2020/10/12 by M. Brož, D. Mourard, J. Budaj +7 · 1 citation
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics and Star Formation Studies #Doppler effect #Emission spectrum #Interferometry #Measure (data warehouse) #RADIUS #Radiative transfer #Spectral line #Spectroscopy #Stellar, planetary, and galactic studies #Visibility #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/202039035
published as A&A 645, A51 (2021) · 19 pages, 31 figures
arxiv created 2020/10/12 · openalex created_date 2020/10/15 · openalex publication_date 2020/10/30 · arxiv updated 2021/01/13 · openalex updated_date 2026/08/06
The complex binary system β Lyr A has an extensive observational dataset: light curves (from far UV to far IR), interferometric squared visibility, closure phase, triple product measurements, spectral-energy distribution, high-resolution spectroscopy, differential visibility amplitude, and also a differential phase. In particular, we used spectra from the Ondřejov 2m telescope from 2013 to 2015 to measure the emission in H α , He I , Si II , Ne I , or C II lines, and differential interferometry by CHARA/VEGA from the 2013 campaign to measure wavelength-dependent sizes across H α and He I 6678. This allowed us to constrain not only optically thick objects (primary, secondary, accretion disc), but also optically thin objects (disc atmosphere, jets, shell). We extended our modelling tool, Pyshellspec (based on Shellspec; a 1D local thermodynamical equilibrium radiative transfer code), to include all new observables, to compute differential visibilities/phases, to perform a Doppler tomography, and to determine a joint χ 2 metric. After an optimisation of 38 free parameters, we derived a robust model of the β Lyr A system. According to the model, the emission is formed in an extended atmosphere of the disc, two perpendicular jets expanding at ∼700 km s −1 , and a symmetric shell with the radius ∼70 R ⊙ . The spectroscopy indicates a low abundance of carbon, 10 −2 of the solar value. We also quantified systematic differences between datasets, and we discuss here alternative models with higher resolutions, additional asymmetries, or He-rich abundances.