neutrino double electron capture of T_half > 1.8e19 yrs (90% CL) is
obtained. The non-observation of de-excitation gammas from the 0+ at 1888.5keV
results in a lower half-life limit on the 0 neutrino double electron capture
decay of 112Sn of T_half > 0.8e19 yrs (90% CL), despite a possible resonant
enhancement of the decay rate due to degenerated states.Comment: 6 pages, 7 figures, updated analysis and tex
Mit Grünfutter und Tageslicht strahlen Hühnereier anders
Mit dem einfachen und schnellen Untersuchungsverfahren der Biophotonenanalyse lassen sich am Ei Unterschiede feststellen, die durch Haltungssystem, Fütterung und Klimafaktoren bedingt sind
Full counting statistics of heteronuclear molecules from Feshbach-assisted photo association
We study the effects of quantum statistics on the counting statistics of
ultracold heteronuclear molecules formed by Feshbach-assisted photoassociation
[Phys. Rev. Lett. {\bf 93}, 140405 (2004)]. Exploiting the formal similarities
with sum frequency generation and using quantum optics methods we consider the
cases where the molecules are formed from atoms out of two Bose-Einstein
condensates, out of a Bose-Einstein condensate and a gas of degenerate
fermions, and out of two degenerate Fermi gases with and without superfluidity.
Bosons are treated in a single mode approximation and fermions in a degenerate
model. In these approximations we can numerically solve the master equations
describing the system's dynamics and thus we find the full counting statistics
of the molecular modes. The full quantum dynamics calculations are complemented
by mean field calculations and short time perturbative expansions. While the
molecule production rates are very similar in all three cases at this level of
approximation, differences show up in the counting statistics of the molecular
fields. The intermediate field of closed-channel molecules is for short times
second-order coherent if the molecules are formed from two Bose-Einstein
condensates or a Bose-Fermi mixture. They show counting statistics similar to a
thermal field if formed from two normal Fermi gases. The coherence properties
of molecule formation in two superfluid Fermi gases are intermediate between
the two previous cases. In all cases the final field of deeply-bound molecules
is found to be twice as noisy as that of the intermediate state. This is a
consequence of its coupling to the lossy optical cavity in our model, which
acts as an input port for quantum noise, much like the situation in an optical
beam splitter.Comment: replacement of earlier manuscript cond-mat/0508080
''Feshbach-assisted photoassociation of ultracold heteronuclear molecules''
with minor revision
The QSO evolution derived from the HBQS and other complete QSO surveys
An ESO Key programme dedicated to an Homogeneous Bright QSO Survey (HBQS) has
been completed. 327 QSOs (Mb<-23, 0.3<z<2.2) have been selected over 555 deg^2
with 15<B<18.75. For B<16.4 the QSO surface density turns out to be a factor
2.2 higher than what measured by the PG survey, corresponding to a surface
density of 0.013+/-.006 deg^{-2}. If the Edinburgh QSO Survey is included, an
overdensity of a factor 2.5 is observed, corresponding to a density of
0.016+/-0.005 deg^{-2}. In order to derive the QSO optical luminosity function
(LF) we used Monte Carlo simulations that take into account of the selection
criteria, photometric errors and QSO spectral slope distribution. The LF can be
represented with a Pure Luminosity Evolution (L(z)\propto(1+z)^k) of a two
power law both for q_0=0.5 and q_0=0.1. For q_0=0.5 k=3.26, slower than the
previous Boyle's (1992) estimations of k=3.45. A flatter slope beta=-3.72 of
the bright part of the LF is also required. The observed overdensity of bright
QSOs is concentrated at z<0.6. It results that in the range 0.3<z<0.6 the
luminosity function is flatter than observed at higher redshifts. In this
redshift range, for Mb<-25, 32 QSOs are observed instead of 19 expected from
our best-fit PLE model. This feature requires a luminosity dependent luminosity
evolution in order to satisfactorily represent the data in the whole 0.3<z<2.2
interval.Comment: Invited talk in "Wide Field Spectroscopy" (20-24 May 1996, Athens),
eds. M. Kontizas et al. 6 pages and 3 eps figures, LaTex file, uses epfs.sty
and crckapb.sty (included
Extraction of the electron mass from factor measurements on light hydrogenlike ions
The determination of the electron mass from Penning-trap measurements with
C ions and from theoretical results for the bound-electron
factor is described in detail. Some recently calculated contributions slightly
shift the extracted mass value. Prospects of a further improvement of the
electron mass are discussed both from the experimental and from the theoretical
point of view. Measurements with He ions will enable a consistency
check of the electron mass value, and in future an improvement of the He
nuclear mass and a determination of the fine-structure constant
Binaries in star clusters and the origin of the field stellar population
Many, possibly most, stars form in binary and higher-order multiple systems.
Therefore, the properties and frequency of binary systems provide strong clues
to the star-formation process, and constraints on star-formation models.
However, the majority of stars also form in star clusters in which the birth
binary properties and frequency can be altered rapidly by dynamical processing.
Thus, we almost never see the birth population, which makes it very difficult
to know if star formation (as traced by binaries, at least) is universal, or if
it depends on environment. In addition, the field population consists of a
mixture of systems from different clusters which have all been processed in
different ways.Comment: 16 pages, no figures. To appear as invited review article in a
special issue of the Phil. Trans. Royal Soc. A: Ch. 8 "Star clusters as
tracers of galactic star-formation histories" (ed. R. de Grijs). Fully peer
reviewed. LaTeX, requires rspublic.cls style fil
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