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12214395 | [
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12205260 | [
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12103105 | [
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1555749 | [
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12132026 | [
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12201910 | [
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12203029 | [
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] | 2011crpa.conf..352B | [
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"Department of Physics and Maths, University of Insubria, Como, Italy... | [
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12213604 | [
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12224837 | [
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] | 1012 | 1012.1613_arXiv.txt | There exists overwhelming evidence, most recently from the Wilkinson Microwave Anisotropy Probe (WMAP) \cite{Komatsu:2008hk}, that non-baryonic cold dark matter comprises around 23 percent of the Universe's energy density. Identifying this dark matter, presumably an elementary particle, is one of the foremost contempor... | We have investigated the direct and indirect detection of the bino-Higgsino dark matter scenario, and explored its implications for the LHC. We first presented the prediction of SD cross section and the branching ratio of $B_s \to \mu^+\mu^-$, assuming that the WMAP relic density constraint is satisfied. Because the re... | 10 | 12 | 1012.1613 | If the lightest dark matter neutralino has a sufficiently large Higgsino component, its spin-independent and spin-dependent cross sections on nucleons can be sizable enough to be detected soon in direct and indirect surveys. We outline in this paper some characteristic features expected of mixed bino-Higgsino dark matt... | false | [
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12225442 | [
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] | 1012 | 1012.1339_arXiv.txt | \label{intro} The characterization of the flavor conversions for neutrinos emitted by a stellar collapse is a field of intense activity. In particular, the flavor transformation probabilities in supernovae (SNe) not only depend on the matter background~\cite{Matt,Dighe:1999bi}, but also on the neutrino fluxes themse... | We have performed an exploration on the dependence of multi-angle effects in self-induced supernova neutrino oscillations on the original neutrino fluxes. Most of the previous studies~\cite{Duan:2006an,Fogli:2007bk,Fogli:2008pt,EstebanPretel:2007ec} focused on neutrino fluxes typical of the accretion phase, with a pro... | 10 | 12 | 1012.1339 | The nonisotropic nature of the neutrino emission from a supernova (SN) core might potentially affect the flavor evolution of the neutrino ensemble, via neutrino-neutrino interactions in the deepest SN regions. We investigate the dependence of these “multiangle effects” on the original SN neutrino fluxes in a three-flav... | false | [
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12211853 | [
"Durán, Iván",
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"Holographic dark energy at the Ricci scale"
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] | 1012 | 1012.4988_arXiv.txt | Holographic models of late acceleration have become of fashion, among other things, because they link the dark energy density to the cosmic horizon, a global property of the universe, and have a close relationship to the spacetime foam \cite{jng1}, \cite{arzano}. For a summary motivation of holographic dark energy, se... | The statistical analysis sketched above shows that the ratio $\chi^{2}_{total}/dof$ is lower than unity for the holographic interacting model of section \ref{introduction}, whereby it is compatible with observation. However, as Table \ref{table:chi2} shows, the $\Lambda$CDM model fits better the same sets of data. Yet,... | 10 | 12 | 1012.4988 | We consider a holographic cosmological model in which the infrared cutoff is fixed by the Ricci's length and dark matter and dark energy do not evolve separately but interact non-gravitationally with one another. This substantially alleviates the cosmic coincidence problem as the ratio between both components remains f... | false | [
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] | 1012 | 1012.1755_arXiv.txt | \label{sec:intro} The H.E.S.S. (High Energy Stereoscopic System) instrument is an array of four imaging atmospheric Cherenkov telescopes working in stereoscopic mode. It is located in Namibia, in the Khomas Highland and has started its operations in 2004. Each of the present ``small'' Cherenkov telescopes (SCT) has a 1... | This paper describes the design and implementation of the L2 trigger system for the second phase of the H.E.S.S. experiment. The L2 trigger will be used to reject night sky background related and isolated muon events and thus reduce the trigger rate. The principle of the trigger is to build a 2-bit (``combined'') map o... | 10 | 12 | 1012.1755 | HESS is an array of atmospheric Cherenkov telescopes dedicated to GeV-TeV γ-ray astronomy. The original array has been in operation since the beginning of 2004. It is composed of four 12-m diameter telescopes. The installation of a fifth 28-m diameter telescope is being completed. This telescope will operate both in st... | false | [
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... | 7.267416 | 0.873197 | 13 |
12168000 | [
"Pápai, Péter",
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] | 2011ApJ...732...27P | [
"Integrated Sachs-Wolfe Imprint of Superstructures on Linear Scales"
] | 37 | [
"Institute for Astronomy, University of Hawaii at Manoa, HI, USA ; Department of Physics and Astronomy, University of Hawaii at Manoa, HI, USA",
"Institute for Astronomy, University of Hawaii at Manoa, HI, USA",
"INAF Osservatorio Astronomico di Brera, Via E. Bianchi 46, 23807 Merate (LC), Italy"
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] | 1012 | 1012.3750_arXiv.txt | Since the first sky maps of the Wilkinson Microwave Anisotropy Probe (WMAP) were published, there have been claims for the existence of circular features (spots and rings) in the cosmic microwave background (CMB) \citep{Cruz2005,Granett2008}. Their origin and statistical significance are still debated. Sources, such as... | \label{discussion} This paper is the continuation of the work started in \cite{Papai2010}. Our goal is to estimate the ISW imprint of large spherical dark matter overdensities and underdensities. In Section \ref{PinS}, first, we tested a simple Gaussian model for density profiles in the HVS. We created an ISW map by r... | 10 | 12 | 1012.3750 | We build a model for the density and integrated Sachs-Wolfe (ISW) profile of supervoid and supercluster structures. Our model assumes that fluctuations evolve linearly from an initial Gaussian random field. We find these assumptions capable of describing N-body simulations and simulated ISW maps remarkably well on larg... | false | [
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1267068 | [
"Guo, Jingnan",
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"Kontar, Eduard P."
