RAS_WEB (Page 3,812)

Probing Axions with Event Horizon Telescope Polarimetric Measurements. (arXiv:1905.02213v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Chen_Y/0/1/0/all/0/1">Yifan Chen</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Shu_J/0/1/0/all/0/1">Jing Shu</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Xue_X/0/1/0/all/0/1">Xiao Xue</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Yuan_Q/0/1/0/all/0/1">Qiang Yuan</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Zhao_Y/0/1/0/all/0/1">Yue Zhao</a> With high spatial resolution, polarimetric imaging of a supermassive black hole, like M87$^star$ or Sgr A$^star$, by the Event Horizon Telescope can be used to probe the existence of ultralight bosonic particles, such as axions. Such particles can accumulate around a rotating black hole through superradiance mechanism, forming an axion cloud. When linearly polarized photons are emitted from accretion disk near the horizon, their position angles oscillate due to the birefringent effect when traveling through the axion background. In particular,Read More →

A new empirical method to estimate the molecular gas mass in galaxies. (arXiv:1905.02214v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Concas_A/0/1/0/all/0/1">Alice Concas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Popesso_P/0/1/0/all/0/1">Paola Popesso</a> We find a tight correlation between the dust extinction, traced by the Balmer Decrement (BD$=$H$alpha$/H$beta$), the CO(1-0) line luminosity (L$_{CO}$) and total molecular gas mass (M$_{H2}$) in a sample of $222$ local star-forming galaxies drawn from the xCOLD GASS survey. As expected, the galaxy disk inclination affects the correlation by inducing a saturation of the Balmer decrement on highly inclined galaxies. Once this effect is taken into account, L$_{CO}$ and M$_{H2}$ can be expressed as a function of BD with a scatter of $sim 0.3$Read More →

New Horizon: On the origin of the stellar disk and spheroid of field galaxies. (arXiv:1905.02216v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Park_M/0/1/0/all/0/1">Min-Jung Park</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yi_S/0/1/0/all/0/1">Sukyoung K. Yi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dubois_Y/0/1/0/all/0/1">Yohan Dubois</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pichon_C/0/1/0/all/0/1">Christophe Pichon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kimm_T/0/1/0/all/0/1">Taysun Kimm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Devriendt_J/0/1/0/all/0/1">Julien Devriendt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_H/0/1/0/all/0/1">Hoseung Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Volonteri_M/0/1/0/all/0/1">Marta Volonteri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaviraj_S/0/1/0/all/0/1">Sugata Kaviraj</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peirani_S/0/1/0/all/0/1">Sebastien Peirani</a> The origin of the disk and spheroid of galaxies has been a key open question in understanding their morphology. Using the high-resolution cosmological simulation, New Horizon, we explore kinematically decomposed disk and spheroidal components of 144 field galaxies with masses greater than $rm 10^9,M_{odot}$ at $z=0.7$. The origins of stellar particles are classified according to their birthplace (inRead More →

Formation histories of stars, clusters and globular clusters in the E-MOSAICS simulations. (arXiv:1905.02217v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Reina_Campos_M/0/1/0/all/0/1">Marta Reina-Campos</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Kruijssen_J/0/1/0/all/0/1">J. M. Diederik Kruijssen</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Pfeffer_J/0/1/0/all/0/1">Joel L. Pfeffer</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Bastian_N/0/1/0/all/0/1">Nate Bastian</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Crain_R/0/1/0/all/0/1">Robert A. Crain</a> (2) ((1) Heidelberg, (2) LJMU) The formation histories of globular clusters (GCs) are a key diagnostic for understanding their relation to the evolution of the Universe through cosmic time. We use the suite of 25 cosmological zoom-in simulations of present-day Milky Way-mass galaxies from the E-MOSAICS project to study the formation histories of stars, clusters, and GCs, and how these are affected by the environmental dependence of theRead More →

