RAS_WEB (Page 4,568)

Anisotropic inflation with coupled $boldsymbol{p}$-forms. (arXiv:1901.06097v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Almeida_J/0/1/0/all/0/1">Juan P. Beltr&#xe1;n Almeida</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Guarnizo_A/0/1/0/all/0/1">Alejandro Guarnizo</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Kase_R/0/1/0/all/0/1">Ryotaro Kase</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Tsujikawa_S/0/1/0/all/0/1">Shinji Tsujikawa</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Valenzuela_Toledo_C/0/1/0/all/0/1">C&#xe9;sar A. Valenzuela-Toledo</a> We study the cosmology in the presence of arbitrary couplings between $p$-forms in 4-dimensional space-time for a general action respecting gauge symmetry and parity invariance. The interaction between 0-form (scalar field $phi$) and 3-form fields gives rise to an effective potential $V_{rm eff}(phi)$ for the former after integrating out the contribution of the latter. We explore the dynamics of inflation on an anisotropic cosmological background for a coupled system of 0-, 1-, and 2-forms. In the absence of interactions betweenRead More →

Frequent flare events on the short-period M-type eclipsing binary BX Tri. (arXiv:1901.06106v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Luo_C/0/1/0/all/0/1">ChangQing Luo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_X/0/1/0/all/0/1">XiaoBin.Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_K/0/1/0/all/0/1">Kun Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_C/0/1/0/all/0/1">Chao Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fang_X/0/1/0/all/0/1">Xiangsong Fang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_C/0/1/0/all/0/1">Chunguang Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deng_L/0/1/0/all/0/1">Licai Deng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nie_J/0/1/0/all/0/1">Jundan Nie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fox_Machado_L/0/1/0/all/0/1">Lester Fox-Machado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luo_Y/0/1/0/all/0/1">Yangping Luo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Niu_H/0/1/0/all/0/1">Hubiao Niu</a> We present long-term, multi-color photometric monitoring and spectroscopic observations of the short-period M-type eclipsing binary BX Tri. Six flare events were recorded in 4 years from 2014 to 2017. Three of them were detected on one night within an orbital cycle. The strongest one was identified on December 23, 2014. With the amplitudes of $Delta$B=0.48 mag, $Delta$V=0.28 mag, $Delta$R=0.10 mag,Read More →

About the Kerr nature of the stellar-mass black hole in GRS 1915+105. (arXiv:1901.06117v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Zhang_Y/0/1/0/all/0/1">Yuexin Zhang</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Abdikamalov_A/0/1/0/all/0/1">Askar B. Abdikamalov</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Ayzenberg_D/0/1/0/all/0/1">Dimitry Ayzenberg</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Bambi_C/0/1/0/all/0/1">Cosimo Bambi</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Dauser_T/0/1/0/all/0/1">Thomas Dauser</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Garcia_J/0/1/0/all/0/1">Javier A. Garcia</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Nampalliwar_S/0/1/0/all/0/1">Sourabh Nampalliwar</a> We employ the accretion disk reflection model RELXILL_NK to test the spacetime geometry around the stellar-mass black hole in GRS 1915+105. We adopt the Johannsen metric with the deformation parameters $alpha_{13}$ and $alpha_{22}$, for which the Kerr solution is recovered when $alpha_{13} = alpha_{22} = 0$. We analyze a NuSTAR observation of 2012, obtaining vanishing and non-vanishing values of the deformation parameters depending on the astrophysical model adopted.Read More →

