pinecone/core-2020-05-10-deduplication huggingface dataset:
On Effective Spacetime Dimension in the Ho\v{r}ava-Lifshitz Gravity

In this manuscript we explicitly compute the effective dimension of spacetime
in some backgrounds of Ho\v{r}ava-Lifshitz (H-L) gravity. For all the cases
considered, the results are compatible with a dimensional reduction of the
spacetime to $d+1=2$, at high energies (ultraviolet limit), which is confirmed
by other quantum gravity approaches, as well as to $d+1=4$, at low energies
(infrared limit). This is obtained by computing the free energy of massless
scalar and gauge fields. We find that the only effect of the background is to
change the proportionality constant between the internal energy and
temperature. Firstly, we consider both the non-perturbative and perturbative
models involving the matter action, without gravitational sources but with
manifest time and space symmetry breaking, in order to calculate modifications
in the Stephan-Boltzmann law. When gravity is taken into account, we assume a
scenario in which there is a spherical source with mass $M$ and radius $R$ in
thermal equilibrium with radiation, and consider the static and spherically
symmetric solution of the H-L theory found by Kehagias-Sfetsos (K-S), in the
weak and strong field approximations. As byproducts, for the weak field regime,
we used the current uncertainty of the solar radiance measurements to establish
a constraint on the $\omega$ free parameter of the K-S solution. We also
calculate the corrections, due to gravity, to the recently predicted attractive
force that black bodies exert on nearby neutral atoms and molecules.Comment: references adde
Thermodynamic Product Formula for Ho\v{r}ava Lifshitz Black Hole

We examine the thermodynamic properties of inner and outer horizons in the
background of Ho\v{r}ava Lifshitz black hole. We compute the \emph{horizon
radii product, the surface area product, the entropy product, the surface
temperature product, the Komar energy product and the specific heat product}
for both the horizons of said black hole. We show that surface area product,
entropy product and irreducible mass product are \emph{universal} quantities,
whereas the surface temperature product, Komar energy product and specific heat
product are \emph{not universal} quantities because they all are depends on
mass parameter. We also observe that the \emph{First law} of black hole
thermodynamics and \emph {Smarr-Gibbs-Duhem } relations do not hold for this
black hole. The underlying reason behind this failure due to the scale
invariance of the coupling constant. We further derive the \emph{Smarr mass
formula} and \emph{Christodolou-Ruffini mass formula} for such black hole
spacetime. Moreover we study the stability of such black hole by computing the
specific heat for both the horizons. It has been observed that under certain
condition the black hole possesses second order phase transition.Comment: 7 pages Physics Letters B, 30 July 201
Constraining planet structure from stellar chemistry: the cases of
  CoRoT-7, Kepler-10, and Kepler-93

We explore the possibility that the stellar relative abundances of different
species can be used to constrain the bulk abundances of known transiting rocky
planets. We use high resolution spectra to derive stellar parameters and
chemical abundances for Fe, Si, Mg, O, and C in three stars hosting low mass,
rocky planets: CoRoT-7, Kepler-10, and Kepler-93. These planets follow the same
line along the mass-radius diagram, pointing toward a similar composition. The
derived abundance ratios are compared with the solar values. With a simple
stoichiometric model, we estimate the iron mass fraction in each planet,
assuming stellar composition. We show that in all cases, the iron mass fraction
inferred from the mass-radius relationship seems to be in good agreement with
the iron abundance derived from the host star's photospheric composition. The
results suggest that stellar abundances can be used to add constraints on the
composition of orbiting rocky planets.Comment: A&A Letters, in pres
Analysis of the acoustic cut-off frequency and HIPs in six Kepler stars
  with stochastically excited pulsations

Gravito-acoustic modes in the Sun and other stars propagate in resonant
cavities with a frequency below a given limit known as the cut-off frequency.
At higher frequencies, waves are no longer trapped in the stellar interior and
become traveller waves. In this article we study six pulsating solar-like stars
at different evolutionary stages observed by the NASA Kepler mission. These
high signal-to-noise targets show a peak structure that extends at very high
frequencies and are good candidates for studying the transition region between
the modes and the interference peaks or pseudo-modes. Following the same
methodology successfully applied on Sun-as-a-star measurements, we uncover the
existence of pseudo-modes in these stars with one or two dominant interference
patterns depending on the evolutionary stage of the star. We also infer their
cut-off frequency as the midpoint between the last eigenmode and the first peak
of the interference patterns. By using ray theory we show that, while the
period of one of the interference pattern is very close to half the large
separation the other, one depends on the time phase of mixed waves, thus
carrying additional information on the stellar structure and evolution.Comment: Accepted for publication in A&A. 14 pages, 28 figure
Metadynamics Surfing on Topology Barriers: the $CP^{N-1}$ Case

