RAS_WEB (Page 4,428)

The Long Night: Modeling the Climate of Westeros. (arXiv:1903.12195v1 [physics.pop-ph]) <a href="http://arxiv.org/find/physics/1/au:+Paradise_A/0/1/0/all/0/1">Adiv Paradise</a>, <a href="http://arxiv.org/find/physics/1/au:+Obertas_A/0/1/0/all/0/1">Alysa Obertas</a>, <a href="http://arxiv.org/find/physics/1/au:+OGrady_A/0/1/0/all/0/1">Anna O&#x27;Grady</a>, <a href="http://arxiv.org/find/physics/1/au:+Young_M/0/1/0/all/0/1">Matthew Young</a> Many previous authors have attempted to find explanations for Westeros’s climate, characterized by a generally moderate, Earth-like climate punctuated by extremely long and cold winters, separated by thousands of years. One explanation that has been proposed is that the planet orbits in a Sitnikov configuration, where two equal-mass stars (or a star and a black hole) orbit each other on slightly eccentric orbits, and the planet moves along a line through the barycenter perpendicular to the primaries’ orbital plane (Freistetter & Gr”utzbauch 2018).Read More →

Evidence for rapid disk formation and reprocessing in the X-ray bright tidal disruption event AT 2018fyk. (arXiv:1903.12203v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Wevers_T/0/1/0/all/0/1">T. Wevers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pasham_D/0/1/0/all/0/1">D. R. Pasham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Velzen_S/0/1/0/all/0/1">S. van Velzen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leloudas_G/0/1/0/all/0/1">G. Leloudas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schulze_S/0/1/0/all/0/1">S. Schulze</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_Jones_J/0/1/0/all/0/1">J. C. A. Miller-Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jonker_P/0/1/0/all/0/1">P. G. Jonker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gromadzki_M/0/1/0/all/0/1">M. Gromadzki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kankare_E/0/1/0/all/0/1">E. Kankare</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hodgkin_S/0/1/0/all/0/1">S. T. Hodgkin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wyrzykowski_L/0/1/0/all/0/1">L .Wyrzykowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kostrzewa_Rutkowska_Z/0/1/0/all/0/1">Z.Kostrzewa-Rutkowska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moran_S/0/1/0/all/0/1">S.Moran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berton_M/0/1/0/all/0/1">M.Berton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maguire_K/0/1/0/all/0/1">K. Maguire</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Onori_F/0/1/0/all/0/1">F. Onori</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matilla_S/0/1/0/all/0/1">S. Matilla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nicholl_M/0/1/0/all/0/1">M. Nicholl</a> We present optical spectroscopic and Swift UVOT/XRT observations of the X-ray and UV/optical bright tidal disruption event (TDE) AT 2018fyk/ASASSN-18ul discovered by ASAS-SN. The Swift lightcurve is atypical for aRead More →

Radio continuum size evolution of star-forming galaxies over 0.35 < z < 2.25. (arXiv:1903.12217v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Jimenez_Andrade_E/0/1/0/all/0/1">E.F. Jim&#xe9;nez-Andrade</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Magnelli_B/0/1/0/all/0/1">B. Magnelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karim_A/0/1/0/all/0/1">A. Karim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zamorani_G/0/1/0/all/0/1">G. Zamorani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bondi_M/0/1/0/all/0/1">M. Bondi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schinnerer_E/0/1/0/all/0/1">E. Schinnerer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sargent_M/0/1/0/all/0/1">M. Sargent</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romano_Diaz_E/0/1/0/all/0/1">E. Romano-D&#xed;az</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Novak_M/0/1/0/all/0/1">M. Novak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lang_P/0/1/0/all/0/1">P. Lang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertoldi_F/0/1/0/all/0/1">F. Bertoldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vardoulaki_E/0/1/0/all/0/1">E. Vardoulaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Toft_S/0/1/0/all/0/1">S. Toft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smolcic_V/0/1/0/all/0/1">V. Smol&#x10d;i&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harrington_K/0/1/0/all/0/1">K. Harrington</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leslie_S/0/1/0/all/0/1">S. Leslie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delhaize_J/0/1/0/all/0/1">J. Delhaize</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_D/0/1/0/all/0/1">D. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karoumpis_C/0/1/0/all/0/1">C. Karoumpis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kartaltepe_J/0/1/0/all/0/1">J. Kartaltepe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koekemoer_A/0/1/0/all/0/1">A.M. Koekemoer</a> We present the first systematic study of the radio continuum size evolution of star-forming galaxies (SFGs) over the redshift range $0.35Read More →