SN 2016coi (ASASSN-16fp): an energetic H-stripped core-collapse supernova from a massive stellar progenitor with large mass loss. (arXiv:1905.02226v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Terreran_G/0/1/0/all/0/1">G. Terreran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Margutti_R/0/1/0/all/0/1">R. Margutti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bersier_D/0/1/0/all/0/1">D. Bersier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brimacombe_J/0/1/0/all/0/1">J. Brimacombe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caprioli_D/0/1/0/all/0/1">D. Caprioli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Challis_P/0/1/0/all/0/1">P. Challis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chornock_R/0/1/0/all/0/1">R. Chornock</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coppejans_D/0/1/0/all/0/1">D. L. Coppejans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dong_S/0/1/0/all/0/1">Subo Dong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guidorzi_C/0/1/0/all/0/1">C. Guidorzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hurley_K/0/1/0/all/0/1">K. Hurley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kirshner_R/0/1/0/all/0/1">R. Kirshner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Migliori_G/0/1/0/all/0/1">G. Migliori</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milisavljevic_D/0/1/0/all/0/1">D. Milisavljevic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Palmer_D/0/1/0/all/0/1">D. M. Palmer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prieto_J/0/1/0/all/0/1">J. L. Prieto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tomasella_L/0/1/0/all/0/1">L. Tomasella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marchant_P/0/1/0/all/0/1">P. Marchant</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pastorello_A/0/1/0/all/0/1">A. Pastorello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shappee_B/0/1/0/all/0/1">B. J. Shappee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stanek_K/0/1/0/all/0/1">K. Z. Stanek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stritzinger_M/0/1/0/all/0/1">M. D. Stritzinger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benetti_S/0/1/0/all/0/1">S. Benetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Demarchi_L/0/1/0/all/0/1">L. Demarchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elias_rosa_N/0/1/0/all/0/1">N. Elias-rosa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gall_C/0/1/0/all/0/1">C. Gall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harmanen_J/0/1/0/all/0/1">J.Read More →

The Astrochemical Impact of Cosmic Rays in Protoclusters I: Molecular Cloud Chemistry. (arXiv:1905.02232v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Gaches_B/0/1/0/all/0/1">Brandt A.L. Gaches</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Offner_S/0/1/0/all/0/1">Stella S.R. Offner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bisbas_T/0/1/0/all/0/1">Thomas G. Bisbas</a> We present astrochemical photo-dissociation region models in which cosmic ray attenuation has been fully coupled to the chemical evolution of the gas. We model the astrochemical impact of cosmic rays, including those accelerated by protostellar accretion shocks, on molecular clouds hosting protoclusters. Our models with embedded protostars reproduce observed ionization rates. We study the imprint of cosmic ray attenuation on ions for models with different surface cosmic ray spectra and different star formation efficiencies. We find that abundances, particularlyRead More →

Understanding extreme quasar optical variability with CRTS: II. Changing-state quasars. (arXiv:1905.02262v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Graham_M/0/1/0/all/0/1">Matthew J. Graham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ross_N/0/1/0/all/0/1">Nicholas P. Ross</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stern_D/0/1/0/all/0/1">Daniel Stern</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drake_r/0/1/0/all/0/1">rew J. Drake</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McKernan_B/0/1/0/all/0/1">Barry McKernan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ford_K/0/1/0/all/0/1">K. E. Saavik Ford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Djorgovski_S/0/1/0/all/0/1">S. G. Djorgovski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mahabal_A/0/1/0/all/0/1">Ashish Mahabal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glikman_E/0/1/0/all/0/1">Eilat Glikman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Larson_S/0/1/0/all/0/1">Steve Larson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Christensen_E/0/1/0/all/0/1">Eric Christensen</a> We present the results of a systematic search for quasars in the Catalina Real-time Transient Survey exhibiting both strong photometric and spectroscopic variability over a decadal baseline. We identify 73 sources with specific patterns of optical and mid-IR photometric behavior and a defined spectroscopic change. These “Changing-State” quasars (CSQs) form a higher luminosity sampleRead More →