Decay of I-ball/Oscillon in Classical Field Theory. (arXiv:1901.06130v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Ibe_M/0/1/0/all/0/1">Masahiro Ibe</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kawasaki_M/0/1/0/all/0/1">Masahiro Kawasaki</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Nakano_W/0/1/0/all/0/1">Wakutaka Nakano</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Sonomoto_E/0/1/0/all/0/1">Eisuke Sonomoto</a> I-balls/oscillons are long-lived and spatially localized solutions of real scalar fields. They are produced in various contexts of the early universe in, such as, the inflaton evolution and the axion evolution. However, their decay process has long been unclear. In this paper, we derive an analytic formula of the decay rate of the I-balls/oscillons within the classical field theory. In our approach, we calculate the Poynting vector of the perturbation around the I-ball/oscillon profile by solving a relativistic field equation, with which the decayRead More →

An Analytical Model of the Kelvin-Helmholtz Instability of Transverse Coronal Loop Oscillations. (arXiv:1901.06132v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Barbulescu_M/0/1/0/all/0/1">Mihai Barbulescu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruderman_M/0/1/0/all/0/1">Michael S. Ruderman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doorsselaere_T/0/1/0/all/0/1">Tom Van Doorsselaere</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Erdelyi_R/0/1/0/all/0/1">Robert Erdelyi</a> Recent numerical simulations have demonstrated that transverse coronal loop oscillations are susceptible to the Kelvin-Helmholtz (KH) instability due to the counter-streaming motions at the loop boundary. We present the first analytical model of this phenomenon. The region at the loop boundary where the shearing motions are greatest is treated as a straight interface separating time-periodic counter-streaming flows. In order to consider a twisted tube, the magnetic field at one side of the interface is inclined. We showRead More →

Fermi GBM GRBs with characteristics similar to GRB 170817A. (arXiv:1901.06158v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kienlin_A/0/1/0/all/0/1">A. von Kienlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Veres_P/0/1/0/all/0/1">P. Veres</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roberts_O/0/1/0/all/0/1">O. J. Roberts</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hamburg_R/0/1/0/all/0/1">R. Hamburg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bissaldi_E/0/1/0/all/0/1">E. Bissaldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Briggs_M/0/1/0/all/0/1">M. S. Briggs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burns_E/0/1/0/all/0/1">E. Burns</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goldstein_A/0/1/0/all/0/1">A. Goldstein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kocevski_D/0/1/0/all/0/1">D. Kocevski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Preece_R/0/1/0/all/0/1">R. D. Preece</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilson_Hodge_C/0/1/0/all/0/1">C. A. Wilson-Hodge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hui_C/0/1/0/all/0/1">C. M. Hui</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mailyan_B/0/1/0/all/0/1">B. Mailyan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malacaria_C/0/1/0/all/0/1">C. Malacaria</a> We present a search for gamma-ray bursts in the Fermi-GBM 10 year catalog that show similar characteristics to GRB 170817A, the first electromagnetic counterpart to a GRB identified as a binary neutron star (BNS) merger via gravitational wave observations. Our search is focused on a non-thermalRead More →

Asteroseismology of the Hyades red giant and planet host epsilon Tau. (arXiv:1901.06187v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Arentoft_T/0/1/0/all/0/1">Torben Arentoft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grundahl_F/0/1/0/all/0/1">Frank Grundahl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+White_T/0/1/0/all/0/1">Timothy R. White</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Slumstrup_D/0/1/0/all/0/1">Ditte Slumstrup</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Handberg_R/0/1/0/all/0/1">Rasmus Handberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lund_M/0/1/0/all/0/1">Mikkel N. Lund</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brogaard_K/0/1/0/all/0/1">Karsten Brogaard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andersen_M/0/1/0/all/0/1">Mads F. Andersen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aquirre_V/0/1/0/all/0/1">Victor Silva Aquirre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_C/0/1/0/all/0/1">Chunguang Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_X/0/1/0/all/0/1">Xiaodian Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yan_Z/0/1/0/all/0/1">Zhengzhou Yan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pope_B/0/1/0/all/0/1">Benjamin J.S. Pope</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huber_D/0/1/0/all/0/1">Daniel Huber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kjeldsen_H/0/1/0/all/0/1">Hans Kjeldsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Christensen_Dalsgaard_J/0/1/0/all/0/1">J&#xf8;rgen Christensen-Dalsgaard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jessen_Hansen_J/0/1/0/all/0/1">Jens Jessen-Hansen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antoci_V/0/1/0/all/0/1">Victoria Antoci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frandsen_S/0/1/0/all/0/1">S&#xf8;ren Frandsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bedding_T/0/1/0/all/0/1">Timothy R. Bedding</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Palle_P/0/1/0/all/0/1">Pere L. Palle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_R/0/1/0/all/0/1">Rafael A. Garcia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deng_L/0/1/0/all/0/1">Licai Deng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hon_M/0/1/0/all/0/1">Marc Hon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stello_D/0/1/0/all/0/1">Dennis Stello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jorgensen_U/0/1/0/all/0/1">Uffe G. J&#xf8;rgensen</a> Asteroseismic analysis of solar-like starsRead More →