] | 2011ApJ...728....4G | [
"Relationship Between Hard and Soft X-ray Emission Components of a Solar Flare"
] | 13 | [
"School of Physics and Astronomy, SUPA, University of Glasgow, Glasgow G12 8QQ, UK; Max-Planck Institute for Solar System Research, Katlenburg-Lindau 37191, Germany; Purple Mountain Observatory, Nanjing 210008, China",
"School of Physics and Astronomy, SUPA, University of Glasgow, Glasgow G12 8QQ, UK; Purple Moun... | [
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] | 1012 | 1012.4346_arXiv.txt | \label{intro} High-energy observations of solar flares with the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) \citep{lin2002rhessi} allows high resolution studies over a broad energy range from 3 keV soft X-rays to $\gamma$-rays up to 17 MeV. The photon flux in the energy range of $\sim 20 - 100$~keV ... | \label{s:conclusions} We have developed a new method to study in detail the temporal evolution of thermal and non-thermal photon fluxes in solar flares. The application of this method to a flare on Feburary 20 2002 demonstrates that as expected, the low energy part of the spectrum evolves slowly, and the high energy p... | 10 | 12 | 1012.4346 | X-ray observations of solar flares routinely reveal an impulsive high-energy and a gradual low-energy emission component, whose relationship is one of the key issues of solar flare study. The gradual and impulsive emission components are believed to be associated with, respectively, the thermal and nonthermal component... | false | [
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12164208 | [
"Mannarelli, Massimo",
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] | 2011AIPC.1343..577M | [
"Dissipative processes in superfluid neutron stars"
] | 0 | [
"Departament d'Estructura i Constituents de la Matèria and Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona, Martí i Franquès 1, 08028 Barcelona, Spain",
"Università di Bari, I-70126 Bari, Italia and .N.F.N., Sezione di Bari, I-70126 Bari, Italia",
"Instituto de Ciencias del Espacio (IEEC/CSIC)... | null | [
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] | 1012 | 1012.0345_arXiv.txt | Fermionic superfluidity might be realized in the interior of neutron stars where the temperature is low and the typical energy scale of particles is extremely high. In particular, in the inner crust of standard neutron stars the attractive interaction between neutrons can lead to the formation of a BCS condensate. ... | 10 | 12 | 1012.0345 | We present some results about a novel damping mechanism of r-mode oscillations in neutron stars due to processes that change the number of protons, neutrons and electrons. Deviations from equilibrium of the number densities of the various species lead to the appearance in the Euler equations of the system of a dissipat... | false | [
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12228750 | [
"Pakter, Renato",
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"Core-Halo Distribution in the Hamiltonian Mean-Field Model"
] | 56 | [
"Instituto de Física, Universidade Federal do Rio Grande do Sul, Caixa Postal 15051, CEP 91501-970, Porto Alegre, Rio Grande do Sul, Brazil",
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] | 1012 | 1012.0035_arXiv.txt | 10 | 12 | 1012.0035 | We study a paradigmatic system with long-range interactions: the Hamiltonian mean-field (HMF) model. It is shown that in the thermodynamic limit this model does not relax to the usual equilibrium Maxwell-Boltzmann distribution. Instead, the final stationary state has a peculiar core-halo structure. In the thermodynamic... | false | [
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12225445 | [
"Beyer, J.",
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] | 2011PhRvD..84b3010B | [
"Coupled dark energy and dark matter from dilatation anomaly"
] | 17 | [
"Institut für Theoretische Physik, Universität Heidelberg, Philosophenweg 16, 69120 Heidelberg, Germany",
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"10.1103/PhysRevD.84.023010",
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] | 1012 | 1012.1175_arXiv.txt | Dilatation symmetry and its anomaly could play an important role for cosmology \cite{Wetterich:1987fm}. Models with a dilatation symmetric fixed point could provide a dynamical solution for the cosmological constant problem \cite{Wetterich:1994bg, Wetterich:1987fm, Wetterich:2002wm}. As one of the most characteristic f... | In summary, we have found rather simple models for coupled cosmon and bolon scalar fields which realize a consistent cosmology without the need of other dark matter particles. The essential ingredients are the presence of a period where the bolon energy density is much smaller than radiation, and the increase of the bo... | 10 | 12 | 1012.1175 | Cosmological runaway solutions may exhibit an exact dilatation symmetry in the asymptotic limit of infinite time. In this limit, the massless dilaton or cosmon could be accompanied by another massless scalar field—the bolon. At finite time, small time-dependent masses for both the cosmon and the bolon are still present... | false | [
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2418558 | [
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] | 2011AmJPh..79..461G | [
"Equation of the field lines of an axisymmetric multipole with a source surface"
] | 12 | [
"Astrophysics Group, School of Physics, University of Exeter, Exeter, EX4 4QL, United Kingdom, and California Institute of Technology, MC 249-17, Pasadena, California 91101"
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] | 1012 | 1012.4799_arXiv.txt | The solution of Laplace's equation by separation of variables for the electrostatic potential in a region external to a charge distribution is a standard topic in graduate and undergraduate courses in electromagnetism.\cite{jea27,ble76,hea95,wyl99} As an example application, the long-range interaction between molecular... | \label{sum} Over the past five years the current generation of optical spectropolarimeters has allowed stellar magnetic field topologies to be probed in unprecedented detail. Large observational programs have provided maps of the magnetic fields of stars spanning a range of masses, rotation rates, and evolutionary stag... | 10 | 12 | 1012.4799 | Optical spectropolarimeters can be used to produce maps of the surface magnetic fields of stars and hence to determine how stellar magnetic fields vary with stellar mass, rotation rate, and evolutionary stage. In particular, we now can map the surface magnetic fields of forming solar-like stars, which are still contrac... | false | [
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3237698 | [
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12225187 | [
