<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Maravelias, G.</style></author><author><style face="normal" font="default" size="100%">Kraus, M.</style></author><author><style face="normal" font="default" size="100%">Cidale, L. S.</style></author><author><style face="normal" font="default" size="100%">Borges Fernandes, M.</style></author><author><style face="normal" font="default" size="100%">Arias, M. L.</style></author><author><style face="normal" font="default" size="100%">Curé, M.</style></author><author><style face="normal" font="default" size="100%">Vasilopoulos, G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Resolving the kinematics of the discs around Galactic B[e] supergiants</style></title><short-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></short-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astrophysics - Solar and Stellar Astrophysics</style></keyword><keyword><style  face="normal" font="default" size="100%">circumstellar matter</style></keyword><keyword><style  face="normal" font="default" size="100%">outflows</style></keyword><keyword><style  face="normal" font="default" size="100%">stars: early-type</style></keyword><keyword><style  face="normal" font="default" size="100%">stars: massive</style></keyword><keyword><style  face="normal" font="default" size="100%">stars: winds</style></keyword><keyword><style  face="normal" font="default" size="100%">supergiants</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2018</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2018/10/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2018MNRAS.480..320M</style></url></web-urls></urls><publisher><style face="normal" font="default" size="100%">OUP</style></publisher><volume><style face="normal" font="default" size="100%">480</style></volume><pages><style face="normal" font="default" size="100%">320 - 344</style></pages><isbn><style face="normal" font="default" size="100%">0035-8711</style></isbn><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">B[e] supergiants are luminous evolved massive stars. The mass-loss during this phase creates a complex circumstellar environment with atomic, molecular, and dusty regions usually found in rings or disc-like structures. For a better comprehension of the mechanisms behind the formation of these rings, detailed knowledge about their structure and dynamics is essential. To address that, we obtained high-resolution optical and near-infrared (near-IR) spectra for eight selected Galactic B[e] supergiants, for which CO emission has been detected. Assuming Keplerian rotation for the disc, we combine the kinematics obtained from the CO bands in the near-IR with those obtained by fitting the forbidden emission [O I] λ5577, [O I] λλ6300,6363, and [Ca II] λλ7291,7323 lines in the optical to probe the disc structure. We find that the emission originates from multiple ring structures around all B[e] supergiants, with each one of them displaying a unique combination of rings regardless of whether the object is part of a binary system. The confirmed binaries display spectroscopic variations of their line intensities and profiles as well as photometric variability, whereas the ring structures around the single stars are stable.</style></abstract></record></records></xml>