Super-CMB fluctuations can resolve the Hubble tension. (arXiv:1905.02278v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Adhikari_S/0/1/0/all/0/1">Saroj Adhikari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huterer_D/0/1/0/all/0/1">Dragan Huterer</a> We study the covariance in the angular power spectrum estimates of CMB fluctuations when the primordial fluctuations are non-Gaussian. The non-Gaussian covariance comes from a nonzero connected four-point correlation function — or the trispectrum in Fourier space — and can be large when long-wavelength (super-CMB) modes are strongly coupled to short-wavelength modes. The effect of such non-Gaussian covariance can be modeled through additional freedom in the theoretical CMB angular power spectrum and can lead to different inferred values of the standard cosmological parameters relative to those in $Lambda$CDM. Taking theRead More →

Binary Survival in the Outer Solar System. (arXiv:1905.02282v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Nesvorny_D/0/1/0/all/0/1">David Nesvorny</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vokrouhlicky_D/0/1/0/all/0/1">David Vokrouhlicky</a> As indicated by their special characteristics, the cold classical Kuiper belt objects (KBOs) formed and survived at 42-47 au. Notably, they show a large fraction of equal-size binaries whose formation is probably related to the accretion of KBOs themselves. These binaries are uncommon in other –hot, resonant, scattered– populations, which are thought to have been implanted from the massive disk below 30 au to >30 au during Neptune’s migration. Here we highlight the possibility that equal-size binaries formed in the disk but were subsequently removed by impacts and/or dynamical effectsRead More →

Effects of adiabatic index on the sonic surface and time variability of low angular momentum accretion flows. (arXiv:1905.02289v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Palit_I/0/1/0/all/0/1">Ishika Palit</a> (CTP PAS), <a href="http://arxiv.org/find/astro-ph/1/au:+Janiuk_A/0/1/0/all/0/1">Agnieszka Janiuk</a> (CTP PAS), <a href="http://arxiv.org/find/astro-ph/1/au:+Sukova_P/0/1/0/all/0/1">Petra Sukova</a> (ASU CAS) We study the role of adiabatic index in determining the critical points in the transonic low angular momentum accretion flow onto a black hole. We present the general relativistic 2D hydrodynamic simulations of axisymmetric, inviscid accretion flows in a fixed Kerr black hole gravitational field. A relativistic fluid where its bulk velocity is comparable to the speed of light, flowing in the accretion disk very close to the horizon can beRead More →

Five new real-time detections of Fast Radio Bursts with UTMOST. (arXiv:1905.02293v1 [astro-ph.HE]) <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:+Flynn_C/0/1/0/all/0/1">C. Flynn</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:+Jameson_A/0/1/0/all/0/1">A. Jameson</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:+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. T. 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:+Gupta_V/0/1/0/all/0/1">V. Gupta</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:+Lower_M/0/1/0/all/0/1">M. E. Lower</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:+Parthasarathy_A/0/1/0/all/0/1">A. Parthasarathy</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:+Ravi_V/0/1/0/all/0/1">V. Ravi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shannon_R/0/1/0/all/0/1">R. M. Shannon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sutherland_A/0/1/0/all/0/1">A. Sutherland</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Temby_D/0/1/0/all/0/1">D. Temby</a>, <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:+Caleb_M/0/1/0/all/0/1">M. Caleb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chang_S/0/1/0/all/0/1">S.-W. Chang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cruces_M/0/1/0/all/0/1">M. Cruces</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roy_J/0/1/0/all/0/1">J. Roy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morello_V/0/1/0/all/0/1">V. Morello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Onken_C/0/1/0/all/0/1">C. A. Onken</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stappers_B/0/1/0/all/0/1">B. W. Stappers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wolf_C/0/1/0/all/0/1">C. Wolf</a>Read More →

Solar Center–Limb Variation of the Strengths of Spectral Lines: Classification and Interpretation of Observed Trends. (arXiv:1905.02306v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Takeda_Y/0/1/0/all/0/1">Y. Takeda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+UeNo_S/0/1/0/all/0/1">S. UeNo</a> The equivalent widths (W) of 565 spectral lines in the wavelength range of 4690–6870A were evaluated at 31 consecutive points from the solar disk center (mu=cos(theta)=1) to near the limb (mu=0.25) by applying the synthetic spectrum-fitting technique, in order to clarify the nature of their center–limb variations, especially the observed slope differing from line to line and its interpretation in terms of line properties. We found that the distribution of the gradient beta (= -dlog W/dlog mu) well correlates with that ofRead More →