A Radiative Heating Model for Chondrule and Chondrite Formation. (arXiv:1903.12224v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Herbst_W/0/1/0/all/0/1">William Herbst</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Greenwood_J/0/1/0/all/0/1">James P. Greenwood</a> We propose that chondrules and chondrites formed together during a brief radiative heating event caused by the close encounter of a small (m to km-scale), primitive planetesimal (SPP) with incandescent lava on the surface of a large (100 km-scale) differentiated planetesimal (LDP). In our scenario, chondrite lithification occurs by hot isostatic pressing (HIP) simultaneously with chondrule formation, in accordance with the constraints of complementarity and cluster chondrites. Thermal models of LDPs formed near t=0 predict that there will be a very narrow window of time, coincident withRead More →

Ultra-heavy cosmic-ray science–Are r-process nuclei in the cosmic rays produced in supernovae or binary neutron star mergers?. (arXiv:1903.12228v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Binns_W/0/1/0/all/0/1">W.R. Binns</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Israel_M/0/1/0/all/0/1">M.H. Israel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rauch_B/0/1/0/all/0/1">B.F. Rauch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cummings_A/0/1/0/all/0/1">A.C. Cummings</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davis_A/0/1/0/all/0/1">A.J. Davis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Labrador_A/0/1/0/all/0/1">A.W. Labrador</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leske_R/0/1/0/all/0/1">R.A. Leske</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mewaldt_R/0/1/0/all/0/1">R.A Mewaldt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stone_E/0/1/0/all/0/1">E.C. Stone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wiedenbeck_M/0/1/0/all/0/1">M.E. Wiedenbeck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brandt_T/0/1/0/all/0/1">T.J. Brandt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Christian_E/0/1/0/all/0/1">E.R. Christian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Link_J/0/1/0/all/0/1">J.T. Link</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mitchell_J/0/1/0/all/0/1">J.W. Mitchell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nolfo_G/0/1/0/all/0/1">G.A. de Nolfo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosenvinge_T/0/1/0/all/0/1">T.T. von Rosenvinge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sakai_K/0/1/0/all/0/1">K. Sakai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sasaki_M/0/1/0/all/0/1">M. Sasaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Waddington_C/0/1/0/all/0/1">C.J. Waddington</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Janka_H/0/1/0/all/0/1">H.T. Janka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melott_A/0/1/0/all/0/1">A.L. Melott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mason_G/0/1/0/all/0/1">G.M. Mason</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seo_E/0/1/0/all/0/1">E-S. Seo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adams_J/0/1/0/all/0/1">J.H. Adams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thielemann_F/0/1/0/all/0/1">F-K. Thielemann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heger_A/0/1/0/all/0/1">A. Heger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lugaro_M/0/1/0/all/0/1">M. Lugaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Westphal_A/0/1/0/all/0/1">A.J. Westphal</a>Read More →

Comparison between the influence of outflows and supermassive binary black holes in active galactic nuclei on the polarization angle profiles. (arXiv:1903.12250v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Savic_%7B/0/1/0/all/0/1">&#x110;or&#x111;e Savi&#x107;</a> Optical polarization signal coming from the innermost part of active galactic nuclei (AGNs) is highly sensitive on the geometry and kinematics of the central engine. Due to the compact size of the AGN central region, which is spatially unresolved with current observing facilities, we rely on spectropolarimetry which can provide us insight in their hidden physics. We model equatorial scattering for various broad line region (BLR) configurations using radiative transfer code STOKES. We analyze the polarization position angle () profilesRead More →

