RAS_WEB (Page 4,114)

Dynamo theories. (arXiv:1903.07829v1 [physics.plasm-ph]) <a href="http://arxiv.org/find/physics/1/au:+Rincon_F/0/1/0/all/0/1">Francois Rincon</a> (CNRS, IRAP, France) These lecture notes are based on a tutorial given in 2017 at a plasma physics winter school in Les Houches. Their aim is to provide a self-contained graduate-student level introduction to the theory and modelling of the dynamo effect in turbulent fluids and plasmas, blended with a review of current research in the field. The primary focus is on the physical and mathematical concepts underlying different (turbulent) branches of dynamo theory, with some astrophysical, geophysical and experimental context disseminated throughout the document. The text begins with an introduction to the rationale, observational and historical rootsRead More →

GRBs as Probes of the Early Universe with TSO. (arXiv:1903.07835v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Tanvir_N/0/1/0/all/0/1">Nial Tanvir</a> (Leicester Univ.), <a href="http://arxiv.org/find/astro-ph/1/au:+Grindlay_J/0/1/0/all/0/1">Jonathan Grindlay</a> (CfA), <a href="http://arxiv.org/find/astro-ph/1/au:+Berger_E/0/1/0/all/0/1">Edo Berger</a> (CfA), <a href="http://arxiv.org/find/astro-ph/1/au:+Metzger_B/0/1/0/all/0/1">Brian Metzger</a> (Columbia Univ.), <a href="http://arxiv.org/find/astro-ph/1/au:+Gezari_S/0/1/0/all/0/1">Suvi Gezari</a> (Univ.Md.), <a href="http://arxiv.org/find/astro-ph/1/au:+Ivezic_Z/0/1/0/all/0/1">Zeljko Ivezic</a> (Univ. Washington), <a href="http://arxiv.org/find/astro-ph/1/au:+Jencson_J/0/1/0/all/0/1">Jacob Jencson</a> (Caltech), <a href="http://arxiv.org/find/astro-ph/1/au:+Kasliwal_M/0/1/0/all/0/1">Mansi Kasliwal</a> (Caltech), <a href="http://arxiv.org/find/astro-ph/1/au:+Kutyrev_A/0/1/0/all/0/1">Alexander Kutyrev</a> (NASA/GSFC), <a href="http://arxiv.org/find/astro-ph/1/au:+Macleod_C/0/1/0/all/0/1">Chelsea Macleod</a> (CfA), <a href="http://arxiv.org/find/astro-ph/1/au:+Melnick_G/0/1/0/all/0/1">Gary Melnick</a> (CfA), <a href="http://arxiv.org/find/astro-ph/1/au:+Purcell_B/0/1/0/all/0/1">Bill Purcell</a> (Ball Aerospace), <a href="http://arxiv.org/find/astro-ph/1/au:+Rieke_G/0/1/0/all/0/1">George Rieke</a> (Univ. AZ), <a href="http://arxiv.org/find/astro-ph/1/au:+Shen_Y/0/1/0/all/0/1">Yue Shen</a> (Univ. Illinois), <a href="http://arxiv.org/find/astro-ph/1/au:+Vasey_M/0/1/0/all/0/1">Michael Wood Vasey</a> (Univ. Pittsburgh) Long gamma-ray bursts (GRBs) are the most luminous known electromagnetic radiation sources in the Universe for the 3 to 300 sec of their prompt flashes (isotropicRead More →

EPIC 202843107 : A Close Eclipsing Binary Containing a {delta} Scuti Variable. (arXiv:1903.07846v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ou_J/0/1/0/all/0/1">Jian-Wen Ou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_M/0/1/0/all/0/1">Ming Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_J/0/1/0/all/0/1">Ji-Lin Zhou</a> This paper reports on the discovery that an eclipsing binary system, EPIC 202843107 , has a {delta} Scuti variable component. The phased light curve from Kepler space telescope presents a detached configuration. The binary modelling indicates that the two component stars have almost the same radius and may have experienced orbital circularization. Frequency analyses are performed for the residual light curve after subtracting the binary variations. The frequency spectrum reveals that one component star is a {delta} Scuti variable. A large frequencyRead More →

