RAS_WEB (Page 3,813)

Correlation between the ionizing continuum and variable C iv broad absorption line in multi-epoch observations of SDSS J141007.74+541203.3. (arXiv:1905.02407v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_H/0/1/0/all/0/1">Hong-Yan Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pan_C/0/1/0/all/0/1">Cai-Juan Pan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lu_W/0/1/0/all/0/1">Wei-Jian Lu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qin_Y/0/1/0/all/0/1">Yi-Ping Qin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_Y/0/1/0/all/0/1">Ying-Ru Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_W/0/1/0/all/0/1">Wei-Rong Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_Y/0/1/0/all/0/1">Yu-Tao Zhou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yao_M/0/1/0/all/0/1">Min Yao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nong_W/0/1/0/all/0/1">Wei-Jing Nong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lu_M/0/1/0/all/0/1">Mei-Mei Lu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yao_Z/0/1/0/all/0/1">Zhi-Kao Yao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Han_Q/0/1/0/all/0/1">Qing-Lin Han</a> Correlation between the variations of quasar absorption lines and the ionizing continuum have been recently confirmed in systematic studies. However, no convincing individual case is reported. We present a statistical analysis of the variable C iv broad absorption line (BAL) in the quasar SDSS J141007.74+541203.3, which have been observedRead More →

Differences in Faraday Rotation Between Adjacent Extragalactic Radio Sources as a Probe of Cosmic Magnetic Fields. (arXiv:1905.02410v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Vernstrom_T/0/1/0/all/0/1">T. Vernstrom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaensler_B/0/1/0/all/0/1">B. Gaensler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rudnick_L/0/1/0/all/0/1">L. Rudnick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andernach_H/0/1/0/all/0/1">H. Andernach</a> Faraday rotation measures (RMs) of extragalactic radio sources provide information on line-of-sight magnetic fields, including contributions from our Galaxy, source environments, and the intergalactic medium (IGM). Looking at differences in RMs, $Delta$RM, between adjacent sources on the sky can help isolate these different components. In this work, we classify adjacent polarized sources in the NVSS as random or physical pairs. We recompute and correct the uncertainties in the NVSS RM catalog, since these were significantlyRead More →

The UTMOST Survey for Magnetars, Intermittent pulsars, RRATs and FRBs I: System description and overview. (arXiv:1905.02415v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Krishnan_V/0/1/0/all/0/1">V. Venkatraman Krishnan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flynn_C/0/1/0/all/0/1">C. Flynn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Farah_W/0/1/0/all/0/1">W. Farah</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jameson_A/0/1/0/all/0/1">A. Jameson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bailes_M/0/1/0/all/0/1">M. Bailes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oslowski_S/0/1/0/all/0/1">S. Os&#x142;owski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bateman_T/0/1/0/all/0/1">T. Bateman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gupta_V/0/1/0/all/0/1">V. Gupta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Straten_W/0/1/0/all/0/1">W. van Straten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keane_E/0/1/0/all/0/1">E. F. Keane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barr_E/0/1/0/all/0/1">E. D. Barr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhandari_S/0/1/0/all/0/1">S. Bhandari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caleb_M/0/1/0/all/0/1">M. Caleb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Campbell_Wilson_D/0/1/0/all/0/1">D. Campbell-Wilson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Day_C/0/1/0/all/0/1">C. K. Day</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deller_A/0/1/0/all/0/1">A. Deller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Green_A/0/1/0/all/0/1">A. J. Green</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hunstead_R/0/1/0/all/0/1">R. Hunstead</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jankowski_F/0/1/0/all/0/1">F. Jankowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lower_M/0/1/0/all/0/1">M. E. Lower</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parthasarathy_A/0/1/0/all/0/1">A. Parthasarathy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Plant_K/0/1/0/all/0/1">K. Plant</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Price_D/0/1/0/all/0/1">D. C. Price</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosado_P/0/1/0/all/0/1">P. A. Rosado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Temby_D/0/1/0/all/0/1">D. Temby</a> We describe the ongoingRead More →