Baryon density extraction and isotropy analysis of Cosmic Microwave Background using a multilayer perceptron. (arXiv:1903.12253v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mishra_A/0/1/0/all/0/1">Amit Mishra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reddy_P/0/1/0/all/0/1">Pranath Reddy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nigam_R/0/1/0/all/0/1">Rahul Nigam</a> The discovery of cosmic microwave background (CMB) was a paradigm shift in the study and fundamental understanding of the early universe and also the Big Bang phenomenon. Cosmic microwave background is one of the richest and intriguing sources of information available to cosmologists. Although there are some well established statistical methods for the analysis of CMB, here we explore the use of deep learning in this respect. We correlate the baryon density obtained from the power spectrum of CMB temperatureRead More →

Probing the protosolar disk using dust filtering at gaps in the early Solar System. (arXiv:1903.12274v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Haugbolle_T/0/1/0/all/0/1">Troels Haugb&#xf8;lle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weber_P/0/1/0/all/0/1">Philipp Weber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wielandt_D/0/1/0/all/0/1">Daniel P. Wielandt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benitez_Llambay_P/0/1/0/all/0/1">Pablo Ben&#xed;tez-Llambay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bizzarro_M/0/1/0/all/0/1">Martin Bizzarro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gressel_O/0/1/0/all/0/1">Oliver Gressel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pessah_M/0/1/0/all/0/1">Martin E. Pessah</a> Jupiter and Saturn formed early, before the gas disk dispersed. The presence of gap-opening planets affects the dynamics of the gas and embedded solids, and halts the inward drift of grains above a certain size. A drift barrier can explain the absence of calcium-aluminium-rich inclusions (CAIs) in chondrites originating from parent bodies that accreted in the inner Solar System. Employing an interdisciplinary approach, we use aRead More →

Comparative analysis of solar radio bursts before and during CME propagation. (arXiv:1903.12279v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Dididze_G/0/1/0/all/0/1">G.Dididze</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shergelashvili_B/0/1/0/all/0/1">B.M. Shergelashvili</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melnik_V/0/1/0/all/0/1">V.N. Melnik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dorovskyy_V/0/1/0/all/0/1">V.V. Dorovskyy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brazhenko_A/0/1/0/all/0/1">A.I. Brazhenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poedts_S/0/1/0/all/0/1">S. Poedts</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zaqarashvili_T/0/1/0/all/0/1">T.V. Zaqarashvili</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khodachenko_M/0/1/0/all/0/1">M. Khodachenko</a> As is well known, CME propagation often results in the fragmentation of the solar atmosphere on smaller regions of density (magnetic field) enhancement (depletion). It is expected that this type of fragmentation may have radio signatures. The general aim of the present paper is to perform a comparative analysis of type III solar and narrow-band type-III-like radio burst properties before and during CME events, respectively. The main goal isRead More →

Planetesimal fragmentation and giant planet formation II: dependencies with planetesimal relative velocities and compositions. (arXiv:1903.12288v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sebastian_I/0/1/0/all/0/1">I. L. San Sebasti&#xe1;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guilera_O/0/1/0/all/0/1">O. M. Guilera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parisi_M/0/1/0/all/0/1">M. G. Parisi</a> Most of planet formation models that incorporate planetesimal fragmentation consider a catastrophic impact energy threshold for basalts at a constant velocity of 3 km/s during all the process of the formation of the planets. However, as planets grow the relative velocities of the surrounding planetesimals increase from velocities of the order of m/s to a few km/s. In addition, beyond the ice line where giant planets are formed, planetesimals are expected to be composed roughly byRead More →

The XXL Survey: XXXVII. The role of the environment in shaping the stellar population properties of galaxies at 0.1Read More →