As one approaches the continuum limit, $QCD$ systems, investigated via
numerical simulations, remain trapped in sectors of field space with fixed
topological charge. As a consequence the numerical studies of physical
quantities may give biased results. The same is true in the case of two
dimensional $CP^{N-1}$ models. In this paper we show that metadynamics, when
used to simulate $CP^{N-1}$, allows to address efficiently this problem. By
studying $CP^{20}$ we show that we are able to reconstruct the free energy of
the topological charge $F(Q)$ and compute the topological susceptibility as a
function of the coupling and of the volume. This is a very important physical
quantity in studies of the dynamics of the $\theta$ vacuum and of the axion.
This method can in principle be extended to $QCD$ applications.Comment: Final version accepted on JHEP. Simulations extended and statistics
  made homogeneous to ease comparison with HM
Becoming a Performance Analyst :
                    Autoethnographic Reflections on Agency, and Facilitated Transformational Growth

This is an Accepted Manuscript of an article published by Taylor & Francis Group in Reflective Practice, on 3 September 2014, available online at: http://dx.doi.org/10.1080/14623943.2014.900014.This paper features an autoethnographic approach in presenting and reflecting upon the story of one higher education student???s rapid vocational and academic transformation. Initially an inconspicuous undergraduate student, Andrew experienced an accelerated development that catapulted him to working in elite sport performance analysis (PA) environments, within a year. PA is a sub-discipline of sports coaching that involves using the latest technological advances to influence sporting performance, through the objective analysis of performance data. This autoethnographic piece is partly Andrew???s personal reflection upon that journey towards his newfound profession, which initially grew out of his experience of a generic sports degree at a university. Through stepping out of his comfort zone, and analysing sports previously unknown to him, extraordinary progress was made, and various vocational and academic opportunities arose. The initial catalyst for this developmental journey was facilitated by coaching lecturer David, who reflects upon how Andrew???s story links to his own educational philosophies. Andrew and David explore what these stories might mean to them personally, including potential links to the metaphor of learning as becoming, and notions around the concepts of learner agency, and educational facilitation. The paper ends by exploring the theoretical frameworks that guided this paper???s structure and focu
Coreleased orexin and glutamate evoke nonredundant spike outputs and computations in histamine neurons.

Stable wakefulness requires orexin/hypocretin neurons (OHNs) and OHR2 receptors. OHNs sense diverse environmental cues and control arousal accordingly. For unknown reasons, OHNs contain multiple excitatory transmitters, including OH peptides and glutamate. To analyze their cotransmission within computational frameworks for control, we optogenetically stimulated OHNs and examined resulting outputs (spike patterns) in a downstream arousal regulator, the histamine neurons (HANs). OHR2s were essential for sustained HAN outputs. OHR2-dependent HAN output increased linearly during constant OHN input, suggesting that the OHN→HAN(OHR2) module may function as an integral controller. OHN stimulation evoked OHR2-dependent slow postsynaptic currents, similar to midnanomolar OH concentrations. Conversely, glutamate-dependent output transiently communicated OHN input onset, peaking rapidly then decaying alongside OHN→HAN glutamate currents. Blocking glutamate-driven spiking did not affect OH-driven spiking and vice versa, suggesting isolation (low cross-modulation) of outputs. Therefore, in arousal regulators, cotransmitters may translate distinct features of OHN activity into parallel, nonredundant control signals for downstream effectors
Search for microscopic black holes and string balls in final states with leptons and jets with the ATLAS detector at √s = 8 TeV

A search for an excess of events with multiple high transverse momentum objects including charged leptons and jets is presented, using 20.3 fb−1 of proton-proton collision data recorded by the ATLAS detector at the Large Hadron Collider in 2012 at a centre-of-mass energy of √s = 8TeV. No excess of events beyond Standard Model expectations is observed. Using extra-dimensional models for black hole and string ball production and decay, exclusion contours are determined as a function of the mass threshold for production and the fundamental gravity scale for two, four and six extra dimensions. For six extra dimensions, mass thresholds of 4.8–6.2TeV are excluded at 95% confidence level, depending on the fundamental gravity scale and model assumptions. Upper limits on the fiducial cross-sections for non-Standard Model production of these final states are set
MAGIC search for VHE gamma-ray emission from AE Aquarii in a multiwavelength context