Stars from the GTSh10 catalogue in “Shajn’s plan”. (arXiv:1903.07871v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Gorbunov_M/0/1/0/all/0/1">M.A. Gorbunov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shlyapnikov_A/0/1/0/all/0/1">A.A. Shlyapnikov</a> We examined objects from the GTSh10 catalogue among the studied stars as a part of implementing the “Plan of Academician G.A. Shajn” (hereinafter – “Shajn’s Plan”) in order to replenish the database of photometric and spectral observations of red dwarfs. We consider the question concerning the cross-identification of data from the GTSh10 interactive version and the “Shajn’s Plan “catalogs, as well as the access to the archive of photographic observations. The article is illustrated with examples of working with the obtained list by means of the Virtual Observatory inRead More →

Core-Jet Blending Effects in Active Galactic Nuclei under the Korean VLBI Network View at 43 GHz. (arXiv:1903.07874v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Algaba_J/0/1/0/all/0/1">Juan-Carlos Algaba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hodgson_J/0/1/0/all/0/1">Jeffrey Hodgson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kang_S/0/1/0/all/0/1">Sin-Cheol Kang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_D/0/1/0/all/0/1">Dae-Won Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_J/0/1/0/all/0/1">Jae-Young Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_J/0/1/0/all/0/1">Jee Won Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_S/0/1/0/all/0/1">Sang-Sung Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trippe_S/0/1/0/all/0/1">Sascha Trippe</a> A long standing problem in the study of Active Galactic Nuclei (AGNs) is that the observed VLBI core is in fact a blending of the actual AGN core (classically defined by the $tau=1$ surface) and the upstream regions of the jet or optically thin emitting region flows. This blending may cause some biases towards the observables of the core, such as itsRead More →

Could an X-ray Flare after GRB 170817A Originate from a Post-merger Slim Accretion Disc?. (arXiv:1903.07878v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_Y/0/1/0/all/0/1">Yi-Qing Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dai_Z/0/1/0/all/0/1">Zi-Gao Dai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gu_W/0/1/0/all/0/1">Wei-Min Gu</a> GRB 170817A, detected by Fermi-GBM 1.7,s after the merger of a neutron star (NS) binary, provides the first direct evidence for a link between such a merger and a short-duration gamma-ray burst. The X-ray observations after GRB 170817A indicate a possible X-ray flare with a peak luminosity $L_{rm peak} sim 2times 10^{39},{rm erg,s}^{-1}$ near day 156. Here we show that this X-ray flare may be understood based on a slim disc around a compact object. On the one hand, thereRead More →

The galaxy luminosity function in the LAMOST Complete Spectroscopic Survey of Pointing Area at the Southern Galactic Cap. (arXiv:1903.07893v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhao_P/0/1/0/all/0/1">Pinsong Zhao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wu_H/0/1/0/all/0/1">Hong Wu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_C/0/1/0/all/0/1">C.K. Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_M/0/1/0/all/0/1">Ming Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_F/0/1/0/all/0/1">Fan Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_Y/0/1/0/all/0/1">Yinan Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lam_M/0/1/0/all/0/1">Man I Lam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jin_J/0/1/0/all/0/1">Junjie Jin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yuan_H/0/1/0/all/0/1">Hailong Yuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_H/0/1/0/all/0/1">Haotong Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shen_S/0/1/0/all/0/1">Shiyin Shen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shi_J/0/1/0/all/0/1">Jianrong Shi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luo_A/0/1/0/all/0/1">Ali Luo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wu_X/0/1/0/all/0/1">Xuebing Wu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhao_Y/0/1/0/all/0/1">Yongheng Zhao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jing_Y/0/1/0/all/0/1">Yipeng Jing</a> We present optical luminosity functions (LFs) of galaxies in the $^{0.1}g$, $^{0.1}r$, and $^{0.1}i$ bands, calculated using data in $sim 40$ $deg^{2}$ sky area of LAMOST Complete Spectroscopic Survey of Pointing Area (LaCoSSPAr) in Southern GalacticRead More →