Quantum non-linear evolution of inflationary tensor perturbations. (arXiv:1903.12295v1 [hep-th]) <a href="http://arxiv.org/find/hep-th/1/au:+Gong_J/0/1/0/all/0/1">Jinn-Ouk Gong</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Seo_M/0/1/0/all/0/1">Min-Seok Seo</a> We study the quantum mechanical evolution of the tensor perturbations during inflation with non-linear tensor interactions. We first obtain the Lindblad terms generated by non-linear interactions by tracing out unobservable sub-horizon modes. Then we calculate explicitly the reduced density matrix for the super-horizon modes, and show that the probability of maintaining the unitarity of the squeezed state decreases in time. The decreased probability is transferred to other elements of the reduced density matrix including off-diagonal ones, so the evolution of the reduced density matrix describes the quantum-to-classical transition of theRead More →

Cosmology with powerful radio-loud AGNs. (arXiv:1903.12308v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Turner_R/0/1/0/all/0/1">Ross Turner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shabala_S/0/1/0/all/0/1">Stanislav Shabala</a> Immensely bright quasars and radio-loud active galactic nuclei (AGNs) provide an enticing opportunity to construct standard candles detectable up to the very early universe. An analytic theory is proposed to measure the distance to powerful citeauthor{FR+1974} type-II radio sources based on their integrated flux density across a broad range of radio frequencies, and the angular size and axis ratio of their synchrotron-emitting lobes. This technique can be used at low-redshift to construct absolute standard candles in conjunction with X-ray observations of the host cluster, or at high-redshift to measure the relative distancesRead More →

Models of Multi-component Splash Bridges in Face-on Galaxy Disc Collisions. (arXiv:1903.12323v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Yeager_T/0/1/0/all/0/1">Travis Yeager</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Struck_C/0/1/0/all/0/1">Curtis Struck</a> We use an inelastic particle code with shocks and cooling calculated on a subgrid level to study the gas in direct collisions between galaxy discs. The interstellar media (ISM) of the discs are modeled with continuous thermal phases. The models produce many unique structures, ranging from central bridge discs to swirled sheets, which resemble those observed in interacting galaxies. These morphologies are sensitive to the rotation, relative mass, disc offsets and the gas structure in the discs. In the case of the Taffy galaxies – NGC 12914/15,Read More →

A Collision Probability Estimation Algorithm Used in the Space Debris Evolutionary Model. (arXiv:1903.12335v1 [physics.space-ph]) <a href="http://arxiv.org/find/physics/1/au:+Wang_X/0/1/0/all/0/1">Xiao-Wei Wang</a>, <a href="http://arxiv.org/find/physics/1/au:+Liu_J/0/1/0/all/0/1">Jing Liu</a>, <a href="http://arxiv.org/find/physics/1/au:+Cui_S/0/1/0/all/0/1">Shuang-Xing Cui</a> An in-depth analysis is performed on the problem that one parameter of the Cube model can affects the final simulation results of space debris long-term evolution model, which weakens the representativeness of the space debris evolution model. We made some improvements and proposed an Improved-Cube (I-Cube) model. By multiple Monte Carlo simulations, it is indicated that the I-Cube model offered a more accurate and more reasonable option for collision probability estimation in the space debris evolution process. The simulation results of spaceRead More →

Determining Hadron-Quark Phase Transition Chemical Potential via Astronomical Observations. (arXiv:1903.12336v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Bai_Z/0/1/0/all/0/1">Zhan Bai</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Liu_Y/0/1/0/all/0/1">Yu-xin Liu</a> We propose a scheme to determine the chemical potential and baryon number density of the hadron-quark phase transition in cold dense strong interaction matter (compact star matter). The hadron matter is described with the relativistic mean field theory, and the quark matter is described with the Dyson-Schwinger equation approach of QCD. To study the first-order phase transition, we take the sound speed as the interpolation objective to construct the equation of state in the middle density region. With the maximum mass, the tidal deformability and the radius ofRead More →