Accretion and photodesorption of CO ice as a function of the incident angle of deposition. (arXiv:1905.02426v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Diaz_C/0/1/0/all/0/1">C Gonz&#xe1;lez D&#xed;az</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lucas_H/0/1/0/all/0/1">H Carrascosa de Lucas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aparicio_S/0/1/0/all/0/1">S Aparicio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caro_G/0/1/0/all/0/1">G M Mu&#xf1;oz Caro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sie_N/0/1/0/all/0/1">N-E Sie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hsiao_L/0/1/0/all/0/1">L-C Hsiao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Y/0/1/0/all/0/1">Y-J Chen</a> Non-thermal desorption of inter- and circum-stellar ice mantles on dust grains, in particular ultraviolet photon-induced desorption, has gained importance in recent years. These processes may account for the observed gas phase abundances of molecules like CO toward cold interstellar clouds. Ice mantle growth results from gas molecules impinging on the dust from all directions and incidence angles. Nevertheless, the effect of theRead More →

How bright are fast optical bursts associated with fast radio bursts?. (arXiv:1905.02429v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_Y/0/1/0/all/0/1">Yuan-Pei Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_B/0/1/0/all/0/1">Bing Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wei_J/0/1/0/all/0/1">Jian-Yan Wei</a> The origin of fast radio bursts (FRBs) is still unknown. Multi-wavelength observations during or shortly after the FRB phase would be essential to identify the counterpart of an FRB and to constrain its progenitor and environment. In this work, we investigate the brightness of the “fast optical bursts” (FOBs) associated with FRBs and the prospects of detecting them. We investigate several inverse Compton (IC) scattering processes that might produce an FOB, including both the one-zone and two-zone models. We also investigate the extensionRead More →

RadioAstron probes the ultra-fine spatial structure in the H$_2$O maser emission in the star forming region W49N. (arXiv:1905.02440v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Shakhvorostova_N/0/1/0/all/0/1">N.N. Shakhvorostova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sobolev_A/0/1/0/all/0/1">A.M. Sobolev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moran_J/0/1/0/all/0/1">J.M. Moran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alakoz_A/0/1/0/all/0/1">A.V. Alakoz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Imai_H/0/1/0/all/0/1">H. Imai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avdeev_V/0/1/0/all/0/1">V.Y. Avdeev</a> H$_2$O maser emission associated with the massive star formation region W49N were observed with the Space-VLBI mission RadioAstron. The procedure for processing of the maser spectral line data obtained in the RadioAstron observations is described. Ultra-fine spatial structures in the maser emission were detected on space-ground baselines of up to 9.6 Earth diameters. The correlated flux densities of these features range from 0.1% to 0.6% of the totalRead More →

Revisiting Ryskin’s Model of Cosmic Acceleration. (arXiv:1905.02441v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_Z/0/1/0/all/0/1">Zhiqi Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gao_H/0/1/0/all/0/1">Han Gao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_H/0/1/0/all/0/1">Haoting Xu</a> Cosmic backreaction as an additional source of the expansion of the universe has been a debate topic since the discovery of cosmic acceleration. The major concern is whether the self interaction of small-scale nonlinear structures would source gravity on very large scales. Gregory Ryskin argued against the additional inclusion of gravitational interaction energy of astronomical objects, whose masses are mostly inferred from gravitational effects and hence should already contain all sources with long-range gravity forces. Ryskin proposed that the backreaction contribution to the energy momentum tensor is insteadRead More →

Photometry, spectroscopy, and polarimetry of distant comet C/2014 A4 (SONEAR). (arXiv:1905.02465v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ivanova_O/0/1/0/all/0/1">Oleksandra Ivanova</a> (1 and 2 and 3), <a href="http://arxiv.org/find/astro-ph/1/au:+Lukyanyk_I/0/1/0/all/0/1">Igor Luk&#x27;yanyk</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Kolokolova_L/0/1/0/all/0/1">Ludmilla Kolokolova</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Das_H/0/1/0/all/0/1">Himadri Sekhar Das</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Husarik_M/0/1/0/all/0/1">Marek Hus&#xe1;rik</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Rosenbush_V/0/1/0/all/0/1">Vera Rosenbush</a> (2 and 3), <a href="http://arxiv.org/find/astro-ph/1/au:+Afanasiev_V/0/1/0/all/0/1">Viktor Afanasiev</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Svoren_J/0/1/0/all/0/1">J&#xe1;n Svore&#x148;</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Kiselev_N/0/1/0/all/0/1">Nikolai Kiselev</a> (2 and 7), <a href="http://arxiv.org/find/astro-ph/1/au:+Krushinsky_V/0/1/0/all/0/1">Vadim Krushinsky</a> (8) ((1) Astronomical Institute of the Slovak Academy of Sciences, (2) Main Astronomical Observatory of the National Academy of Sciences, (3) Astronomical Observatory, Taras Shevchenko National University of Kyiv, (4) University of Maryland, (5) Department of Physics, (6) Special Astrophysical Observatory, (7) Crimean Astrophysical Observatory,Read More →