The geometry of the magnetic field in the Central Molecular Zone measured by PILOT. (arXiv:1901.06196v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mangilli_A/0/1/0/all/0/1">A. Mangilli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aumont_J/0/1/0/all/0/1">J. Aumont</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernard_J/0/1/0/all/0/1">J.-Ph. Bernard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buzzelli_A/0/1/0/all/0/1">A. Buzzelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gasperis_G/0/1/0/all/0/1">G. de Gasperis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Durrive_J/0/1/0/all/0/1">J. B. Durrive</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferriere_K/0/1/0/all/0/1">K. Ferri&#xe8;re</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Foenard_G/0/1/0/all/0/1">G. Fo&#xeb;nard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughes_A/0/1/0/all/0/1">A. Hughes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lacourt_A/0/1/0/all/0/1">A. Lacourt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Misawa_R/0/1/0/all/0/1">R. Misawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Montier_L/0/1/0/all/0/1">L. Montier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mot_B/0/1/0/all/0/1">B. Mot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ristorcelli_I/0/1/0/all/0/1">I. Ristorcelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roussel_H/0/1/0/all/0/1">H. Roussel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ade_P/0/1/0/all/0/1">P. Ade</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alina_D/0/1/0/all/0/1">D. Alina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernardis_P/0/1/0/all/0/1">P. de Bernardis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pino_E/0/1/0/all/0/1">E. de Gouveia Dal Pino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dubois_J/0/1/0/all/0/1">J. P. Dubois</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Engel_C/0/1/0/all/0/1">C. Engel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hargrave_P/0/1/0/all/0/1">P. Hargrave</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laureijs_R/0/1/0/all/0/1">R. Laureijs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Longval_Y/0/1/0/all/0/1">Y. Longval</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maffei_B/0/1/0/all/0/1">B. Maffei</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Magalhaes_A/0/1/0/all/0/1">A. M. Magalh&#xe3;es</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marty_C/0/1/0/all/0/1">C. Marty</a>,Read More →

Determining the presence of characteristic fragmentation length-scales in filaments. (arXiv:1901.06205v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Clarke_S/0/1/0/all/0/1">S. D. Clarke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Williams_G/0/1/0/all/0/1">G. M. Williams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ibanez_Mejia_J/0/1/0/all/0/1">J. C. Ib&#xe1;&#xf1;ez-Mej&#xed;a</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walch_S/0/1/0/all/0/1">S. Walch</a> Theories suggest that filament fragmentation should occur on a characteristic fragmentation length-scale. This fragmentation length-scale can be related to filament properties, such as the width and the dynamical state of the filament. Here we present a study of a number of fragmentation analysis techniques applied to filaments, and their sensitivity to characteristic fragmentation length-scales. We test the sensitivity to both single-tier and two-tier fragmentation, i.e. when the fragmentation can be characterised with one or two fragmentation length-scales respectively. TheRead More →