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] | 1012 | 1012.2893_arXiv.txt | String theory landscape points towards ultimate unification of particle physics and geography. If the landscape is real it is very likely that in the short and midterm future particle physicists will be busy by mapping the compactification manifold where we happened to live. In the most optimistic scenario---if extra... | \label{conclusions} In this paper we outlined a proposal how rotating astrophysical black hole may open a new window into hidden QCD-like gauge sectors coupled to light axions. Thanks to axion superradiance rotating black holes may give rise to violent bursts of electromagnetic radiation with initial frequencies set by... | 10 | 12 | 1012.2893 | Superradiant instability turns rotating astrophysical black holes into unique probes of light axions. We consider what happens when a light axion is coupled to a strongly coupled hidden gauge sector. In this case superradiance results in an adiabatic increase of a hidden sector CP-violating θ parameter in a near horizo... | false | [
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12208584 | [
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] | 2011JHEP...04..009H | [
"The everpresent η-problem: knowledge of all hidden sectors required"
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"Physics Department, FCFM, Universidad de Chile",
"Instituut-Lorentz for Theoretical Physics, Universiteit Leiden",
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] | 1012 | 1012.5966_arXiv.txt | \label{sec:intro} The construction of realistic models of slow-roll inflation in supergravity is a longstanding puzzle. Supersymmetry can alleviate the finetuning necessary to obtain slow-roll inflation --- if one assumes that the inflaton is a modulus of the supersymmetric ground state --- but cannot solve it complete... | In this paper we have studied the effect of hidden sectors on the finetuning of $F$-term inflation in supergravity, identifying a number of issues in the current methodology of finetuning inflation in supergravity. Finetuning inflationary models is only valid when the neglected physics does not affect this finetuning, ... | 10 | 12 | 1012.5966 | We argue that the η-problem in supergravity inflation cannot be solved without knowledge of the ground state of hidden sectors that are gravitationally coupled to the inflaton. If the hidden sector breaks supersymmetry independently, its fields cannot be stabilized during cosmological evolution of the inflaton. We show... | false | [
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1179849 | [
"Bournaud, Frédéric",
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] | 2011IAUS..271..160B | [
"Star formation in galaxy mergers: ISM turbulence, dense gas excess, and scaling relations for disks and starbusts"
] | 21 | [
"CEA, IRFU, SAp – CEA Saclay, F-91191 Gif-sur-Yvette, France.",
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] | 1012 | 1012.5227_arXiv.txt | Evidence that interactions and mergers can strongly trigger the star formation activity of galaxies has been observed for more than two decades \citep[e.g.,][]{sanders88}. Nevertheless, both the underlying mechanisms the role of mergers in the cosmic budget of star formation remain largely unknown. Mergers have long ap... | The results presented here were based mostly on low-redshift merger simulations. A recent set of high-redshift merger simulations with AMR is presented in Bournaud et al. (2011), and shows similar increase in the ISM velocity dispersions and clumpiness in mergers, with extended starbursts and high $\Sigma_{\mathrm SFR}... | 10 | 12 | 1012.5227 | Galaxy interactions and mergers play a significant, but still debated and poorly understood role in the star formation history of galaxies. Numerical and theoretical models cannot yet explain the main properties of merger-induced starbursts, including their intensity and their spatial extent. Usually, the mechanism inv... | false | [
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2262815 | [
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"Galaxy and Mass Assembly (GAMA): galaxies at the faint end of the Hα luminosity function"
] | 31 | [
"Australian Astronomical Observatory, PO Box 296, Epping, NSW 1710, Australia",
"Australian Astronomical Observatory, PO Box 296, Epping, NSW 1710, Australia",
"Australian Astronomical Observatory, PO Box 296, Epping, NSW 1710, Australia",
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"10.1111/j.1365-2966.2011.18210.x",
"10.48550/arXiv.1012.3771"
] | 1012 | 1012.3771_arXiv.txt | \label{sect:intro} Recent investigations into the evolutionary properties of galaxies have established that the distribution of galaxy colours exhibits a strong bimodality, separating red, quiescent early-type galaxies, with little ongoing star formation, from a blue sequence of star-forming spiral galaxies (e.g. \cit... | \label{sect:discussion} We have investigated the properties of a sample of 90 of the faintest-H$\alpha$ luminosity galaxies from the $r-$band--selected GAMA survey. We find these galaxies to generally be low-stellar mass, blue, in low-density environments with a range of star formation histories. % This is the most ... | 10 | 12 | 1012.3771 | We present an analysis of the properties of the lowest Hα-luminosity galaxies (L<SUB>Hα</SUB>≤ 4 × 10<SUP>32</SUP> W; SFR < 0.02 M<SUB>⊙</SUB> yr<SUP>-1</SUP>, with SFR denoting the star formation rate) in the Galaxy And Mass Assembly survey. These galaxies make up the rise above a Schechter function in the number d... | false | [
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12206986 | [
"Rani, B.",
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] | 2011JApA...32..217R | [
"Variability of Spectral Energy Distribution of Blazar S5 0716+714"
] | 2 | [
"Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital, India",
"Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital, India",
"Department of Physics, The College of New Jersey, Ewing, USA"
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"2016MNRAS.458.2350W",
"2018AJ....155...90F"
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"10.1007/s12036-011-9055-y",
"10.48550/arXiv.1012.1774"
] | 1012 | 1012.1774_arXiv.txt | \label{sec:intro} S5 0716+714 is a bright, high declination BL Lac object at a redshift, $z = 0.31 \pm$0.08 (Nilsson et al.\ 2008). This source has been extensively studied across the whole electromagnetic spectrum and exhibits strong variability on a wide range of timescales, ranging from minutes to years (e.g., Wagne... | \subsection{Limitations to the model} Although, as seen in Fig.\ 3, we were able to achieve reasonably good fits of the synchrotron emission for all six SEDs of the source, one should bear in mind that the one-zone BPL model is over-simplified in accounting for the radio-optical blazar emission. The applicability of ... | 10 | 12 | 1012.1774 | The emission from blazars is known to be variable at all wavelengths. The flux variability is often accompanied by spectral changes. Spectral energy distribution (SED) changes must be associated with changes in the spectra of emitting electrons and/or the physical parameters of the jet. Meaningful modeling of blazar br... | false | [
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12225612 | [
"Chongchitnan, Sirichai",
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] | 2011PhRvD..83h3504C | [
"Scale-dependent bias from the reconstruction of non-Gaussian distributions"
] | 9 | [