Revealing the nature of central emission nebulae in the dwarf elliptical galaxy NGC 185. (arXiv:1905.02468v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Vucetic_M/0/1/0/all/0/1">M. M. Vu&#x10d;eti&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ilic_D/0/1/0/all/0/1">D. Ili&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Egorov_O/0/1/0/all/0/1">O. V. Egorov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moiseev_A/0/1/0/all/0/1">A. Moiseev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Onic_D/0/1/0/all/0/1">D. Oni&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pannuti_T/0/1/0/all/0/1">T. G. Pannuti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arbutina_B/0/1/0/all/0/1">B. Arbutina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petrov_N/0/1/0/all/0/1">N. Petrov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Urosevic_D/0/1/0/all/0/1">D. Uro&#x161;evi&#x107;</a> In this paper we present new optical observations of NGC 185 galaxy that are intended to reveal the status of supernova remnants (SNRs) in this dwarf elliptical companion of Andromeda galaxy. Previously, it was reported that this galaxy hosts one SNR. Our deep photometric study with the 2-m telescope at Rozhen National Astronomical Observatory using narrow-band H$alpha$ and [SII]Read More →

High Energy Emission and its Variability in Young Stellar Objects. (arXiv:1905.02471v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Argiroffi_C/0/1/0/all/0/1">Costanza Argiroffi</a> Young stars show a variety of highly energetic phenomena, from accretion and outflow processes to hot coronal plasmas confined in their outer atmosphere, all regulated by the intense stellar magnetic fields. Many aspects on each of these phenomena are debated, but, most notably, their complex mutual interaction remains obscure. In this work I report how these phenomena are simultaneously responsible for the high-energy emission from young stars, with a special focus on the expected and observed variability in the X-ray band. Investigating variations in the X-ray emission from young starsRead More →

Twin CME Launched by a Blowout Jet Originated from the Eruption of a Quiet-Sun Mini-filament. (arXiv:1905.02475v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Solanki_R/0/1/0/all/0/1">Ritika Solanki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Srivastava_A/0/1/0/all/0/1">Abhishek K. Srivastava</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rao_Y/0/1/0/all/0/1">Yamini K. Rao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dwivedi_B/0/1/0/all/0/1">Bhola N. Dwivedi</a> We study a quiet-Sun blowout jet which is observed on 2014 May 16 by the instruments on board Solar Dynamics Observatory (SDO). We find the twin CME as jet-like and bubble-like CME simultaneously as observed by LASCO C2 on board Solar and Heliospheric Observatory (SoHO), Solar Terrestrial Relation Observatory (STEREO A and STEREO B/COR2). They are respectively associated with the eruption of the northern and southern sections of the filament. A circular filamentRead More →

Lyman Radiation Hydrodynamics of Turbulent H II Regions in Molecular Clouds: A Physical Origin of LyC Leakage and the Associated Ly$alpha$ Spectra. (arXiv:1905.02480v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kakiichi_K/0/1/0/all/0/1">Koki Kakiichi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gronke_M/0/1/0/all/0/1">Max Gronke</a> We examine Lyman continuum (LyC) leakage through H II regions regulated by turbulence and radiative feedback in a giant molecular cloud in the context of fully-coupled radiation hydrodynamics (RHD). The physical relations of the LyC escape with H I covering fraction, kinematics, spectral hardness, and the emergent Lyman-$alpha$ (Ly$alpha$) line profiles are studied using a series of RHD turbulence simulations performed with RAMSES-RT. The turbulence-regulated mechanism allows ionizing photons to leak out at early timesRead More →