The Size, Shape, and Scattering of Sagittarius A* at 86 GHz: First VLBI with ALMA. (arXiv:1901.06226v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Issaoun_S/0/1/0/all/0/1">S. Issaoun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnson_M/0/1/0/all/0/1">M. D. Johnson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blackburn_L/0/1/0/all/0/1">L. Blackburn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brinkerink_C/0/1/0/all/0/1">C. D. Brinkerink</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moscibrodzka_M/0/1/0/all/0/1">M. Mo&#x15b;cibrodzka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chael_A/0/1/0/all/0/1">A. Chael</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goddi_C/0/1/0/all/0/1">C. Goddi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marti_Vidal_I/0/1/0/all/0/1">I. Mart&#xed;-Vidal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wagner_J/0/1/0/all/0/1">J. Wagner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doeleman_S/0/1/0/all/0/1">S. S. Doeleman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Falcke_H/0/1/0/all/0/1">H. Falcke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krichbaum_T/0/1/0/all/0/1">T. P. Krichbaum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Akiyama_K/0/1/0/all/0/1">K. Akiyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bach_U/0/1/0/all/0/1">U. Bach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouman_K/0/1/0/all/0/1">K. L. Bouman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bower_G/0/1/0/all/0/1">G. C. Bower</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Broderick_A/0/1/0/all/0/1">A. Broderick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cho_I/0/1/0/all/0/1">I. Cho</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crew_G/0/1/0/all/0/1">G. Crew</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dexter_J/0/1/0/all/0/1">J. Dexter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fish_V/0/1/0/all/0/1">V. Fish</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gold_R/0/1/0/all/0/1">R. Gold</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gomez_J/0/1/0/all/0/1">J. L. G&#xf3;mez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hada_K/0/1/0/all/0/1">K. Hada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hernandez_Gomez_A/0/1/0/all/0/1">A. Hern&#xe1;ndez-G&#xf3;mez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Janssen_M/0/1/0/all/0/1">M. Jan&#xdf;en</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kino_M/0/1/0/all/0/1">M. Kino</a>,Read More →

Effects of SASI and LESA in the neutrino emission of rotating supernovae. (arXiv:1901.06235v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Walk_L/0/1/0/all/0/1">Laurie Walk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tamborra_I/0/1/0/all/0/1">Irene Tamborra</a> (Niels Bohr Institute), <a href="http://arxiv.org/find/astro-ph/1/au:+Janka_H/0/1/0/all/0/1">Hans-Thomas Janka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Summa_A/0/1/0/all/0/1">Alexander Summa</a> (MPA, Garching) Rotation of core-collapse supernovae (SNe) affects the neutrino emission characteristics. By comparing the neutrino properties of three three-dimensional SN simulations of a 15 M_sun progenitor (one non-rotating model and two models rotating at different velocities), we investigate how the neutrino emission varies with the flow dynamics in the SN core depending on the different degrees of rotation. The large-amplitude sinusoidal modulations due to the standing accretion-shock instability (SASI) are weaker in both the rotatingRead More →

Near-infrared observations of star formation and gas flows in the NUGA galaxy NGC 1365. (arXiv:1901.06241v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Fazeli_N/0/1/0/all/0/1">Nastaran Fazeli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Busch_G/0/1/0/all/0/1">Gerold Busch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valencia_S%2E_M/0/1/0/all/0/1">Monica Valencia-S.</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eckart_A/0/1/0/all/0/1">Andreas Eckart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zajacek_M/0/1/0/all/0/1">Michal Zajacek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Combes_F/0/1/0/all/0/1">Francoise Combes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Burillo_S/0/1/0/all/0/1">Santiago Garcia-Burillo</a> In the framework of understanding the gas and stellar kinematics and their relations to AGNs and galaxy evolution scenarios, we present spatially resolved distributions and kinematics of the stars and gas in the central $sim 800$-pc radius of the nearby Seyfert galaxy NGC 1365. We obtained $H+K$- and $K$-band near-infrared (NIR) integral-field observations from VLT/SINFONI. Our results reveal strong broad and narrow emission-line components of ionized gas (hydrogenRead More →

