A Profile Analysis of Raman-Scattered O Vi Bands at 6825 Å and 7082 Å in Sanduleak’s Star

Heo, Jeong Eun; Angeloni, R.; Mille, F. Di; Palma, Tali; Lee, Hee Won

doi:10.3847/1538-4357/833/2/286

Cited by 12 publications

(17 citation statements)

References 34 publications

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“…Many Raman scattered O vi features show double or triple peak profiles. Lee & Kang (2007) undertook profile analyses of the two symbiotic stars V1016 Cygni and HM Sagittae to show that the double peak profiles in these objects are well fit by adopting a Keplerian accretion disk around the hot white dwarf component (see also Heo & Lee 2015;Heo et al 2016). The fitted profiles are consistent with the O vi emission region in Keplerian motion with ∼ 50 km s −1 implying the physical dimension of the accretion disk ≤ 1 au.…”

Section: Introductionmentioning

confidence: 88%

Stellar-wind accretion and Raman-scattered O vi features in the symbiotic star AG Draconis

Lee

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present high resolution spectroscopy of the yellow symbiotic star AG Draconis with ESPaDOnS at the Canada-France-Hawaii Telescope. Our analysis is focused on the profiles of Raman scattered O vi features centered at 6825Å and 7082Å, which are formed through Raman scattering of O viλλ1032 and 1038 with atomic hydrogen. These features are found to exhibit double component profiles with conspicuously enhanced red parts. Assuming that the O vi emission region constitutes a part of the accretion flow around the white dwarf, Monte Carlo simulations for O vi line radiative transfer are performed to find that the overall profiles are well fit with the accretion flow azimuthally asymmetric with more matter on the entering side than on the opposite side. As the mass loss rate of the giant component is increased, we find that the flux ratio F (6825)/F (7082) of Raman 6825 and 7082 features decreases and that our observational data are consistent with a mass loss rateṀ ∼ 2 × 10 −7 M ⊙ yr −1 . We also find that additional bipolar components moving away with a speed ∼ 70 km s −1 provide considerably improved fit to the red wing parts of Raman features. The possibility that the two Raman profiles differ is briefly discussed in relation to the local variation of the O vi doublet flux ratio.

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Section: Introductionmentioning

confidence: 88%

Stellar-wind accretion and Raman-scattered O vi features in the symbiotic star AG Draconis

Lee

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Subsequent studies reveal that the Raman O VI features provide strong constraints on the kinematics of emission nebulae around the white dwarf and extend our understanding of the mass loss process in symbiotic systems (e.g. Heo et al 2016).…”

Section: Raman O VI Features and Accretion Flowmentioning

confidence: 55%

MIKE High Resolution Spectroscopy of Raman-scattered O VI and C II Lines in the Symbiotic Nova RR Telescopii

et al. 2018

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We present a high-resolution optical spectrum of the symbiotic nova RR Tel obtained with MIKE at Magellan-Clay telescope. RR Tel is a wide binary system of a hot white dwarf and a Mira with an orbital period of a few decades, where the white dwarf is accreting through gravitational capture of some fraction of material shed by the Mira. We find broad emission features at 6825, 7082, 7023, and 7053 Å, which are formed through Raman scattering of far-UV O VI ⋋⋋ 1032 and 1038 Å, C II ⋋⋋ 1036 and 1037 Å with atomic hydrogen. Raman O VI features exhibit clear double-peak profiles indicative of an accretion flow with a characteristic speed ∼ 30 km s−1, whereas the Raman C II features have a single Gaussian profile. We perform a profile analysis of the Raman O VI by assuming that O VI emission traces the accretion flow around the white dwarf with a fiducial scale of 1 AU. A comparison of the restored fluxes of C II ⋋⋋ 1036 and 1037 from Raman C II features with the observed C II ⋋ 1335 multiplet is consistent with the distance of RR Tel ∼ 2.6 kpc based on interstellar extinction of C II.

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“…In particular, a small sample of SySts with known Raman OVI bands have been observed in order to characterize the sensitivity of our method to Raman OVI emission of different intensities against different types of local continua. An example of GMOS-S/RAMSES II images of Sanduleak's star (Heo et al 2016), a SySt in the Large Magellanic Cloud, is shown in Fig. 1.…”

Section: Early Results From the Filter Acceptance Test At Gemini-southmentioning

confidence: 99%

RAMSES II Raman Search for Extragalactic Symbiotic Stars

Angeloni¹,

Gonçalves

Díaz

et al. 2018

Proc. IAU

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Symbiotic stars (SySts) are long-period interacting binaries composed of a hot compact star, an evolved giant star, and a tangled network of gas and dust nebulae. Presently, we know 252 SySts in the Milky Way and 62 in external galaxies. However, these numbers are still in striking contrast with the predicted population of SySts in our Galaxy. In this contribution, I present the concept and the early results from RAMSES II (Raman Search for Extragalactic Symbiotic Stars), a Gemini/GMOS Upgrade Project which makes use of the Raman OVI 6830Å band as a powerful photometric tool to identify new SySts, within and beyond the Galaxy.

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A Profile Analysis of Raman-Scattered O Vi Bands at 6825 Å and 7082 Å in Sanduleak’s Star

Cited by 12 publications

References 34 publications

Stellar-wind accretion and Raman-scattered O vi features in the symbiotic star AG Draconis

Stellar-wind accretion and Raman-scattered O vi features in the symbiotic star AG Draconis

MIKE High Resolution Spectroscopy of Raman-scattered O VI and C II Lines in the Symbiotic Nova RR Telescopii

RAMSES II Raman Search for Extragalactic Symbiotic Stars

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