"Department of Physics, University of Oxford and Beecroft Institute for Particle Astrophysics and Cosmology, Denys Wilkinson Building, 1 Keble Road, Oxford, OX1 3RH, UK",
"Department of Physics, University of Oxford and Beecroft Institute for Particle Astrophysics and Cosmology, Denys Wilkinson Building, 1 Keble ... | [
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"10.1103/PhysRevD.83.083504",
"10.48550/arXiv.1012.1859"
] | 1012 | 1012.1859_arXiv.txt | One of the most intriguing unanswered questions in cosmology is whether or not the primordial seeds that grew into large-scale structures observed today were laid down as a Gaussian random field. In the simplest single-field inflation model of the early Universe, the initial distribution of the primordial seeds, or den... | \lab{conc} In this work, we have demonstrated an alternative method of calculating the bias in the clustering of rare objects in the presence of primordial non-Gaussianity. Our method is based on the reconstruction of the pdf of density fluctuations using the Edgeworth series in one and two variables. The bias obtain... | 10 | 12 | 1012.1859 | Primordial non-Gaussianity introduces a scale-dependent variation in the clustering of density peaks corresponding to rare objects. This variation, parametrized by the bias, is investigated on scales where a linear perturbation theory is sufficiently accurate. The bias is obtained directly in real space by comparing th... | false | [
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2790818 | [
"Morlino, G.",
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] | 2011crpa.conf..550M | [
"Shock acceleration in partially neutral plasmas"
] | 1 | [
"INAF, Osservatorio Astrofisico di Arcetri, L.go E. Fermi-5, Firenze, 50125, Italy;",
"INAF, Osservatorio Astrofisico di Arcetri, L.go E. Fermi-5, Firenze, 50125, Italy",
"INAF, Osservatorio Astrofisico di Arcetri, L.go E. Fermi-5, Firenze, 50125, Italy",
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"2011ApJ...731L..14R"
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"10.1142/9789814329033_0068",
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] | 1012 | 1012.2966_arXiv.txt | \label{sec:intro} Supernova remnants (SNRs) are thought to be the primary sources of Galactic cosmic rays (CRs). Diffusive shock acceleration (DSA) occurring around the forward shock is considered the most promising mechanism for the acceleration of particles up to very high energies. In order to explain the flux of ... | \label{sec:disc} We consider a typical case of shock with the following parameters: shock speed $u_0=2000$ km/s, total upstream density $\rho_0= 1 \rm cm^{-3}$, neutral fraction 50\%, upstream temperature $T_0=10^4$ K, upstream magnetic field strength $B_1= 10 \mu$G and maximum momentum of accelerated protons fixed to ... | 10 | 12 | 1012.2966 | We present the non-linear theory of shock acceleration applied to SNRs expanding into partially neutral plasma. Using this theory we show how the Balmer lines detected from young SNRs can be used to test the efficiency of shocks in the production of cosmic rays. In particular we investigate the effect of charge-exchang... | false | [
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... | 4.547194 | 4.54249 | -1 |
12205181 | [
"López-Morales, M."
] | 2011hsa6.conf...60L | [
"Exoplanet atmospheres: a brand-new and rapidly expanding research field"
] | 1 | [
"Institut de Ciencies de L'Espai (CSIC-IEEC), Campus UAB, Fac. Ciencies. Torre C5 parell 2, 08193 Bellaterra, Barcelona, Spain; Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Road NW, Washington, DC, 20015, USA"
] | [
"2012A&A...537A.147H"
] | [
"astronomy"
] | 6 | [
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] | 1012 | 1012.2157_arXiv.txt | } The introduction of any general talk about exoplanets always includes an account of the number of planets found. The number of planets discovered as of mid-September 2010 was 490\footnote{http://exoplanet.eu}. All exoplanets detected thus far, and recognized as such by the IAU, have been discovered within the past 1... | The detection and characterization of exoplanet amospheres is a brand new field which has started to bloom just in the past 3--4 years, thanks first to the advent of the SST, and most recently to the quick start off of successful detections with telescopes on the ground. Basically all atmospheres detected thus far are ... | 10 | 12 | 1012.2157 | The field of exoplanets is quickly expanding from just the detectionof new planets and the measurement of their most basic parameters,such as mass, radius and orbital configuration, to the firstmeasurements of their atmospheric characteristics, such astemperature, chemical composition, albedo, dynamics andstructure. He... | false | [
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"Radio Flaring Activity of 3C 345 and its Connection to Gamma-ray Emission"
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] | 1012 | 1012.2820_arXiv.txt | The quasar \object{3C~345} is one of the best studied ``superluminal'' radio sources, with its parsec-scale radio emission monitored over the past 30 years. Substantial variability of the optical (\cite{1984Ap.....20..461B,1990A&A...239L...9K}) and radio (\cite{1996ASPC..110..208A, 1998A&AS..132..305T, 1999ApJ...521..5... | We have found a correspondence between the long-term \textit{Fermi}-LAT lightcurve of the region 1FGL~J1642.5$+$3947 and the radio emission of 3C~345, establishing the detection of $\gamma$-ray emission from 3C~345 by comparison of radio and $\gamma$-ray variability. More importantly, we find $\gamma$-ray emission to ... | 10 | 12 | 1012.2820 | 3C 345 is one of the archetypical active galactic nuclei, showing structural and flux variability on parsec scales near a compact unresolved radio core. During the last 2 years, the source has been undergoing a period of high activity visible in the broad spectral range, from radio through high-energy bands. We have be... | false | [
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] | 2011ASSP...27...47P | [
"Measuring the Halo Mass Function in Loose Groups"
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"Department of Physics, West Virginia University",
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"Centre for Astrophysics, University of Central Lancashire",
"School of Physics, M013, University of Western Australia",
"RSAA, Mount Stromlo Observatory",
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] | 1012 | 1012.1362_arXiv.txt | 10 | 12 | 1012.1362 | Using data from our Parkes and ATCA HI survey of six groups analogous to the Local Group, we find that the HI mass function and velocity distribution function for loose groups are the same as those for the Local Group. Both mass functions confirm that the "missing satellite" problem exists in other galaxy groups. | false | [
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"Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA; Warsaw University Astronomical Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland",
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4898954 | [
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"Galliano, F.",
"Charmandaris, V.",
"Madden, S.",
"Kunth, D."