Fermi-LAT Observations of Extreme Spectral Variability in IC 310. (arXiv:1903.07897v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Graham_J/0/1/0/all/0/1">Jamie Graham</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_A/0/1/0/all/0/1">Anthony Brown</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Chadwick_P/0/1/0/all/0/1">Paula Chadwick</a> (1) ((1) Durham University) We investigate the physical mechanisms of high-energy gamma-ray emission from the TeV-emitting misaligned active galactic nucleus IC 310. Eight years of data from the Fermi Large Area Telescope (Fermi-LAT) between 100 MeV and 500 GeV are reduced and analysed to study the temporal and spectral characteristics of IC 310. Point spread function-partitioned instrument response functions are used to improve the resolvability of IC 310 from nearby NGC 1275. Systematic effects due to this choice of instrument response functions andRead More →

Thermodynamics conditions of matter in neutron star mergers. (arXiv:1903.07898v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Perego_A/0/1/0/all/0/1">Albino Perego</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Bernuzzi_S/0/1/0/all/0/1">Sebastiano Bernuzzi</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Radice_D/0/1/0/all/0/1">David Radice</a> Matter in neutron star collisions can reach densities up to few times the nuclear saturation threshold and temperatures up to one hundred MeV. Understanding the structure and composition of such matter requires many-body nonperturbative calculations that are currently highly uncertain.Unique constraints on the neutron star matter are provided by gravitational-wave observations aided by numerical relativity simulations. In this work, we explore the thermodynamical conditions of matter and radiation along the merger dynamics. We consider 3 microphysical equation of state models and numerical relativity simulations including anRead More →

The Structure of a Quasi-Keplerian Accretion Disk around Magnetized Stars. (arXiv:1903.07907v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Habumugisha_I/0/1/0/all/0/1">Isaac Habumugisha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jurua_E/0/1/0/all/0/1">Edward Jurua</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tessema_S/0/1/0/all/0/1">Solomon B. Tessema</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simon_A/0/1/0/all/0/1">Anguma K. Simon</a> In this paper, we present the complete structure of a quasi-Keplerian thin accretion disk with an internal dynamo around a magnetized neutron star. We assume a full quasi-Keplerian disk with the azimuthal velocity deviating from the Keplerian fashion by a factor of $xi$ ($0Read More →

The role of an invariant IR cutoff in late time cosmological dynamics. (arXiv:1903.07934v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Nozari_K/0/1/0/all/0/1">Kourosh Nozari</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Dehghani_P/0/1/0/all/0/1">Parham Dehghani</a> We study the role of an invariant infra-red cutoff in the late time cosmological dynamics. This low energy cutoff originates from the existence of a minimal measurable uncertainty as a result of the curvature of background manifold, and can be encoded in an extended uncertainty relation. Inspired by black hole entropy-area relation, we extend the analysis to the thermodynamics of apparent horizon of the universe. By treating both the Newtonian and general relativistic cosmologies, we show that the contribution of infra-red cutoff in the equationsRead More →

Optimization of seismometer arrays for the cancellation of Newtonian noise from seismic body waves. (arXiv:1903.07936v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Harms_F/0/1/0/all/0/1">F. Badaracco J. Harms</a> Newtonian noise from seismic fields is predicted to become a sensitivity limiting noise contribution of the gravitational-wave detectors Advanced LIGO and Virgo in the next few years. It also plays a major role in the planning of next-generation detectors, which might be constructed underground, as planned for the Einstein Telescope, mostly to suppress Newtonian noise. Coherent noise cancellation using Wiener filters provides a way to mitigate Newtonian noise. So far, only the cancellation of Newtonian noise produced by seismic surface waves has been studiedRead More →

