Evidence for Different Disk Mass Distributions between Early- and Late-type Be Stars in the BeSOS Survey

Arcos, C.; Jones, C. E.; Sigut, T. A. A.; Kanaan, S.; Curé, M.

doi:10.3847/1538-4357/aa6f5f

Cited by 34 publications

(70 citation statements)

References 53 publications

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“…Moreover, statistical results were based on a percentage of the representative models (best range of models) for each Hα emission line, where they found that the disk mass and angular momentum distributions are different between early (B0-B3) and late (B4-B9) subspectral types. Also, they found values of the power-law density distribution (see eq.1 on Arcos et al (2017)) of log ρ ∼ -10.4 to -10.2, and n ∼ 2.0 to 2.5 and disk masses of 3.4×10 −9 and 9.5×10 −10 M for early and late spectral types, respectively. For the disk size, they calculated the emitting region containing 90% of the total Hα flux given a range of values concentrated between 10 and 15 stellar radius.…”

Section: Physical Models Fitted On Hα Emission Linesmentioning

confidence: 99%

“…It is important to note that our actual photometric analysis does not fit the infrared excess. The reader is invited to use radiative transfer codes such as Hdust (Carciofi 2001) to reproduce the IR excess as well as physical models of Be stars (e.g., Domiciano de Souza et al 2014;Silaj et al 2016;Arcos et al 2017).…”

Section: Photometrymentioning

confidence: 99%

“…These stars are poorly studied and there is no information available in the literature about an existing disk, except for HD 42167 where previous work was done deriving the disk parameters in Arcos et al (2017). The spectral type is taken from the literature and is compared with that obtained in this work.…”

Section: New Emission Line Starsmentioning

confidence: 99%

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Stellar parameters and H α line profile variability of Be stars in the BeSOS survey

Arcos

Kanaan

Chavez

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The Be phenomenon is present in about 20% of the B-type stars. Be stars show variability on a broad range of timescales, which in most cases is related to the presence of a circumstellar disk of variable size and structure. For this reason a time resolved survey is highly desirable in order to understand the mechanisms of disk formation which are still poorly understood. In addition, a complete observational sample would improve the statistical significance of the study of the stellar and disk parameters. The "Be Stars Observation Survey" (BeSOS) is a survey containing reduced spectra obtained using the echelle spectrograph PUCHEROS with a spectral resolution of 17000 in the range of 4260-7300Å. BeSOS's main objective is to offer consistent spectroscopic and time resolved data obtained with one instrument. The user can download or plot the data and get the stellar parameters directly from the website. We also provide a starby-star analysis based on photometric, spectroscopic and interferometric data as well as general information about the whole BeSOS sample. Recently, BeSOS led to the discovery of a new Be star HD 42167 and facilitated study of the V/R variation of HD 35165 and HD 120324, the steady disk of HD 110335 and the Be shell status of HD 127972. Optical spectra used in this work, as well as the derived stellar parameters are available online in http://besos.ifa.uv.cl.

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Section: Physical Models Fitted On Hα Emission Linesmentioning

confidence: 99%

Section: Photometrymentioning

confidence: 99%

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Stellar parameters and H α line profile variability of Be stars in the BeSOS survey

Arcos

Kanaan

Chavez

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…Other studies have determined the radial extent of the Hα emitting region for sets of Be stars and specific stars. For example, using Hα spectroscopy Hanuschik (1986) find the emitting regions of 20 R * for 24 bright Be stars, Slettebak et al (1992) determine sizes of 7 to 19 for a sample of 41 Be stars, and more recently Arcos et al (2016) find a concentration of disk sizes of 5 to 20 R * . Size estimates based on interferometric GD models encompassing 80% of a star's brightness at FWHM for Hα emitting regions for 12 Be stars are shown in Rivinius et al (2013).…”

Section: Discussion and Summarymentioning

confidence: 99%

The Disk Physical Conditions of 48 Persei Constrained by Contemporaneous Hα Spectroscopy and Interferometry

Jones

Sigut

Grzenia

et al. 2017

ApJ

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We utilize a multi-step modelling process to produce synthetic interferometric and spectroscopic observables, which are then compared to their observed counterparts. (2010) and Vieira et al. (2017). Our best-fitting combined model from Hα spectroscopy, Hα interferometry and SED fitting has a power law density fall off, n, of 2.3 and an initial density at the stellar surface of ρ 0 = 1.0 × 10 −11 g · cm −3 with a inclination constrained by Hα spectroscopy and interferometry of 45 • ± 5 • . The position angle for the system, measured east from north, is 121 • ± 1 • . Our bestfit model shows that the disk emission originates in a moderately large disk with a radius of 25 R * which is consistent with a disk mass of approximately 5 × 10 24 g or 3 × 10 −10 M * . Finally, we compare our results with previous studies of 48 Per by Quirrenbach et al. (1997) with agreement but find, with our much larger data set, that our disk size contradicts the findings of Delaa et al. (2011).

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“…Carciofi (2011) used the VDD model to construct the basis of new paradigm for the interpretation of Be stars observations. Then, it was widely used to successfully model Be stars Silaj et al, 2010;Touhami et al, 2011;Carciofi et al, 2012;Klement et al, 2015;Vieira et al, 2015;Faes et al, 2016;Arcos et al, 2017;Jones et al, 2017;Klement et al, 2017;Vieira et al, 2017;Marr et al, 2018;Rímulo et al, 2018). More details about the VDD model can be found in Sect.…”

Section: The Disks Of Be Starsmentioning

confidence: 99%

A Multi-technique Study of the Dynamical Evolution of the Viscous Disk around the Be Star CMa

Ghoreyshi

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The observed emission lines of Be stars originate from a circumstellar Keplerian disk that are generally well explained by the Viscous Decretion Disk model. In an earlier work we performed the modeling of the full light curve of the bright Be star ω CMa (Ghoreyshi et al. 2018) with the 1-D time-dependent hydrodynamics code SINGLEBE and the Monte Carlo radiative-transfer code HDUST. We used the V-band light curve that probes the inner disk through four disk formation and dissipation cycles. This new study compares predictions of the same set of model parameters with time-resolved photometry from the near UV through the mid-infrared, comprehensive series of optical spectra, and optical broad-band polarimetry, that overall represent a larger volume of the disk. Qualitatively, the models reproduce the trends in the observed data due to the growth and decay of the disk. However, quantitative differences exist, e.g., an overprediction of the flux increasing with wavelength, too slow decreases in Balmer emission-line strength that are too slow during disk dissipation, and the discrepancy between the range of polarimetric data and the model. We find that a larger value of the viscosity parameter alone, or a truncated disk by a companion star, reduces these discrepancies by increasing the dissipation rate in the outer regions of the disk.

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Evidence for Different Disk Mass Distributions between Early- and Late-type Be Stars in the BeSOS Survey

Cited by 34 publications

References 53 publications

Stellar parameters and H α line profile variability of Be stars in the BeSOS survey

Stellar parameters and H α line profile variability of Be stars in the BeSOS survey

The Disk Physical Conditions of 48 Persei Constrained by Contemporaneous Hα Spectroscopy and Interferometry

A Multi-technique Study of the Dynamical Evolution of the Viscous Disk around the Be Star CMa

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