] | 2011ApJ...728...45L | [
"Influence of the Environment on Polycyclic Aromatic Hydrocarbon Emission in Star-forming Regions"
] | 28 | [
"Center for Radiophysics and Space Research, Cornell University, Space Sciences Building, Ithaca, NY 14853-6801, USA; Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot DAPNIA/Service d'Astrophysique Bât. 709, CEA-Saclay, F-91191 Gif-sur-Yvette Cédex, France",
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] | 1012 | 1012.1728.txt | \label{sec:intro} From a simplistic chemical viewpoint, the abundance of molecules in the interstellar medium (ISM) of galaxies should scale with the metallicity of the environment, either because of the presence of nucleosynthetic constituents or because of the need for catalysts (dust grains). Obviously, indirect co... | In this paper, we first investigated the PAH emission properties of several sources within three giant H\2\ regions, NGC\,3603 in the Milky Way, 30\,Dor in the LMC, and N\,66 in the SMC. The sample spans an interesting range of metallicities (down to $0.2$\,Z$_\odot$) and physical conditions (ISRF hardness). The sample... | 10 | 12 | 1012.1728 | We investigate the emission properties of polycyclic aromatic hydrocarbons (PAHs) in various metallicity environments with the Infrared Spectrograph on board Spitzer. Local giant H II regions are used as references as they enable access to the distinct interstellar medium components that contribute to the mid-infrared ... | false | [
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2388730 | [
"Price, Daniel J."
] | 2011IAUS..270..169P | [
"Magnetic fields and Turbulence in Star Formation using Smoothed Particle Hydrodynamics"
] | 3 | [
"Centre for Stellar and Planetary Astrophysics, Monash University, Clayton Vic 3800, Australia."
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] | 1012 | 1012.4547_arXiv.txt | Magnetic fields and turbulence are thought to be two of the most important ingredients in the star formation process, so it is critical that we are able to model the effect of both in star formation simulations. Smoothed Particle Hydrodynamics (SPH, for recent reviews see \citealt{monaghan05,price04}), since it is a La... | In summary: \begin{itemize} \item Being a television presenter is easier than getting MHD in SPH to work \item Development of MHD in SPH would proceed faster in the absence of arguments over basic misunderstandings of SPH which require lengthy comparison projects to resolve. \item Simulations with supercritical field s... | 10 | 12 | 1012.4547 | Firstly, we give a historical overview of attempts to incorporate magnetic fields into the Smoothed Particle Hydrodynamics method by solving the equations of Magnetohydrodynamics (MHD), leading an honest assessment of the current state-of-the-art in terms of the limitations to performing realistic calculations of the s... | false | [
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3825907 | [
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] | 1012 | 1012.3659_arXiv.txt | \subsection{Background} The Ninth Cambridge (9C) Survey of Radio Sources \citep{waldram2003,waldram2010}, carried out using the Ryle Telescope (RT) at an observing frequency of 15.2 GHz, was a milestone in the exploration of the high-radio-frequency sky, as the first survey of significant extent and depth at such a hi... | The AMI LA has been used to carry out the 10C survey, the deepest radio source survey of any significant extent ($\gtrsim 0.2$~deg$^{2}$) above 1.4~GHz. The resulting deep 15.7-GHz source counts are useful for the interpretation of CMB data, for which foreground radio sources are an important contaminant. The source ... | 10 | 12 | 1012.3659 | In a previous paper (Paper I), the observational, mapping and source-extraction techniques used for the Tenth Cambridge (10C) Survey of Radio Sources were described. Here, the first results from the survey, carried out using the Arcminute Microkelvin Imager Large Array (LA) at an observing frequency of 15.7 GHz, are pr... | false | [
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12168004 | [
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] | 2011ApJ...728...75K | [
"Kick Velocity Induced by Magnetic Dipole and Quadrupole Radiation"
] | 2 | [
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"Department of Physics, Hiroshima University, Higashi-Hiroshima 739-8526, Japan"
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"10.1088/0004-637X/728/2/75",
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] | 1012 | 1012.1376_arXiv.txt | The surface magnetic field strength $B_{s}$ of a pulsar is conventionally estimated by matching the rotational energy loss rate with the magnetic dipole radiation rate, that is, $B_{s} \approx $ $(3 c^{3} I P \dot{P} )^{1/2} /(2\sqrt{2} \pi R_{s} ^{3})$, where $I$ is the inertial moment, $R_{s}$ is the stellar radius, ... | Magnetic field strength itself is critical in most kick mechanisms. For example, $ B_{s} > 10^{15}$ G at the surface is required in asymmetric neutrino emission (e.g., \cite{ArLa99}), as well as in asymmetric magnetized core collapse (e.g., \cite{SaKoYa08}). The resultant velocity increases with the field strength beca... | 10 | 12 | 1012.1376 | We examine the recoil velocity induced by the superposition of magnetic dipole and quadrupole radiation from a pulsar/magnetar born with rapid rotation. The resultant velocity depends on not the magnitude, but rather the ratio of the two moments and their geometrical configuration. The model does not necessarily lead t... | false | [