Probing the weak wind phenomenon in Galactic O-type giants. (arXiv:1903.07937v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Almeida_E/0/1/0/all/0/1">E. S. G. de Almeida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marcolino_W/0/1/0/all/0/1">W. L. F. Marcolino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouret_J/0/1/0/all/0/1">J.-C. Bouret</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pereira_C/0/1/0/all/0/1">C. B. Pereira</a> Analyses of Galactic late O dwarfs (O8-O9.5V stars) raised the `weak wind problem’: spectroscopic mass loss rates ($dot{M}$) are up to two orders of magnitude lower than the theoretical values. We investigated the stellar and wind properties of Galactic late O giants (O8-O9.5III stars). We performed a spectroscopic analysis of nine O8-O9.5III stars in the ultraviolet (UV) and optical regions using the model atmosphere code CMFGEN. From the UV region, we found $dot{M}$ $sim$ $10^{-8}-10^{-9}$ $mathrm{M_odot}$Read More →

Stellar Spectra Classification and Feature evaluation Based on Random Forest. (arXiv:1903.07939v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Li_X/0/1/0/all/0/1">Xiangru Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_Y/0/1/0/all/0/1">Yangtao Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qiu_K/0/1/0/all/0/1">Kaibin Qiu</a> With the availability of multi-object spectrometers and the designing & running of some large scale sky surveys, we are obtaining massive spectra. Therefore, it becomes more and more important to deal with the massive spectral data efficiently and accurately. This work investigated the classification problem of stellar spectra under the assumption that there is no perfect absolute flux calibration, for example, the spectra from Guoshoujing Telescope (the Large Sky Area Multi-Object Fiber Spectroscopic Telescope, LAMOST). The proposed scheme consists of the following two procedures:Read More →

The Galactic Faraday depth sky revisited. (arXiv:1903.06735v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hutschenreuter_S/0/1/0/all/0/1">Sebastian Hutschenreuter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ensslin_T/0/1/0/all/0/1">Torsten A. En&#xdf;lin</a> The Galactic Faraday depth sky is a tracer for both the Galactic magnetic field and the thermal electron distribution. It has been previously reconstructed from polarimetric measurements of extra-galactic point sources. Here, we improve on these works by using an updated inference algorithm as well as by taking into account the free-free emission measure map from the Planck survey. In the future, the data situation will improve drastically with the next generation Faraday rotation measurements from SKA and its pathfinders. Anticipating this, the aim of this paper is to updateRead More →

On the properties of the massive binary black hole merger GW170729. (arXiv:1903.06742v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Chatziioannou_K/0/1/0/all/0/1">Katerina Chatziioannou</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Cotesta_R/0/1/0/all/0/1">Roberto Cotesta</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Ghonge_S/0/1/0/all/0/1">Sudarshan Ghonge</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Lange_J/0/1/0/all/0/1">Jacob Lange</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Ng_K/0/1/0/all/0/1">Ken K.-Y. Ng</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Bustillo_J/0/1/0/all/0/1">Juan Calderon Bustillo</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Clark_J/0/1/0/all/0/1">James Clark</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Haster_C/0/1/0/all/0/1">Carl-Johan Haster</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Khan_S/0/1/0/all/0/1">Sebastian Khan</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Puerrer_M/0/1/0/all/0/1">Michael Puerrer</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Raymond_V/0/1/0/all/0/1">Vivien Raymond</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Vitale_S/0/1/0/all/0/1">Salvatore Vitale</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Afshari_N/0/1/0/all/0/1">Nousha Afshari</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Babak_S/0/1/0/all/0/1">Stanislav Babak</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Barkett_K/0/1/0/all/0/1">Kevin Barkett</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Blackman_J/0/1/0/all/0/1">Jonathan Blackman</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Bohe_A/0/1/0/all/0/1">Alejandro Bohe</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Boyle_M/0/1/0/all/0/1">Michael Boyle</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Buonanno_A/0/1/0/all/0/1">Alessandra Buonanno</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Campanelli_M/0/1/0/all/0/1">Manuela Campanelli</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Carullo_G/0/1/0/all/0/1">Gregorio Carullo</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Chu_T/0/1/0/all/0/1">Tony Chu</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Flynn_E/0/1/0/all/0/1">Eric Flynn</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Fong_H/0/1/0/all/0/1">Heather Fong</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Garcia_A/0/1/0/all/0/1">Alyssa Garcia</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Giesler_M/0/1/0/all/0/1">Matthew Giesler</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Haney_M/0/1/0/all/0/1">Maria Haney</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Hannam_M/0/1/0/all/0/1">Mark Hannam</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Harry_I/0/1/0/all/0/1">Ian Harry</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Healy_J/0/1/0/all/0/1">James Healy</a>,Read More →

