Discovery of optical outflows and inflows in the black hole candidate GRS 1716−249. Issue 1 (6th August 2020)

• Record Type: Journal Article
• Authors: Cúneo, V A; Muñoz-Darias, T; Sánchez-Sierras, J; Jiménez-Ibarra, F; Armas Padilla, M; Buckley, D A H; Casares, J; Charles, P; Corral-Santana, J M; Fender, R; Fernández-Ontiveros, J A; Mata Sánchez, D; Panizo-Espinar, G; Ponti, G; Torres, M A P
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 498:Issue 1(2020)
• Page Start: 25
• Page End: 32
• Publication Date: 2020-08-06
• Subjects: accretion, accretion discs -- black hole physics -- stars: individual: GRS 1716−249 -- stars: winds, outflows -- X-rays: binaries; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa2241
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We present optical spectroscopy obtained with the GTC, VLT, and SALT telescopes during the decline of the 2016–2017 outburst of the black hole candidate GRS 1716−249 (Nova Oph 1993). Our 18-epoch data set spans 6 months and reveals that the observational properties of the main emission lines are very variable, even on time-scales of a few hours. Several epochs are characterized by P-Cyg (as well as flat-top and asymmetric) profiles in the Hα, Hβ, and He ii (λ4686) emission lines, implying the presence of an accretion disc wind, which is likely hot and dense. The wind's terminal velocity (∼2000 km s −1 ) is similar to that observed in other black hole X-ray transients. These lines also show transient and sharp red-shifted absorptions, taking the form of inverted P-Cyg profiles. We argue that these profiles can be explained by the presence of infalling material at ∼1300 km s −1 . We propose a failed wind scenario to explain this inflow and discuss other alternatives, such as obscuration produced by an accretion-related structure (e.g. the gas stream) in a high inclination system.