Thermal Component in Gamma-ray Burst. I. How they Affect Non-Thermal Spectral Parameters?. (arXiv:1905.02340v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Li_L/0/1/0/all/0/1">Liang Li</a> The spectral components of prompt emission of gamma-ray bursts (GRBs) mainly consist of two possible origins: synchrotron (non-thermal) and photosphere (thermal). The typically spectral properties of GRBs can be modeled by a dominant non-thermal component (Band-like function or cutoff power-law), some of them have an additional thermal component (Planck-like function). In this paper, in order to study how the thermal components affect the non-thermal spectral parameters, we focus on eight {it Fermi}-GBM bursts of which the spectra deviate from a Band-only function, and the thermal components are significant.Read More →

Fast localization of coalescing binaries with a heterogeneous network of advanced gravitational wave detectors. (arXiv:1905.02362v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Fujii_Y/0/1/0/all/0/1">Y. Fujii</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adams_T/0/1/0/all/0/1">T. Adams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marion_F/0/1/0/all/0/1">F. Marion</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flaminio_R/0/1/0/all/0/1">R. Flaminio</a> We present the expected performance regarding fast sky localization of coalescing binaries with a network of three gravitational wave detectors having heterogeneous sensitivities, such as the LIGO-Virgo network. A hierarchical approach can be used in order to make an effective use of information from the least sensitive detector. In this approach, the presence of an event seen in coincidence in the two more sensitive detectors triggers a focused search in the data of the third, less sensitive,Read More →

Why does ammonia not freeze out in the center of pre-stellar cores?. (arXiv:1905.02384v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sipila_O/0/1/0/all/0/1">O. Sipil&#xe4;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caselli_P/0/1/0/all/0/1">P. Caselli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Redaelli_E/0/1/0/all/0/1">E. Redaelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Juvela_M/0/1/0/all/0/1">M. Juvela</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bizzocchi_L/0/1/0/all/0/1">L. Bizzocchi</a> We carried out a parameter-space exploration of the ammonia abundance in the pre-stellar core L1544, where it has been observed to increase toward the center of the core with no signs of freeze-out onto grain surfaces. We considered static and dynamical physical models coupled with elaborate chemical and radiative transfer calculations, and explored the effects of varying model parameters on the (ortho+para) ammonia abundance profile. None of our models are able to reproduce the inward-increasing tendencyRead More →

Regulation of accretion by its outflow in a symbiotic star: the 2016 outflow fast state of MWC 560. (arXiv:1905.02399v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lucy_A/0/1/0/all/0/1">Adrian B. Lucy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sokoloski_J/0/1/0/all/0/1">J. L. Sokoloski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Munari_U/0/1/0/all/0/1">U. Munari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roy_N/0/1/0/all/0/1">Nirupam Roy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuin_N/0/1/0/all/0/1">N. Paul M. Kuin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rupen_M/0/1/0/all/0/1">Michael P. Rupen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Knigge_C/0/1/0/all/0/1">Christian Knigge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Darnley_M/0/1/0/all/0/1">M. J. Darnley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luna_G/0/1/0/all/0/1">G. J. M. Luna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Somogyi_P/0/1/0/all/0/1">P&#xe9;ter Somogyi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valisa_P/0/1/0/all/0/1">P. Valisa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milani_A/0/1/0/all/0/1">A. Milani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sollecchia_U/0/1/0/all/0/1">U. Sollecchia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weston_J/0/1/0/all/0/1">Jennifer H. S. Weston</a> The symbiotic binary MWC 560 (=V694 Mon) is a laboratory for the complex relationship between an accretion disk and its outflow. In 2016, at the peak of a slow rise in optical flux,Read More →