Cometary topography and phase darkening. (arXiv:1901.06250v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Vincent_J/0/1/0/all/0/1">Jean-Baptiste Vincent</a> Cometary surfaces can change significantly and rapidly due to the sublimation of their volatile material. Many authors have investigated this evolution; Vincent et al. (2017) have used topographic data from all comets visited by spacecrafts to derive a quantitative model which relates large scale roughness (i.e. topography) with the evolution state of the nucleus for Jupiter Family Comets (JFCs). Meanwhile, ground based observers have published measurements of the phase functions of many JFCs and reported a trend in the phase darkening, with primitive objects showing a stronger darkening than evolved ones). In this paper, weRead More →

A macronova associated with GRB 070809. (arXiv:1901.06269v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Jin_Z/0/1/0/all/0/1">Zhi-Ping Jin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Covino_S/0/1/0/all/0/1">Stefano Covino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liao_N/0/1/0/all/0/1">Neng-Hui Liao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_X/0/1/0/all/0/1">Xiang Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAvanzo_P/0/1/0/all/0/1">Paolo D&#x27;Avanzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fan_Y/0/1/0/all/0/1">Yi-Zhong Fan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wei_D/0/1/0/all/0/1">Da-Ming Wei</a> GRB 070809 is a typical short gamma-ray burst (sGRB) detected by the Neil Gehrels {it Swift} Observatory and at the location of the burst no underlying galaxy down to $sim 28$th AB magnitude in F606W-band has been detected. The X-ray emission was detected quickly after the trigger of the burst and the late time spectrum is very hard. The optical component, substantially brighter than the X-ray extrapolation, is also roughly consistent with a thermal-like emission, andRead More →

Probing the Turbulence Dissipation Range and Magnetic Field Strengths in Molecular Clouds. II. Directly Probing the Ion-neutral Decoupling Scale. (arXiv:1901.06289v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Tang_K/0/1/0/all/0/1">Kwok Sun Tang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_H/0/1/0/all/0/1">Hua-Bai Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_W/0/1/0/all/0/1">Wing-Kit Lee</a> The linewidth of ions has been observed to be systematically narrower than that of the coexisting neutrals in molecular clouds (Houde et al. 2000) and been interpreted as the signature of the decoupling of the neutral turbulence from magnetic fields in partially ionized medium (Li & Houde 2008; Paper I, hereafter). As a sequel of Paper I, here we present further observational evidence that lend support to these earlier proposals with the velocity coordinateRead More →

On particle creation/decay in nonminimally coupled models of gravity. (arXiv:1901.06299v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Azevedo_R/0/1/0/all/0/1">R.P.L. Azevedo</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Avelino_P/0/1/0/all/0/1">P.P. Avelino</a> In extended models of gravity a nonminimal coupling to matter has been assumed to lead to irreversible particle creation. In this paper we challenge this assumption. We argue that a non-minimal coupling of the matter and gravitational sectors results in a change in particle-momentum on a cosmological timescale, irrespective of particle creation or decay. We further argue that particle creation or decay associated with a non-minimal coupling to gravity could only happen as a result of significant deviations from a homogeneous Friedmann-Robertson-Walker geometry on microscopic scales, and provideRead More →

The onset of the AGB wind tied to a transition between sequences in the period-luminosity diagram. (arXiv:1901.06325v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+McDonald_I/0/1/0/all/0/1">Iain McDonald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trabucchi_M/0/1/0/all/0/1">Michele Trabucchi</a> We link the onset of pulsation-enhanced, dust-driven winds from asymptotic giant branch (AGB) stars in the Magellanic Clouds to the star’s transition between period–luminosity sequences (from B to C’). This transition occurs at ~60 days for solar-mass stars, which represent the bulk of the AGB population: this is the same period at which copious dust production starts in solar-neighbourhood AGB stars. It is contemporaneous with the onset of long-secondary period (LSP) variability on sequence D. The combined amplitude of the first-overtoneRead More →