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12226136 | [
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"New class of high-energy transients from crashes of supernova ejecta with massive circumstellar material shells"
] | 135 | [
"CCAPP, The Ohio State University, 191 W. Woodruff Avenue, Columbus, Ohio 43210, USA; Department of Physics, The Ohio State University, 191 W. Woodruff Avenue, Columbus, Ohio 43210, USA",
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] | 1012 | 1012.2834_arXiv.txt | Introduction} The much-anticipated era of multi-messenger astronomy is coming. GeV-TeV gamma rays, which are powerful tracers of cosmic rays (CRs), are detected by \textit{Fermi} and ground-based Cherenkov detectors. Neutrinos, which can uniquely identify the production of hadronic CRs and probe dense sources, are dete... | We have shown that SNe crashing into dense CSM are interesting targets for current and near-future high-energy detectors. Importantly, new types of coordinated multi-messenger searches are required to detect such $0.1-1$~yr transients. CR acceleration in dense surroundings is also motivated by recent gamma-ray observa... | 10 | 12 | 1012.2834 | A new class of core-collapse supernovae (SNe) has been discovered in recent years by optical/infrared surveys; these SNe suggest the presence of one or more extremely dense (∼10<SUP>5-11</SUP>cm<SUP>-3</SUP>) shells of circumstellar material (CSM) on 10<SUP>2-4</SUP>AU scales. We consider the collisions of the SN eject... | false | [
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11411263 | [
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] | 2010arXiv1012.5413W | [
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] | [
"10.48550/arXiv.1012.5413"
] | 1012 | 1012.5413_arXiv.txt | According to core accretion models \citep{mizuno-78}, giant gas planets such as Jupiter and Saturn formed via the accumulation of an protocore of rock and ice which gained solid material until it reached sufficient size to begin accreting the gaseous component of the protosolar nebula. The existence of solid ice in the... | The consequences of core erosion for planetary evolution models have been previously considered by \citet{stevenson-pss-82} and later \citet{guillot-book}. The effects of core erosion can potentially be detected either by orbital probes such as Juno or by atmospheric entry probes, since the redistribution of core mater... | 10 | 12 | 1012.5413 | Using ab initio simulations we investigate whether water ice is stable in the cores of giant planets, or whether it dissolves into the layer of metallic hydrogen above. By Gibbs free energy calculations we find that for pressures between 10 and 40 Mbar the ice-hydrogen interface is unstable at temperatures above approx... | false | [
"metallic hydrogen",
"giant planets",
"temperatures",
"solar and extrasolar giant planets",
"water ice",
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"Gibbs free energy calculations",
"ab initio simulations",
"the ice-hydrogen interface",
"the temperature",
"the cores",
"pressures",
... | 8.541603 | 14.676139 | 98 |
12162956 | [
"Morais, M. H. M.",
"Correia, A. C. M."
] | 2011A&A...525A.152M | [
"Stellar wobble caused by a nearby binary system: eccentric and inclined orbits"
] | 12 | [
"Department of Physics, I3N, University of Aveiro, Campus Universitário de Santiago, 3810-193 Aveiro, Portugal",
"Department of Physics, I3N, University of Aveiro, Campus Universitário de Santiago, 3810-193 Aveiro, Portugal; Astronomie et Systèmes Dynamiques, IMCCE-CNRS UMR 8028, 77 Avenue Denfert-Rochereau, 7501... | [
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"2021A&A...647A.160H",
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"2022MNRAS.510..708W",
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] | [
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] | 7 | [
"technique: radial velocities",
"celestial mechanics",
"planetary systems",
"binaries: general",
"Astrophysics - Earth and Planetary Astrophysics",
"Astrophysics - Solar and Stellar Astrophysics"
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"10.1051/0004-6361/201014812",
"10.48550/arXiv.1012.2375"
] | 1012 | 1012.2375_arXiv.txt | In \citet{Morais&Correia2008}, we studied a triple system consisting of a star perturbed by a binary system. Our aim was to derive an expression for the star's radial velocity in order to determine whether the binary's effect could be mistaken for that of a planet companion to the star. This question is relevant if one... | We have studied a triple system composed of a star and a binary system. The star and binary system have eccentric and inclined orbits. This is an extension of earlier work where we assumed that the star and binary system are on circular coplanar orbits \citep{Morais&Correia2008}. We demonstrated that if we are unawar... | 10 | 12 | 1012.2375 | Most extrasolar planets currently known were discovered by means of an indirect method that measures the stellar wobble caused by the planet. We previously studied a triple system composed of a star and a nearby binary on circular coplanar orbits. We showed that although the effect of the binary on the star can be diff... | false | [
"circular coplanar orbits",
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"a nearby binary",
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"the binarys effect",
"the circular case",
"the stellar wobble",... | 7.972722 | 13.994123 | -1 |
12213679 | [
"Mustill, Alexander J.",
"Wyatt, Mark C."
