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Optical spectroscopy of Galactic field classical Be stars

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dc.contributor.author Banerjee, G
dc.contributor.author Mathew, B
dc.contributor.author Paul, K. T
dc.contributor.author Subramaniam, A
dc.contributor.author Bhattacharyya, S
dc.contributor.author Anusha, R
dc.date.accessioned 2021-02-14T06:04:24Z
dc.date.available 2021-02-14T06:04:24Z
dc.date.issued 2021-01
dc.identifier.citation Monthly Notices of the Royal Astronomical Society, Vol. 500, No. 3, pp. 3926-3943 en_US
dc.identifier.issn 1365-2966
dc.identifier.uri http://hdl.handle.net/2248/7631
dc.description Restricted Access © The Royal Astronomical Society https://doi.org/10.1093/mnras/staa3469 en_US
dc.description.abstract In this study, we analyse the emission lines of different species present in 118 Galactic field classical Be stars in the wavelength range of 3800–9000 Å. We re-estimated the extinction parameter (AV) for our sample stars using the newly available data from Gaia DR2 and suggest that it is important to consider AV while measuring the Balmer decrement (i.e. D34 and D54) values in classical Be stars. Subsequently, we estimated the Balmer decrement values for 105 program stars and found that ≈20 per cent of them show D34 ≥ 2.7, implying that their circumstellar disc are generally optically thick in nature. One program star, HD 60855 shows H α in absorption – indicative of disc-less phase. From our analysis, we found that in classical Be stars, H α emission equivalent width values are mostly lower than 40 Å, which agrees with that present in literature. Moreover, we noticed that a threshold value of ∼10 Å of H α emission equivalent width is necessary for Fe II emission to become visible. We also observed that emission line equivalent widths of H α, P14, Fe II 5169, and O I 8446 Å for our program stars tend to be more intense in earlier spectral types, peaking mostly near B1-B2. Furthermore, we explored various formation regions of Ca II emission lines around the circumstellar disc of classical Be stars. We suggest the possibility that Ca II triplet emission can originate either in the circumbinary disc or from the cooler outer regions of the disc, which might not be isothermal in nature. en_US
dc.language.iso en en_US
dc.publisher Oxford University Press on behalf of the Royal Astronomical Society en_US
dc.subject techniques: spectroscopic en_US
dc.subject stars: emission-line en_US
dc.subject Be en_US
dc.subject circumstellar matter en_US
dc.title Optical spectroscopy of Galactic field classical Be stars en_US
dc.type Article en_US

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