Variability in X-ray line ratios in helium-like ions of massive stars: the wind-driven case. (arXiv:1903.06745v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ignace_R/0/1/0/all/0/1">R. Ignace</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Damrau_Z/0/1/0/all/0/1">Z. Damrau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hole_K/0/1/0/all/0/1">K. T. Hole</a> High spectral resolution and long exposure times are providing unprecedented levels of data quality of massive stars at X-ray wavelengths. A key diagnostic of the X-ray emitting plasma are the fir lines for He-like triplets. In particular, owing to radiative pumping effects, the forbidden-to-intercombination line luminosity ratio, R=f/i, can be used to determine the proximity of the hot plasma to the UV-bright photospheres of massive stars. Moreover, the era of large observing programs additionally allows for investigation of lineRead More →

Effect of Different Angular Momentum Transport mechanisms on the Distribution of Water in Protoplanetary Disks. (arXiv:1903.06746v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kalyaan_A/0/1/0/all/0/1">Anusha Kalyaan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desch_S/0/1/0/all/0/1">Steven J. Desch</a> The snow line in a protoplanetary disk demarcates regions with H$_2$O ice from regions with H$_2$O vapor. Where a planet forms relative to this location determines how much water and other volatiles it forms with. Giant planet formation may be triggered at the water snow line if vapor diffuses outward and is cold-trapped beyond the snow line faster than icy particles can drift inward. In this study we investigate the distribution of water across the snow line, considering three different radialRead More →

The physics and astrophysics of X-ray outflows from Active Galactic Nuclei. (arXiv:1903.06748v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Laha_S/0/1/0/all/0/1">Sibasish Laha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_R/0/1/0/all/0/1">Randall Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tzanavaris_P/0/1/0/all/0/1">Panayiotis Tzanavaris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kallman_T/0/1/0/all/0/1">Tim Kallman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Veilleux_S/0/1/0/all/0/1">Sylvain Veilleux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tombesi_F/0/1/0/all/0/1">Francesco Tombesi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kriss_G/0/1/0/all/0/1">Gerard Kriss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guainazzi_M/0/1/0/all/0/1">Matteo Guainazzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaspari_M/0/1/0/all/0/1">Massimo Gaspari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaastra_J/0/1/0/all/0/1">Jelle Kaastra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Markowitz_A/0/1/0/all/0/1">Alex Markowitz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crenshaw_M/0/1/0/all/0/1">Mike Crenshaw</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Behar_E/0/1/0/all/0/1">Ehud Behar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fukumura_K/0/1/0/all/0/1">Keigo Fukumura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Longinotti_A/0/1/0/all/0/1">Anna Lia Longinotti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rozanska_A/0/1/0/all/0/1">Agata Rozanska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ebrero_J/0/1/0/all/0/1">Jacobo Ebrero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferland_G/0/1/0/all/0/1">Gary Ferland</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricci_C/0/1/0/all/0/1">Claudio Ricci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Done_C/0/1/0/all/0/1">Chris Done</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Proga_D/0/1/0/all/0/1">Daniel Proga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Revalski_M/0/1/0/all/0/1">Mitchell Revalski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vayner_A/0/1/0/all/0/1">Andrey Vayner</a> The highly energetic outflows from Active Galactic Nuclei detected in X-rays are one of the most powerful mechanisms by which the centralRead More →