Efficient, Divergence-Free, High Order MHD on 3D Spherical Meshes with Optimal Geodesic Meshing. (arXiv:1905.02504v1 [physics.comp-ph]) <a href="http://arxiv.org/find/physics/1/au:+Balsara_D/0/1/0/all/0/1">Dinshaw S. Balsara</a>, <a href="http://arxiv.org/find/physics/1/au:+Florinski_V/0/1/0/all/0/1">Vladimir Florinski</a>, <a href="http://arxiv.org/find/physics/1/au:+Garain_S/0/1/0/all/0/1">Sudip Garain</a>, <a href="http://arxiv.org/find/physics/1/au:+Subramanian_S/0/1/0/all/0/1">Sethupathy Subramanian</a>, <a href="http://arxiv.org/find/physics/1/au:+Gurski_K/0/1/0/all/0/1">Katharine F. Gurski</a> There is a great need in several areas of astrophysics and space-physics to carry out high order of accuracy, divergence-free MHD simulations on spherical meshes. This requires us to pay careful attention to the interplay between mesh quality and numerical algorithms. Methods have been designed that fundamentally integrate high order isoparametric mappings with the other high accuracy algorithms that are needed for divergence-free MHD simulations on geodesic meshes. The goal of this paperRead More →

Constraining coherent low frequency radio flares from compact binary mergers. (arXiv:1905.02509v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Rowlinson_A/0/1/0/all/0/1">A. Rowlinson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_G/0/1/0/all/0/1">G.E. Anderson</a> The presence and detectability of coherent radio emission from compact binary mergers (containing at least one neutron star) remains poorly constrained due to large uncertainties in the models. These compact binary mergers may initially be detected by a Short Gamma-ray Burst (SGRB) or via their gravitational wave emission. Several radio facilities have developed rapid response modes enabling them to trigger on these events and search for this emission. This paper uses the current deepest constraints on this emission, for GRB 150424A from the Murchison Widefield Array. FollowingRead More →

Mapping the structural diversity of C60 carbon clusters and their infrared spectra. (arXiv:1905.02550v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Dubosq_C/0/1/0/all/0/1">C. Dubosq</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Falvo_C/0/1/0/all/0/1">C. Falvo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calvo_F/0/1/0/all/0/1">F. Calvo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rapacioli_M/0/1/0/all/0/1">M. Rapacioli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parneix_P/0/1/0/all/0/1">P. Parneix</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pino_T/0/1/0/all/0/1">T. Pino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simon_A/0/1/0/all/0/1">A. Simon</a> The current debate about the nature of the carbonaceous material carrying the infrared (IR) emission spectra of planetary and proto-planetary nebulae, including the broad plateaus, calls for further studies on the interplay between structure and spectroscopy of carbon-based compounds of astrophysical interest. The recent observation of C60 buckminsterfullerene in space suggests that carbon clusters of similar size may also be relevant. In the present work, broad statistical samples of C60Read More →

Testing the Swampland: $H_0$ tension. (arXiv:1905.02555v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Colgain_E/0/1/0/all/0/1">Eoin &#xd3; Colg&#xe1;in</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yavartanoo_H/0/1/0/all/0/1">Hossein Yavartanoo</a> The de Sitter Swampland conjecture compels us to consider dark energy models where $lambda(phi) equiv |nabla_{phi} V|/V$ is bounded below by a positive constant. Moreover, it has been argued for Quintessence models that the constant $lambda$ scenario is the least constrained. Here we demonstrate that increasing $lambda$ only exacerbates existing tension in the Hubble constant $H_0$. The identification of dark energy models that both evade observational bounds and alleviate $H_0$ tension constitutes a robust test for the Swampland program. The de Sitter Swampland conjecture compels us to consider dark energy modelsRead More →

Detectability of atmospheric features of Earth-like planets in the habitable zone around M dwarfs. (arXiv:1905.02560v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Wunderlich_F/0/1/0/all/0/1">F. Wunderlich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Godolt_M/0/1/0/all/0/1">M. Godolt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grenfell_J/0/1/0/all/0/1">J.L. Grenfell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stadt_S/0/1/0/all/0/1">S. St&#xe4;dt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_A/0/1/0/all/0/1">A.M.S. Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gebauer_S/0/1/0/all/0/1">S. Gebauer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schreier_F/0/1/0/all/0/1">F. Schreier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hedelt_P/0/1/0/all/0/1">P. Hedelt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rauer_H/0/1/0/all/0/1">H. Rauer</a> We investigate the detectability of atmospheric spectral features of Earth-like planets in the habitable zone (HZ) around M dwarfs with the future James Webb Space Telescope (JWST). We use a coupled 1D climate-chemistry-model to simulate the influence of a range of observed and modelled M-dwarf spectra on Earth-like planets. The simulated atmospheres served as input for the calculation of the transmission spectraRead More →

