Spectral synthesis for Be stars

Sigut, T. A. A.

doi:10.1017/s1743921311011045

Cited by 2 publications

(1 citation statement)

References 8 publications

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“…The rotationally distorted star irradiates the disc, which is assumed to extend out to a radius of R d equatorial radii, and the star-plus-disc system is viewed at an inclination angle (angle between the star's rotation axis and the line of sight) of i. Then, in state-of-the-art disc models such as HDUST [14] or Bedisc/BeRay [15,16], each computed observable is a function of four model parameters: ρ 0 , n, R d , and i, where ρ 0 is the axisymmetric volume density at the innermost part of the disc, and n is the exponent of the radial power law usually used to describe the Be star disc's density.…”

Section: Introductionmentioning

confidence: 99%

Infrared Spectroscopy of Be Stars: Influence of the Envelope Parameters on Brackett-Series Behaviour

Cochetti,

Granada,

Arias

et al. 2023

Galaxies

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The IR spectra of Be stars display numerous hydrogen recombination lines, constituting a great resource for obtaining information on the physical and dynamic structures of different regions within the circumstellar envelope. Nevertheless, this spectral region has not been analysed in depth, and there is a lack of synthetic spectra with which to compare observations. Therefore, we computed synthetic spectra with the HDUST code for different disc parameters. Here, we present our results on the spectral region that includes lines of the Brackett series. We discuss the dependence of the line series strengths on several parameters that describe the structure of the disc. We also compared model line profiles, fluxes, and EWs with observational data for two Be stars (MX Pup and π Aqr). Even though the synthetic spectra adequately fit our observations of both stars and allow us to constrain the parameters of the disc, there is a discrepancy with the observed data in the EW and flux measurements, especially in the case of MX Pup. It is possible that by including Brackett lines of higher terms or adding the analysis of other series, we may be able to better constrain the parameters of the observed disc.

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Section: Introductionmentioning

confidence: 99%

Infrared Spectroscopy of Be Stars: Influence of the Envelope Parameters on Brackett-Series Behaviour

Cochetti,

Granada,

Arias

et al. 2023

Galaxies

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New insights on Be shell stars from modelling their Hα emission profiles

Silaj¹,

Jones²,

Sigut³

et al. 2014

Proc. IAU

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Be shell stars are believed to be ordinary Be stars seen edge-on, which makes them particularly desirable objects for study since the uncertainty in the inclination of the rotation axis is largely eliminated. We have recently modelled high resolution Hα spectroscopic observations for eight Be shell stars, using the non-local thermodynamical equilibrium radiative transfer codeBedisk(Sigut & Jones 2007) and the new spectral synthesis packageBeray(Sigut 2011). Generally, we confirm that these systems are oriented at high inclination angles, although we find that they are not necessarily as close to edge-on as initially expected.

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Spectral synthesis for Be stars

Cited by 2 publications

References 8 publications

Infrared Spectroscopy of Be Stars: Influence of the Envelope Parameters on Brackett-Series Behaviour

Infrared Spectroscopy of Be Stars: Influence of the Envelope Parameters on Brackett-Series Behaviour

New insights on Be shell stars from modelling their Hα emission profiles

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