Context. It has been claimed that the nova-like cataclysmic variable (CV) AE Aquarii (AE Aqr) is a very-high-energy (VHE, E >100 GeV) source both on observational and theoretical grounds.\ud
Aims. We search for VHE gamma-ray emission from AE Aqr during diferent states of the source at several wavelengths to confirm or rule out previous claims of detection of gamma-ray emission from this object.\ud
Methods. We report on observations of AE Aqr performed by MAGIC. The source was observed during 12 hours as part of a multiwavelength campaign carried out between May and June 2012 covering the optical, X-ray, and gamma-ray ranges. Besides MAGIC, the other facilities involved were the KVA, Skinakas, and Vidojevica telescopes in the optical and Swift in X-rays. We calculated integral upper limits coincident with diferent states of the source in the optical. We computed upper limits to the pulsed emission limiting the signal region to 30% of the phaseogram and we also searched for pulsed emission at diferent frequencies applying the Rayleigh test.\ud
Results. AE Aqr was not detected at VHE energies during the multiwavelength campaign. We establish integral upper limits at the 95% confidence level for the steady emission assuming the diferential flux proportional to a power-law function dф  /dE α E^(-Γ) with a Crab-like photon spectral index of Γ =2.6. The upper limit above 200 GeV is 6.4X10^(-12) cm^(-2)s^(-1) and above 1 TeV is 7.4X10^(-13) cm^(-2)s^(-1). We obtained an upper limit for the pulsed emission of 2.6X10^(-12) cm^(-2)s^(-1) for energies above 200 GeV. Applying the Rayleigh test for pulsed emission at diferent frequencies we did not find any significant signal.\ud
Conclusions. Our results indicate that AE Aqr is not a VHE gamma-ray emitter at the level of emission previously claimed. We have established the most constraining upper limits for the VHE gamma-ray emission of AE Aqr
Search for heavy Majorana neutrinos in μ±μ± + jets events in proton-proton collisions at s=8 TeV

A search is performed for heavy Majorana neutrinos (N) using an event signature defined by two muons of the same charge and two jets (mu(+/-)mu(+/-)jj). The data correspond to an integrated luminosity of 19.7 fb(-1) of proton-proton collisions at a center-of-mass energy of 8TeV, collected with the CMS detector at the CERN LHC. No excess of events is observed beyond the expected standard model background and upper limits are set on vertical bar V-mu N vertical bar(2) as a function of Majorana neutrino mass mN for masses in the range of 40-500GeV, where V-mu N is the mixing element of the heavy neutrino with the standard model muon neutrino. The limits obtained are vertical bar V-mu N vertical bar(2) &lt; 0.00470 for m(N) = 90GeV, vertical bar V-mu N vertical bar(2) &lt; 0.0123 for m(N) = 200GeV, and vertical bar V-mu N vertical bar(2) &lt; 0.583 for m(N) = 500 GeV. These results extend considerably the regions excluded by previous direct searches
Measurement of the t-channel single-top-quark production cross section and of the |Vtb| CKM matrix element in pp collisions at sqrt(s) = 8 TeV

Measurements are presented of the t-channel single-top-quark production cross section in proton-proton collisions at sqrt(s) = 8 TeV. The results are based on a data sample corresponding to an integrated luminosity of 19.7 inverse femtobarns recorded with the CMS detector at the LHC. The cross section is measured inclusively, as well as separately for top (t) and antitop (t-bar), in final states with a muon or an electron. The measured inclusive t-channel cross section is sigma[t-ch] = 83.6 +/- 2.3 (stat.) +/- 7.4 (syst.) pb. The single t and t-bar cross sections are measured to be sigma[t-ch,t] = 53.8 +/- 1.5 (stat.) +/- 4.4 (syst.) pb and sigma[t-ch,t-bar] = 27.6 +/- 1.3 (stat.) +/- 3.7 (syst.) pb, respectively. The measured ratio of cross sections is R[t-ch] = sigma[t-ch,t]/sigma[t-ch,t-bar] = 1.95 +/- 0.10 (stat.) +/- 0.19 (syst.), in agreement with the standard model prediction. The modulus of the Cabibbo-Kobayashi-Maskawa matrix element Vtb is extracted and, in combination with a previous CMS result at sqrt(s) = 7 TeV, a value abs(Vtb) = 0.998 +/- 0.038 (exp.) +/- 0.016 (theo.) is obtained
Scheme independent consequence of the NSVZ relation for =1 SQED with Nf flavors