Is helium the key parameter in the extended color spread of the first generation stars in M3?. (arXiv:1905.02584v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Tailo_M/0/1/0/all/0/1">M. Tailo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAntona_F/0/1/0/all/0/1">F. D&#x27;Antona</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caloi_V/0/1/0/all/0/1">V. Caloi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milone_A/0/1/0/all/0/1">A. P. Milone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marino_A/0/1/0/all/0/1">A. F. Marino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lagioia_E/0/1/0/all/0/1">E. Lagioia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cordoni_G/0/1/0/all/0/1">G. Cordoni</a> The study of the “chromosome maps” of Galactic Globular Clusters has shown that the stars identified as `first generation’ often define an extended sequence in the $m_{F275W}-m_{F814W}$ colour, whose straightforward interpretation, by comparison with synthetic spectra, is that they are inhomogeneous in helium content. The cluster M 3 (NGC 5272) is one of the most prominent example of this phenomenon, since its firstRead More →

NGTS-5b: a highly inflated planet offering insights into the sub-Jovian desert. (arXiv:1905.02593v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Eigmuller_P/0/1/0/all/0/1">Philipp Eigm&#xfc;ller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chaushev_A/0/1/0/all/0/1">Alexander Chaushev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gillen_E/0/1/0/all/0/1">Edward Gillen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_A/0/1/0/all/0/1">Alexis Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nielsen_L/0/1/0/all/0/1">Louise D. Nielsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Turner_O/0/1/0/all/0/1">Oliver Turner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Czismadia_S/0/1/0/all/0/1">Szilard Czismadia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smalley_B/0/1/0/all/0/1">Barry Smalley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bayliss_D/0/1/0/all/0/1">Daniel Bayliss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belardi_C/0/1/0/all/0/1">Claudia Belardi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouchy_F/0/1/0/all/0/1">Fran&#xe7;ois Bouchy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burleigh_M/0/1/0/all/0/1">Matthew R. Burleigh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cabrera_J/0/1/0/all/0/1">Juan Cabrera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Casewell_S/0/1/0/all/0/1">Sarah L. Casewell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chazelas_B/0/1/0/all/0/1">Bruno Chazelas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cooke_B/0/1/0/all/0/1">Benjamin F. Cooke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Erikson_A/0/1/0/all/0/1">Anders Erikson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gansicke_B/0/1/0/all/0/1">Boris T. G&#xe4;nsicke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gunther_M/0/1/0/all/0/1">Maximilian N. G&#xfc;nther</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goad_M/0/1/0/all/0/1">Michael R. Goad</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grange_A/0/1/0/all/0/1">Andrew Grange</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jackman_J/0/1/0/all/0/1">James A. G. Jackman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jenkins_J/0/1/0/all/0/1">James S. Jenkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McCormac_J/0/1/0/all/0/1">James McCormac</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moyano_M/0/1/0/all/0/1">Maximiliano Moyano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pollacco_D/0/1/0/all/0/1">Don Pollacco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poppenhaeger_K/0/1/0/all/0/1">Katja Poppenhaeger</a>, <aRead More →

Application of the electromotive force as a shock front indicator in the inner heliosphere. (arXiv:1905.02596v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hofer_B/0/1/0/all/0/1">Bernhard Hofer</a> (1,2), <a href="http://arxiv.org/find/astro-ph/1/au:+Bourdin_P/0/1/0/all/0/1">Philippe-A. Bourdin</a> (1) ((1) Space Research Institute, Austrian Academy of Sciences, Graz/Austria, (2) Max-Planck-Institut f&#xfc;r Sonnensystemforschung, G&#xf6;ttingen/Germany) The electromotive force (EMF) describes how the evolution and generation of a large-scale magnetic field is influenced by small-scale turbulence. Recent studies of in-situ measurements have shown a significant peak in the EMF while a coronal mass ejection (CME) shock front passes by the spacecraft. The goal of this study is to use the EMF as an indicator for the arrival of CME shock fronts. With HeliosRead More →