Detecting Baryon Acoustic Oscillations in Dark Matter from Kinematic Weak Lensing Surveys. (arXiv:1901.06326v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ding_Z/0/1/0/all/0/1">Zhejie Ding</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seo_H/0/1/0/all/0/1">Hee-Jong Seo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huff_E/0/1/0/all/0/1">Eric Huff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saito_S/0/1/0/all/0/1">Shun Saito</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clowe_D/0/1/0/all/0/1">Douglas Clowe</a> We investigate the feasibility of extracting Baryon Acoustic Oscillations (BAO) from cosmic shear tomography. We particularly focus on the BAO scale precision that can be achieved by future spectroscopy-based, kinematic weak lensing (KWL) surveys citep[e.g.,][]{Huff13} in comparison to the traditional photometry-based weak lensing surveys. We simulate cosmic shear tomography data of such surveys with a few simple assumptions to focus on the BAO information, extract the spacial power spectrum, and constrain the recovered BAO feature. DueRead More →

The Milky Way like galaxy NGC 6384 and its nuclear star cluster at high NIR spatial resolution using LBT/ARGOS commissioning data. (arXiv:1901.06350v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Georgiev_I/0/1/0/all/0/1">Iskren Y. Georgiev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Neumayer_N/0/1/0/all/0/1">Nadine Neumayer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaessler_W/0/1/0/all/0/1">Wolfgang Gaessler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rabien_S/0/1/0/all/0/1">Sebastian Rabien</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Busoni_L/0/1/0/all/0/1">Lorenzo Busoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonaglia_M/0/1/0/all/0/1">Marco Bonaglia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ziegleder_J/0/1/0/all/0/1">Julian Ziegleder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xivry_G/0/1/0/all/0/1">Gilles Orban de Xivry</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peter_D/0/1/0/all/0/1">Diethard Peter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kulas_M/0/1/0/all/0/1">Martin Kulas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Borelli_J/0/1/0/all/0/1">Jose Borelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rahmer_G/0/1/0/all/0/1">Gustavo Rahmer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lefebvre_M/0/1/0/all/0/1">Michael Lefebvre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baumgardt_H/0/1/0/all/0/1">Holger Baumgardt</a> We analyse high spatial resolution near infra-red (NIR) imaging of NGC6384, a Milky Way like galaxy, using ARGOS commissioning data at the Large Binocular Telescope (LBT). ARGOS provides a stable PSF$_{rm FWHM}!=!0.2″!-!0.3″$ AO correction of the groundRead More →

The Solar Neighborhood XLV. The Stellar Multiplicity Rate of M Dwarfs Within 25 pc. (arXiv:1901.06364v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Winters_J/0/1/0/all/0/1">Jennifer G. Winters</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henry_T/0/1/0/all/0/1">Todd J. Henry</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jao_W/0/1/0/all/0/1">Wei-Chun Jao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Subasavage_J/0/1/0/all/0/1">John P. Subasavage</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chatelain_J/0/1/0/all/0/1">Joseph P. Chatelain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Slatten_K/0/1/0/all/0/1">Ken Slatten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riedel_A/0/1/0/all/0/1">Adric R. Riedel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silverstein_M/0/1/0/all/0/1">Michele L. Silverstein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Payne_M/0/1/0/all/0/1">Matthew J. Payne</a> We present results of the largest, most comprehensive study ever done of the stellar multiplicity of the most common stars in the Galaxy, the red dwarfs. We have conducted an all-sky, volume-limited survey for stellar companions to 1120 M dwarf primaries known to lie within 25 pc of the Sun via trigonometric parallaxes. In additionRead More →