The exact NSVZ β -function is obtained for =1 SQED with Nf flavors in all orders of the perturbation theory, if the renormalization group functions are defined in terms of the bare coupling constant and the theory is regularized by higher derivatives. However, if the renormalization group functions are defined in terms of the renormalized coupling constant, the NSVZ relation between the β -function and the anomalous dimension of the matter superfields is valid only in a certain (NSVZ) scheme. We prove that for =1 SQED with Nf flavors the NSVZ relation is valid for the terms proportional to (Nf)1 in an arbitrary subtraction scheme, while the terms proportional to (Nf)k with k⩾2 are scheme dependent. These results are verified by an explicit calculation of a three-loop β -function and a two-loop anomalous dimension made with the higher derivative regularization in the NSVZ and MOM subtraction schemes. In this approximation it is verified that in the MOM subtraction scheme the renormalization group functions obtained with the higher derivative regularization and with the dimensional reduction coincide
On exactly marginal deformations dual to B -field moduli of IIB theory on SE 5

The complex dimension of the space of exactly marginal deformations for quiver CFTs dual to IIB theory compactified on Y p , q is known to be generically three. Simple general formulas already exist for two of the exactly marginal directions in the space of couplings, one of which corresponds to the sum of the (inverse squared of) gauge couplings, and the other to the β -deformation. Here we identify the third exactly marginal direction, ∫ which is dual to the modulus ∫ 2 ‐ cycle B 2 $$ {\displaystyle {\int}_{2\hbox{-} \mathrm{cycle}}{B}_2} $$ on the gravity side. This identification leads to a relation between the field theory gauge couplings and the vacuum expectation value of the gravity modulus that we further support by a computation related to the chiral anomaly induced by added fractional branes. We also present a simple algorithm for finding similar exactly marginal directions in any CFT described by brane tiling, and demonstrate it for the quiver CFTs dual to IIB theory compactified on L 1,5,2 and the Suspended Pinch Point
Alpha induced reaction cross section measurements on 162 Er for the astrophysical γ process

The cross sections of the <math altimg="si1.gif" xmlns="http://www.w3.org/1998/Math/MathML"><mmultiscripts><mrow><mtext>Er</mtext></mrow><mprescripts/><none/><mrow><mn>162</mn></mrow></mmultiscripts><mo stretchy="false">(</mo><mi>α</mi><mo>,</mo><mi>γ</mi><mo stretchy="false">)</mo><mmultiscripts><mrow><mtext>Yb</mtext></mrow><mprescripts/><none/><mrow><mn>166</mn></mrow></mmultiscripts></math> and <math altimg="si2.gif" xmlns="http://www.w3.org/1998/Math/MathML"><mmultiscripts><mrow><mtext>Er</mtext></mrow><mprescripts/><none/><mrow><mn>162</mn></mrow></mmultiscripts><mo stretchy="false">(</mo><mi>α</mi><mo>,</mo><mi mathvariant="normal">n</mi><mo stretchy="false">)</mo><mmultiscripts><mrow><mtext>Yb</mtext></mrow><mprescripts/><none/><mrow><mn>165</mn></mrow></mmultiscripts></math> reactions have been measured for the first time. The radiative alpha capture reaction cross section was measured from <math altimg="si3.gif" xmlns="http://www.w3.org/1998/Math/MathML"><msub><mrow><mi>E</mi></mrow><mrow><mi>c</mi><mo>.</mo><mi>m</mi><mo>.</mo></mrow></msub><mo>=</mo><mn>16.09</mn><mtext> </mtext><mtext>MeV</mtext></math> down to <math altimg="si4.gif" xmlns="http://www.w3.org/1998/Math/MathML"><msub><mrow><mi>E</mi></mrow><mrow><mi>c</mi><mo>.</mo><mi>m</mi><mo>.</mo></mrow></msub><mo>=</mo><mn>11.21</mn><mtext> </mtext><mtext>MeV</mtext></math> , close to the astrophysically relevant region (which lies between 7.8 and 11.48 MeV at 3 GK stellar temperature). The <math altimg="si2.gif" xmlns="http://www.w3.org/1998/Math/MathML"><mmultiscripts><mrow><mtext>Er</mtext></mrow><mprescripts/><none/><mrow><mn>162</mn></mrow></mmultiscripts><mo stretchy="false">(</mo><mi>α</mi><mo>,</mo><mi mathvariant="normal">n</mi><mo stretchy="false">)</mo><mmultiscripts><mrow><mtext>Yb</mtext></mrow><mprescripts/><none/><mrow><mn>165</mn></mrow></mmultiscripts></math> reaction was studied above the reaction threshold between <math altimg="si5.gif" xmlns="http://www.w3.org/1998/Math/MathML"><msub><mrow><mi>E</mi></mrow><mrow><mi>c</mi><mo>.</mo><mi>m</mi><mo>.</mo></mrow></msub><mo>=</mo><mn>12.19</mn><mtext> and </mtext><mn>16.09</mn><mtext> </mtext><mtext>MeV</mtext></math> . The fact that the <math altimg="si1.gif" xmlns="http://www.w3.org/1998/Math/MathML"><mmultiscripts><mrow><mtext>Er</mtext></mrow><mprescripts/><none/><mrow><mn>162</mn></mrow></mmultiscripts><mo stretchy="false">(</mo><mi>α</mi><mo>,</mo><mi>γ</mi><mo stretchy="false">)</mo><mmultiscripts><mrow><mtext>Yb</mtext></mrow><mprescripts/><none/><mrow><mn>166</mn></mrow></mmultiscripts></math> cross sections were measured below the <math altimg="si6.gif" xmlns="http://www.w3.org/1998/Math/MathML"><mo stretchy="false">(</mo><mi>α</mi><mo>,</mo><mi mathvariant="normal">n</mi><mo stretchy="false">)</mo></math> threshold at first time in this mass region opens the opportunity to study directly the α -widths required for the determination of astrophysical reaction rates. The data clearly show that compound nucleus formation in this reaction proceeds differently than previously predicted
A novel class of MYB factors controls sperm cell formation in plants

