Orbital motion in symbiotic Mira systems

Schmid, Hans Martin; Schild, Hans H.

doi:10.1051/0004-6361:20021295

Cited by 25 publications

(19 citation statements)

References 15 publications

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“…Previous work by other researchers provides smaller binary separations and shorter binary periods. For example, Schmid & Schild (2002) performed spectropolarimetry to investigate the variation of the polarization direction, which is expected to vary owing to the orbital motion. Based on their polarimetric method, they proposed that the binary period may exceed 100 yr. Lee (2003) investigated the strength of the λ 6545 feature in V1016 Cyg and suggested the opening half angle θ s ≃ 60° adopting the distance estimate by Brocksopp et al (2002).…”

Section: Calculationsmentioning

confidence: 99%

Centre shift of the Raman scattered He iiλ 4850 in the symbiotic star V1016 Cygni

Jung

Lee

2004

Monthly Notices of the Royal Astronomical Society

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We present our spectroscopic data around Hβ of the symbiotic star V1016 Cyg obtained with the Bohyunsan Echelle Spectrograph, in order to secure the broad emission feature at around λ 4850, which is formed through Raman scattering of He II λ 972. The total cross-section around Lyγ is given approximately by σ (λ) 1.7 × 10 −28 [λ Lyγ /(λ − λ Lyγ )] 2 cm 2 , with λ Lyγ being the line centre wavelength of Lyγ . We find a centre shift redward by an amount λ = +0.64 Å in the Raman scattered He II λ 4850. This redward centre shift is exactly analogous to the effect for the Raman scattered He II λ 6545 blueward of Hα discussed in our previous study. We compute the branching ratios of Raman scattering into the level 2s and levels 3s and 3d, which are subsequently incorporated in our Monte Carlo code. Using this code, we present the centre shift of the 4850 feature as a function of the neutral hydrogen column density in the scattering region. Assuming that He II λ 972 emission is characterized by a single Gaussian profile, the redward peak shift observed in the Raman scattered He II λ 4850 feature corresponds to the neutral column density N H I = 1.2 × 10 21 cm −2 . Assuming that the covering factor ∼ 0.1 of the scattering region with respect to the He II emission region and adopting a simple spherical stellar wind model, we may place an upper boundṀ 3.6 × 10 −7 M yr −1 for the massloss rate of the giant component of V1016 Cyg. Our estimate can be severely affected by the kinematics of the scattering and He II emission regions and the exact atomic physics, about which brief discussions are presented.

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Section: Calculationsmentioning

confidence: 99%

Centre shift of the Raman scattered He iiλ 4850 in the symbiotic star V1016 Cygni

Jung

Lee

2004

Monthly Notices of the Royal Astronomical Society

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“…From their characteristics at infrared wavelengths, Webster & Allen (1975) separated the symbiotics into two subclasses, D for dusty-type and S for stellar-type systems. The S-type symbiotics have typical orbital periods of 2-3 yr, while those of the D-type systems are at least an order of magnitude longer (Schmid & Schild 2002). For a more extensive introduction to this group of stars see Fekel et al (2000b) and Mikołajewska (2003).…”

Section: Introductionmentioning

confidence: 99%

Infrared Spectroscopy of Symbiotic Stars. Viii. Orbits for Three S-Type Systems: Ae Arae, Y Coronae Australis, and Ss 73-147

Fekel

Hinkle

Wood

2010

The Astronomical Journal

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With new infrared radial velocities we have computed orbits of the M giants in three southern S-type symbiotic systems. AE Ara and SS 73-147 have circular orbits with periods of 803 and 820 days, respectively. The eccentric orbit of Y CrA has a period that is about twice as long, 1619 days. Except for CH Cyg it is currently the S-type symbiotic system with the longest period for which a spectroscopic orbit has been determined. The Paschen δ emission line velocities of AE Ara are nearly in antiphase with the M giant absorption feature velocities and result in a mass ratio of 2.7. Emission lines in the 1.005 μm region for the other two symbiotic systems are not good proxies for the hot components in those systems. There is no evidence that these three symbiotics are eclipsing. With spectral classes of M5.5 or M6, the three giants presumably also have velocity variations that result from pulsations, but we have been unable to identify specific pulsation periods in the absorption line velocity residuals.

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“…Brocksopp et al (2002) presented their Hubble Space Telescope (HST) image of V1016 Cyg to propose that the projected binary separation of 84±2 AU assuming the distance of 2 kpc. Schmid & Schild (2002) suggested an orbital period longer than a century from their monitoring of the position angle of the linear polarization of the Raman O vi 6825 feature. A photometric variation with a period of 15 years was proposed by Parimucha et al (2003), who attributed the activity to the orbital motion.…”

Section: High Resolution Spectroscopy Of V1016 Cygmentioning

confidence: 99%

ACCRETION FLOW AND DISPARATE PROFILES OF RAMAN SCATTERED O VI Λλ 1032, 1038 IN THE SYMBIOTIC STAR V1016 CYGNI

Heo¹,

Lee²

2015

Journal of The Korean Astronomical Society

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Abstract:The symbiotic star V1016 Cygni, a detached binary system consisting of a hot white dwarf and a mass-losing Mira variable, shows very broad emission features at around 6825Å and 7082Å, which are Raman scattered O vi λλ 1032, 1038 by atomic hydrogen. In the high resolution spectrum of V1016 Cyg obtained with the Bohyunsan Optical Echelle Spectrograph these broad features exhibit double peak profiles with the red peak stronger than the blue counterpart. However, their profiles differ in such a way that the blue peak of the 7082 feature is relatively weaker than the 6825 counterpart when the two Raman features are normalized to exhibit an equal red peak strength in the Doppler factor space. Assuming that an accretion flow around the white dwarf is responsible for the double peak profiles, we attribute this disparity in the profiles to the local variation of the flux ratio of O vi λλ 1032, 1038 in the accretion flow. A Monte Carlo technique is adopted to provide emissivity maps showing the local emissivity of O vi λ1032 and O vi λ1038 in the vicinity of the white dwarf. We also present a map indicating the differing flux ratios of O vi λλ 1032 and 1038. Our result shows that the flux ratio reaches its maximum of 2 in the emission region responsible for the central trough of the Raman feature and that the flux ratio in the inner red emission region is almost 1. The blue emission region and the outer red emission region exhibit an intermediate ratio around 1.5. We conclude that the disparity in the profiles of the two Raman O vi features strongly implies accretion flow around the white dwarf, which is azimuthally asymmetric.

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Orbital motion in symbiotic Mira systems

Cited by 25 publications

References 15 publications

Centre shift of the Raman scattered He iiλ 4850 in the symbiotic star V1016 Cygni

Centre shift of the Raman scattered He iiλ 4850 in the symbiotic star V1016 Cygni

Infrared Spectroscopy of Symbiotic Stars. Viii. Orbits for Three S-Type Systems: Ae Arae, Y Coronae Australis, and Ss 73-147

ACCRETION FLOW AND DISPARATE PROFILES OF RAMAN SCATTERED O VI Λλ 1032, 1038 IN THE SYMBIOTIC STAR V1016 CYGNI

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