] | 2011MNRAS.413..554M | [
"A general model of resonance capture in planetary systems: first- and second-order resonances"
] | 71 | [
"Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA",
"Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA"
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"celestial mechanics",
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"10.1111/j.1365-2966.2011.18201.x",
"10.48550/arXiv.1012.3079"
] | 1012 | 1012.3079_arXiv.txt | Mean motion resonances (MMRs) occur when two objects' orbital periods are close to a ratio of two integers, and a particular combination of orbital angles, the resonant argument, is librating. Examples in the Solar System include Neptune and Pluto (3:2 resonance) and the inner Galilean moons of Jupiter (4:2:1 Laplace r... | We have systematically investigated the Hamiltonian model for capture of a test particle into first and second order resonances with a planet. The model reduces the full complexity of the restricted three body problem to only one degree of freedom, the resonant angle $\theta$, and two parameters, proportional to the pa... | 10 | 12 | 1012.3079 | Mean motion resonances are a common feature of both our own Solar system and of extrasolar planetary systems. Bodies can be trapped in resonance when their orbital semimajor axes change, for instance when they migrate through a protoplanetary disc. We use a Hamiltonian model to thoroughly investigate the capture behavi... | false | [
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"extrasolar plan... | 8.133412 | 15.033359 | -1 |
2725539 | [
"Breger, M.",
"Balona, L.",
"Lenz, P.",
"Hollek, J. K.",
"Kurtz, D. W.",
"Catanzaro, G.",
"Marconi, M.",
"Pamyatnykh, A. A.",
"Smalley, B.",
"Suárez, J. C.",
"Szabo, R.",
"Uytterhoeven, K.",
"Ripepi, V.",
"Christensen-Dalsgaard, J.",
"Kjeldsen, H.",
"Fanelli, M. N.",
"Ibrahim, K. A."... | 2011MNRAS.414.1721B | [
"Regularities in frequency spacings of δ Scuti stars: the Kepler star KIC 9700322"
] | 63 | [
"Institut für Astronomie der Universität Wien, Türkenschanzstr. 17, A-1180 Wien, Austria; Department of Astronomy, University of Texas, Austin, TX 78712, USA",
"South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa",
"Institut für Astronomie der Universität Wien, Türkenschanzstr. 17, ... | [
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"2012MNRAS.422.1092B",
"2012arXiv1210.5834P",
"2013A&A...552A..68Z",
"2013A&A...556A.... | [
"astronomy"
] | 2 | [
"stars: abundances",
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"stars: individual: KIC 9700322",
"stars: oscillations",
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"Astrophysics - Solar and Stellar Astrophysics"
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"10.1111/j.1365-2966.2011.18508.x",
"10.48550/arXiv.1012.4373"
] | 1012 | 1012.4373_arXiv.txt | The {\it Kepler Mission} is designed to detect Earth-like planets around solar-type stars \citep{Koch2010}. To achieve that goal, {\it Kepler} is continuously monitoring the brightness of over 150\,000 stars for at least 3.5\,yr in a 105 square degree fixed field of view. Photometric results show that after one year of... | Although this star was selected because of its very clear exactly equal frequency spacing, it turns out that the frequency spacing is explained as simple combination frequencies arising from non-linearities of the oscillation. This is different from another class of $\delta$\,Sct stars in the {\it Kepler} database whic... | 10 | 12 | 1012.4373 | In the faint star KIC 9700322 observed by the Kepler satellite, 76 frequencies with amplitudes from 14 to 29 000 ppm were detected. The two dominant frequencies at 9.79 and 12.57 d<SUP>-1</SUP> (113.3 and 145.5 μHz), interpreted to be radial modes, are accompanied by a large number of combination frequencies. A small a... | false | [
"combination frequencies",
"frequency",
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"various frequency combinations",
"Stanford University",
"non-radial pulsation",
"slow rotation",
"the combination frequencies",
"the rotation frequency",
"most forms",
"August",
"the observed frequ... | 7.073345 | 11.52259 | 81 |
12201905 | [
"Forbrich, J.",
"Wolk, S. J.",
"Güdel, M.",
"Benz, A.",
"Osten, R.",
"Linsky, J. L.",
"McLean, M.",
"Loinard, L.",
"Berger, E."
] | 2011ASPC..448..455F | [
"The Radio-X-ray Relation in Cool Stars: Are We Headed Toward a Divorce?"
] | 15 | [
"-",
"-",
"-",
"-",
"-",
"-",
"-",
"-",
"-"
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"2011ApJ...736...25F",
"2012ApJ...751L..42P",
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"2013A&A...551A..56F",
"2014PASA...31...21S",
"2014arXiv1412.6481L",
"2015RSPTA.37340259T",
"2016ApJ...818...24K",
"2016ApJ...822...93F",
"2018ASPC..517..395K",
"2018arXiv181006712K",
"2019ApJ...881...33H",
"2022ApJ...926L.... | [
"astronomy"
] | 6 | [
"Astrophysics - Solar and Stellar Astrophysics"
] | [
"1978A&A....68..145N",
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"1983ApJ...267..665W",
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"1985ApJ...293..584H",
"1988ApJ...324.1118K",
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"1993ApJ...410..301C",
"1993ApJ...413..710O",
"1993ApJ...415..236G",
"1993SoPh..146..... | [
"10.48550/arXiv.1012.1626"
] | 1012 | 1012.1626_arXiv.txt | \begin{figure}[t!] \includegraphics[angle=0,width=9cm]{forbrich_j_fig1.eps} \caption{Radio vs. X-ray correlation. Different symbols in the upper right part of the figure refer to different types of active stars. The letters in the lower left show the loci of solar flares (luminosities averaged over the duration of the ... | In short, we are not headed toward a divorce. Instead, the X-ray and radio luminosities of cool stars appear to be in an ``open relationship'' where a lot depends on the type of radio emission that is present. Until now, observational data have not always been sensitive enough to unambiguously identify dominant emissio... | 10 | 12 | 1012.1626 | This splinter session was devoted to reviewing our current knowledge of correlated X-ray and radio emission from cool stars in order to prepare for new large radio observatories such as the EVLA. A key interest was to discuss why the X-ray and radio luminosities of some cool stars are in clear breach of a correlation t... | false | [
"other active stars",
"cool stars",
"new large radio observatories",
"correlated X",
"clear breach",
"-ray and radio emission",
"the X-ray and radio luminosities",
"some cool stars",
"order",
"Güdel-Benz",
"the splinter website",
"the so-called Güdel-Benz relation",
"the EVLA",
"our curren... | 14.900987 | 5.956208 | 119 |
12205820 | [
"Shan, Chung-Lin"
] | 2011IJMPD..20.1453S | [
"Effects of Residue Background Events in Direct Detection Experiments on Identifying WIMP Dark Matter"
] | 1 | [
"Physics Division, National Center for Theoretical Sciences, No. 101, Sec. 2, Kuang-Fu Road, Hsinchu City 30013, Taiwan, R.O.C.;"
] | [
"2011arXiv1103.0481S"
] | [
"astronomy",
"physics"
] | 6 | [
"Dark matter",
"WIMP",
"direct detection",
"background",
"High Energy Physics - Phenomenology",
"Astrophysics - High Energy Astrophysical Phenomena",
"High Energy Physics - Experiment"
] | [
"1991PhLB..264..114E",
"1996PhR...267..195J",
"2007arXiv0710.4296S",
"2009AIPC.1185..631S",
"2009PhLB..681..305E",
"2010APh....32..318L",
"2010APh....33...60L",
"2010PhLB..687..294A",
"2010dmap.conf..521D"
] | [
"10.1142/S0218271811019633",
"10.48550/arXiv.1012.2625"
] | 1012 | 1012.2625_arXiv.txt | In our earlier work on the development of model--independent data analysis methods for extracting properties of Weakly Interacting Massive Particles (WIMPs) by using measured recoil energies from direct Dark Matter detection experiments directly% \cite{DMDDf1v,DMDDmchi,DMDDfp2,DMDDidentification-DARK2009}, it was assum... | In this article we reexamine the data analysis methods introduced in Refs.~\refcite{DMDDmchi,DMDDfp2} for determining the mass of Dark Matter particle and its spin--independent coupling on nucleons from measured recoil energies of direct detection experiments directly, by taking into account small fractions of residue ... | 10 | 12 | 1012.2625 | We reexamine the model-independent data analysis methods for extracting properties of Weakly Interacting Massive Particles (WIMPs) by using data (measured recoil energies) from direct Dark Matter detection experiments directly and, as a more realistic study, consider a small fraction of residue background events, which... | false | [
"direct Dark Matter detection experiments",
"residue background events",
"residue backgrounds",
"Weakly Interacting Massive Particles",
"measured recoil energies",
"Dark Matter",
"WIMP",
"other real WIMP-induced signals",
"data",
"the analyzed data sets",
"WIMPs",
"nucleons",
"properties",
... | 7.77506 | -2.371444 | 54 |
12203081 | [
"Blasi, P."