This is the authors' final draft of a paper subsequently published as Current Biology, 2005, 15, pp. 244-248In contrast to animals, the plant male germ line is established after meiosis in distinctive haploid structures, termed pollen grains. Germ line arises by a distinct asymmetric division of the meiotic products. The fate of the resulting vegetative and generative cells are distinct. In contrast to the larger vegetative cell arrested in the G1 phase of the cell cycle, the smaller generative cell divides once to produce the two male gametes or sperm cells. Sperm cells are delivered to the female gametes by the pollen tube, which develops from the vegetative cell. In spite of recent efforts to understand pollen development  the molecular pathway controlling sperm cell ontogenesis is unknown. Here we present the isolation of DUO1, a novel R2R3 MYB gene of Arabidopsis, as the first gene shown to control male gamete formation in plants. DUO1 is specifically expressed in the male germ line and DUO1 protein accumulates in sperm cell nuclei. Mutations in DUO1 produce a single larger diploid sperm cell unable to perform fertilisation. DUO1 appears to be evolutionarily conserved in several plant species and defines a new subfamily of pollen-specific MYB genes.Peer reviewedPost prin
Detecting the effects of hydrocarbon pollution in the Amazon forest using hyperspectral satellite images.

The global demand for fossil energy is triggering oil exploration and production projects in remote areas of the world. During the last few decades hydrocarbon production has caused pollution in the Amazon forest inflicting considerable environmental impact. Until now it is not clear how hydrocarbon pollution affects the health of the tropical forest flora. During a field campaign in polluted and pristine forest, more than 1100 leaf samples were collected and analysed for biophysical and biochemical parameters. The results revealed that tropical forests exposed to hydrocarbon pollution show reduced levels of chlorophyll content, higher levels of foliar water content and leaf structural changes. In order to map this impact over wider geographical areas, vegetation indices were applied to hyperspectral Hyperion satellite imagery. Three vegetation indices (SR, NDVI and NDVI705) were found to be the most appropriate indices to detect the effects of petroleum pollution in the Amazon forest.This research has been self-founded by the corresponding author and has the support of the Secretariat for Science and Technology of Ecuador (SENESCYT). We thanks the Environmental Ministry of Ecuador for providing environmental studies and the Environmental Program for Pollution Remediation-PRAS for providing digital maps and high resolution satellite images of the study area. H. Balzter was supported by the Royal Society Wolfson Research Merit Award, 2011/R3 and the NERC National Centre for Earth Observation.Peer-reviewedPublisher Versio
Flowing from AdS5 to AdS3 with T 1,1.

We construct supersymmetric domain wall solutions of type IIB supergravity that interpolate between AdS5 × T 1,1 in the UV and AdS3 × R   2 × S 2 × S 3 solutions in the IR. The R   2 factor can be replaced with a two-torus and then the solution describes a supersymmetric flow across dimensions, similar to wrapped brane solutions. While the domain wall solutions preserve (0, 2) supersymmetry, the AdS3 solutions in the IR have an enhanced (4, 2) superconformal supersymmetry and are related by two T-dualities to the AdS3 × S 3 × S 3 × S 1 type IIB solutions which preserve a large (4, 4) superconformal super-symmetry. The domain wall solutions exist within the N = 4 D = 5 gauged supergravity theory that is obtained from a consistent Kaluza-Klein truncation of type IIB supergravity on T 1,1; a feature driving the flows is that two D = 5 axion like fields, residing in the N = 4 Betti multiplet, depend linearly on the two legs of the R   2 factor