Visible and near-infrared spectro-interferometric analysis of the edge-on Be star o Aquarii

  title={Visible and near-infrared spectro-interferometric analysis of the edge-on Be star o Aquarii},
  author={E. S. G. de Almeida and Anthony Meilland and A. Domiciano de Souza and P. Stee and Denis Mourard and Nicolas Nardetto and Roxanne Ligi and I. Tallon-Bosc and Daniel Moser Faes and Alex C. Carciofi and Daniel Bednarski and B. C. Mota and Neal J. Turner and Theo A. ten Brummelaar},
  journal={Astronomy and Astrophysics},
We present a detailed visible and near-IR spectro-interferometric analysis of the Be-shell star $\omicron$ Aquarii from quasi-contemporaneous CHARA/VEGA and VLTI/AMBER observations. We measured the stellar radius of $\omicron$ Aquarii as 4.0 $\pm$ 0.3 $\mathrm{R_{\odot}}$. We constrained the disk geometry and kinematics using a kinematic model and a MCMC fitting procedure. The disk sizes in H$\alpha$ and Br$\gamma$ were found to be similar, at $\sim$10-12 $\mathrm{D_{\star}}$, which is uncommon… 
The Hα line emission of the Be star β Psc: the last 40 yr
A study on the photosphere and disc of the Be star β Psc is presented. We recover almost 40 yr of high-resolution spectroscopic observations and additional data gathered from the BeSS data base. We
The Viscosity Parameter for Late-type Stable Be Stars
Using hydrodynamic principles we investigate the nature of the disk viscosity following the parameterization by Shakura & Sunyaev adopted for the viscous decretion model in classical Be stars. We
Eyes on Phact: unraveling a Be star and its disk
Disks are a common feature in astrophysical systems. They are present in young stellar objects, cataclysmic variables, and even active galactic nuclei. Many of these disks can be well described by
A Multi–Observing Technique Study of the Dynamical Evolution of the Viscous Disk around the Be Star ω CMa
The observed emission lines of Be stars originate from a circumstellar Keplerian disk, which is generally well explained by the viscous decretion disk model. In an earlier work we performed modeling
Disks and winds around hot stars: new insights from multi-wavelength spectroscopy and interferometry
Hot stars are the main source of ionization of the interstellar medium and its enrichment due to heavy elements. Constraining the physical conditions of their environments is crucial to understand


The Circumstellar Disk of the Be Star $o$~Aquarii
Omicron Aquarii is late-type, Be shell star with a stable and nearly symmetric H$\alpha$ emission line. We combine H$\alpha$ interferometric observations obtained with the Navy Precision Optical
Statistical analysis of intrinsic polarization, IR excess and projected rotational velocity distributions of classical Be stars
We present the results of statistical analyses of a sample of 627 Be stars. The parameters of intrinsic polarization $(p_{\ast})$, projected rotational velocity $(v \sin{i})$, and near IR excesses
GRAVITY Spectro-interferometric Study of the Massive Multiple Stellar System HD 93206 A
Characterization of the dynamics of massive star systems and the astrophysical properties of the interacting components are a prerequisite for understanding their formation and evolution. Optical
Resolving Vega and the inclination controversy with CHARA/MIRC
Optical and infrared interferometers definitively established that the photometric standard Vega (={alpha} Lyrae) is a rapidly rotating star viewed nearly pole-on. Recent independent spectroscopic
The life cycles of Be viscous decretion discs: time-dependent modelling of infrared continuum observations
We apply the viscous decretion disc (VDD) model to interpret the infrared disc continuum emission of 80 Be stars observed in different epochs. In this way, we determined 169 specific disc structures,
Near-IR and visible interferometry of Be stars: Constraints from wind models
We report theoretical HI visible and near-IR line profiles, i.e. Hα (6562 A), Hβ (4861 A) and Brγ (21 656 A), and intensity maps for a large set of parameters (density, temperature, envelope
The polar wind of the fast rotating Be star Achernar. VINCI/VLTI interferometric observations of an
Be stars show evidence of mass loss and circumstellar envelopes (CSE), from UV resonance lines, near-IR excesses and the presence of episodic hydrogen emission lines. The geometry of these envelopes
Spectral and spatial imaging of the Be+sdO binary phi Persei
The rapidly rotating Be star phi Persei was spun up by mass and angular momentum transfer from a now stripped-down, hot subdwarf companion. Here we present the first high angular resolution images of
Outbursts and Disk Variability in Be Stars
In order to study the growth and evolution of circumstellar disks around classical Be stars, we analyze optical time-series photometry from the KELT survey with simultaneous infrared and visible
VLTI/MIDI observations of 7 classical Be stars
Context. Classical Be stars are hot non-supergiant stars surrounded by a gaseous circumstellar envelope that is responsible for the observed IR-excess and emission lines. The origin of this envelope,