] | 2011crpa.conf..493B | [
"Cosmic Ray Acceleration in Supernova Remnants"
] | 16 | [
"INAF/Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5 Firenze, 50126, Italy;"
] | [
"2011ASTRA...7..245B",
"2011MmSAI..82..726R",
"2012A&A...545A..28L",
"2012ApJ...745..140Y",
"2012JCAP...01..010B",
"2013MNRAS.433..812O",
"2014PhRvD..89f3007L",
"2015EPJWC..9003001C",
"2018MNRAS.481..666O",
"2019Natur.573..235H",
"2019PhRvD..99f3004C",
"2020NuPhB.95415010B",
"2021MNRAS.504.1... | [
"astronomy"
] | 4 | [
"Style file",
"LATEX",
"Proceedings",
"World Scientific Publishing",
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] | [
"1934PhRv...46...76B",
"1964ocr..book.....G",
"1983A&A...125..249L",
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"1997ApJ...487..197E",
"2001AdSpR..27..717S",
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"2003A&A...407..249S",
"2004MNRAS.353..550B",
"2005A&A...433..229V",
"2005MNRAS.364L..76A",
"2006A&A...453..387P",
"2006AdSpR..37.1... | [
"10.1142/9789814329033_0061",
"10.48550/arXiv.1012.5005"
] | 1012 | 1012.5005_arXiv.txt | The possibility that the bulk of cosmic rays (CRs) observed at Earth may be generated in supernova remnants (SNRs) dates back to the '30s \cite{Baade:1934p886} and with time it has acquired the rank of a paradigm, mainly because of the fact that on energetic grounds \cite{Ginzburg:1964p929} supernovae are the only clas... | We provided a short review of the main arguments in favor and against the so called SNR paradigm for the origin of Galactic CRs. There is a train of recent evidence that efficient CR acceleration takes place in several SNRs. Probably the most striking findings are the detection of narrow X-ray rims interpreted as evide... | 10 | 12 | 1012.5005 | We review the main observational and theoretical facts about acceleration of Galactic cosmic rays in supernova remnants, discussing the arguments in favor and against a connection between cosmic rays and supernova remnants, the so-called supernova remnant paradigm for the origin of Galactic cosmic rays. Recent developm... | false | [
"Galactic cosmic rays",
"cosmic rays",
"supernova remnants",
"diffusive shock acceleration",
"supernova",
"acceleration",
"the supernova-cosmic ray connection",
"favor",
"neutrals",
"nuclei",
"Cherenkov",
"hydrogen",
"emphasis",
"presence",
"the circumstellar environment",
"Fermi-LAT a... | 4.41761 | 4.283011 | -1 |
12268525 | [
"Maciejewski, Andrzej J.",
"Przybylska, Maria",
"Stachowiak, Tomasz"
] | 2012arXiv1211.4639M | [
"Comment on \"Note on the Analytical Solution of the Rabi Model\""
] | 4 | [
"-",
"-",
"-"
] | [
"2013AnP...525L..23B",
"2013JMP....54j2104Z",
"2013JPhA...46G5301C",
"2013JPhA...46S5302Z"
] | [
"physics"
] | 2 | [
"Quantum Physics",
"Mathematical Physics"
] | [
"2011PhRvL.107j0401B",
"2012EL....10060010M",
"2012arXiv1210.1130M",
"2013AnP...525L..23B"
] | [
"10.48550/arXiv.1211.4639"
] | 1012 | 1012.2280_arXiv.txt | } Modified gravity is getting a lot of attention from the scientific community, owing in particular to the remarkable fact that it is able to describe early-time inflation as well as the late-time (dark energy) acceleration epoch in a unified way. This approach appears to be very economical, as it avoids the introduct... | } In summary, we have investigated in this paper some models corresponding to the quite simple exponential theory of modified $F(R)$ gravity which are able to explain the early- and late-time universe accelerations in a unified way. The viability conditions of the models have been carefully investigated and it has bee... | 10 | 12 | 1012.2280 | We make several comments on "Note on the Analytical Solution of the Rabi Model" (arXiv:1210.4946). | true | [
"several comments",
"the Rabi Model",
"the Analytical Solution",
"We"
] | -5.054205 | 6.42605 | -1 |
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