Pulsars, transients and relativistic astrophysics

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Evidence for Late-stage Eruptive Mass-loss in the Progenitor to SN2018gep, a Broad-lined Ic Supernova: Pre-explosion Emission and a Rapidly Rising Luminous Transient

(2019)

Authors:

Anna YQ Ho, Daniel A Goldstein, Steve Schulze, David K Khatami, Daniel A Perley, Mattias Ergon, Avishay Gal-Yam, Alessandra Corsi, Igor Andreoni, Cristina Barbarino, Eric C Bellm, Nadia Blagorodnova, Joe S Bright, Eric Burns, S Bradley Cenko, Virginia Cunningham, Kishalay De, Richard Dekany, Alison Dugas, Rob P Fender, Claes Fransson, Christoffer Fremling, Adam Goldstein, Matthew J Graham, David Hale, Assaf Horesh, Tiara Hung, Mansi M Kasliwal, N Paul M Kuin, Shri R Kulkarni, Thomas Kupfer, Ragnhild Lunnan, Frank J Masci, Chow-Choong Ngeow, Peter E Nugent, Eran O Ofek, Maria T Patterson, Glen Petitpas, Ben Rusholme, Hanna Sai, Itai Sfaradi, David L Shupe, Jesper Sollerman, Maayane T Soumagnac, Yutaro Tachibana, Francesco Taddia, Richard Walters, Xiaofeng Wang, Yuhan Yao, Xinhan Zhang
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The tidal disruption event AT2017eqx: spectroscopic evolution from hydrogen rich to poor suggests an atmosphere and outflow

(2019)

Authors:

M Nicholl, PK Blanchard, E Berger, S Gomez, R Margutti, KD Alexander, J Guillochon, J Leja, R Chornock, B Snios, K Auchettl, AG Bruce, P Challis, DJ D'Orazio, MR Drout, T Eftekhari, RJ Foley, O Graur, CD Kilpatrick, A Lawrence, AL Piro, C Rojas-Bravo, NP Ross, P Short, SJ Smartt, KW Smith, B Stalder
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On the Ca-strong 1991bg-like type Ia supernova 2016hnk: evidence for a Chandrasekhar-mass explosion

(2019)

Authors:

Lluís Galbany, Chris Ashall, Peter Hoeflich, Santiago González-Gaitán, Stefan Taubenberger, Maximilian Stritzinger, Eric Y Hsiao, Paolo Mazzali, Eddie Baron, Stéphane Blondin, Subhash Bose, Mattia Bulla, Jamison F Burke, Christopher R Burns, Régis Cartier, Ping Chen, Massimo Della Valle, Tiara R Diamond, Claudia P Gutiérrez, Jussi Harmanen, Daichi Hiramatsu, TW-S Holoien, Griffin Hosseinzadeh, D Andrew Howell, Yiwen Huang, Cosimo Inserra, Thomas de Jaeger, Saurabh W Jha, Tuomas Kangas, Markus Kromer, Joseph D Lyman, Kate Maguire, George Howie Marion, Dan Milisavljevic, Simon J Prentice, Alessandro Razza, Thomas M Reynolds, David J Sand, Benjamin J Shappee, Rohit Shekhar, Stephen J Smartt, Keivan G Stassun, Mark Sullivan, Stefano Valenti, Steven Villanueva, Xiaofeng Wang, J Craig Wheeler, Qian Zhai, Jujia Zhang
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Are all fast radio bursts repeating sources?

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 484:4 (2019) 5500-5508

Authors:

M Caleb, BW Stappers, K Rajwade, C Flynn
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The luminosity dependence of thermally driven disc winds in low-mass X-ray binaries

Monthly Notices of the Royal Astronomical Society 484:4 (2019) 4635-4644

Authors:

N Higginbottom, C Knigge, KS Long, JH Matthews, EJ Parkinson

Abstract:

© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. We have carried out radiation-hydrodynamic simulations of thermally driven accretion disc winds in low-mass X-ray binaries. Our main goal is to study the luminosity dependence of these outflows and compare with observations. The simulations span the range 0.04 ≤ L acc /L Edd ≤ 1.0 and therefore cover most of the parameter space in which disc winds have been observed. Using a detailed Monte Carlo treatment of ionization and radiative transfer, we confirm two key results found in earlier simulations that were carried out in the optically thin limit: (i) the wind velocity - and hence the maximum blueshift seen in wind-formed absorption lines - increases with luminosity; (ii) the large-scale wind geometry is quasi-spherical, but observable absorption features are preferentially produced along high-column equatorial sightlines. In addition, we find that (iii) the wind efficiency always remains approximately constant at skew4dotM-rm wind/skew4dotM-rm acc simeq 2, a behaviour that is consistent with observations. We also present synthetic Fe xxv and Fe xxvi absorption line profiles for our simulated disc winds in order to illustrate the observational implications of our results.
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