The O I] 1641 Å line as a probe of symbiotic star winds

Shore, Steven N.; Wahlgren, G. M.

doi:10.1051/0004-6361/201014271

Cited by 8 publications

(7 citation statements)

References 35 publications

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“…The phasing of the radial velocity for O I 7774 Å vs 8446 Å points to the latter arising mainly at the L1 point on the A star. Its presence as an emission line can be explained by Lyβ fluorescent excitation of the resonance transition at 1025 Å (e.g., Keenan & Hynek 1950), on exposure of the substellar point to the accretion disk (a Grotrian diagram is shown in Shore & Wahlgren 2010). This is the only line in the optical spectrum with these particular properties.…”

Section: Wind Velocitymentioning

confidence: 98%

An optical spectroscopic and polarimetric study of the microquasar binary system SS 433

Picchi

Shore

Harvey

et al. 2020

A&A

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Aims. Our aim is to study the mass transfer, accretion environment, and wind outflows in the SS 433 system, concentrating on the so-called stationary lines. Methods. We used archival high-resolution (X-shooter) and low-resolution (EMMI) optical spectra, new optical multi-filter polarimetry, and low-resolution optical spectra (Liverpool Telescope), spanning an interval of a decade and a broad range of precessional and orbital phases, to derive the dynamical properties of the system. Results. Using optical interstellar absorption lines and H I 21 cm profiles, we derive E(B − V) = 0.86 ± 0.10, with an upper limit of E(B − V) = 1.8 ± 0.1 based on optical Diffuse Interstellar Bands. We obtain revised values for the ultraviolet and U band polarizations and polarization angles (PA), based on a new calibrator star at nearly the same distance as SS 433 that corrects the published measurement and yields the same PA as the optical. The polarization wavelength dependence is consistent with optical-dominating electron scattering with a Rayleigh component in U and the UV filters. No significant phase modulation was found for PA while there is significant variability in the polarization level. We fortuitously caught a flare event; no polarization changes were observed but we confirm the previously reported associated emission line variations. Studying profile modulation of multiple lines of H I, He I, O I, Na I, Si II, Ca II, Fe II with precessional and orbital phase, we derive properties for the accretion disk and present evidence for a strong disk wind, extending published results. Using transition-dependent systemic velocities, we probe the velocity gradient of the wind, and demonstrate that it is also variable on timescales unrelated to the orbit. Using the rotational velocity, around 140 ± 20 km s−1, a redetermined mass ratio q = 0.37 ± 0.04, and masses MX = 4.2 ± 0.4 M⊙, MA = 11.3 ± 0.6 M⊙, the radius of the A star fills – or slightly overfills – its Roche surface. We devote particular attention to the O I 7772 Å and 8446 Å lines, finding that they show different but related orbital and precessional modulation and there is no evidence for a circumbinary component. The spectral line profile variability can, in general, be understood with an ionization stratified outflow predicted by thermal wind modeling, modulated by different lines of sight through the disk produced by its precession. The wind can also account for an extended equatorial structure detected at long wavelength.

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Section: Wind Velocitymentioning

confidence: 98%

An optical spectroscopic and polarimetric study of the microquasar binary system SS 433

Picchi

Shore

Harvey

et al. 2020

A&A

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“…In contrast, 5577Å is fed from the intercombination 2324Å transition and has a much lower branching ratio from the 3 3 S o 1 state than 1641Å (see Fig. 1 in Shore & Wahlgren (2010)). By Day 99, we know that O I 1304Å emission was extremely weak and O o was a minor species, but the O I 1025Å line could also be pumped by Lyβ throughout the ejecta, leading to 6300Å emission.…”

Section: Contemporary Ultraviolet and Optical Spectroscopic Developme...mentioning

confidence: 99%

The panchromatic spectroscopic evolution of the classical CO nova V339 Delphini (Nova Del 2013) until X-ray turnoff

Shore

Mason

Schwarz

et al. 2016

A&A

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Context. Classical novae are the product of thermonuclear runaway-initiated explosions occurring on accreting white dwarfs. Aims. V339 Del (Nova Delphinus 2013) was one of the brightest classical novae of the last hundred years. Spectroscopy and photometry are available from γ-rays through infrared at stages that have frequently not been observed well. The complete data set is intended to provide a benchmark for comparison with modeling and for understanding more sparsely monitored historical classical and recurrent novae. This paper is the first in the series of reports on the development of the nova. We report here on the early stages of the outburst, through the X-ray active stage. Methods. A time sequence of optical, flux calibrated high resolution spectra was obtained with the Nordic Optical Telescope (NOT) using FIES simultaneously, or contemporaneously, with the Space Telescope Imaging Spectrograph (STIS) aboard the Hubble Space Telescope during the early stages of the outburst. These were supplemented with Mercator/HERMES optical spectra. High resolution IUE ultraviolet spectra of OS And 1986, taken during the Fe curtain phase, served as a template for the distance determination. We used standard plasma diagnostics (e.g., [O III] and [N II] line ratios, and the Hβ line flux) to constrain electron densities and temperatures of the ejecta. Using Monte Carlo modeling of the ejecta, we derived the structure, filling factor, and mass from comparisons of the optical and ultraviolet line profiles. Results. We derive an extinction of E(B − V) = 0.23 ± 0.05 from the spectral energy distribution, the interstellar absorption, and H I emission lines. The distance, about 4−4.5 kpc, is in agreement with the inferred distance from near infrared interferometry. The maximum velocity was about 2500 km s −1 , measured from the UV resonance and optical profiles. The ejecta showed considerable fine structure in all transitions, much of which persisted as emission knots. The line profiles were modeled using a bipolar conical structure for the ejecta within a relatively restricted range of parameters. For V339 Del, we find that an inclination to the line of sight of about 35• −55• , an opening angle of 60 • −80• , and an inner radius ∆R/R(t) ≈ 0.3 based on v rad,max matches the permitted and intercombination lines. The filling factor is f ≈ 0.1, and the derived range in the ejecta mass is (2−3) × 10 −5 M .

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“…Adopting Ṁwd ≈ (R 2 wd /4a 2 ) Ṁg , a typical white dwarf radius, and the measured a yields Ṁwd ≈ 10 −17 M yr −1 . Thus, substantial gravitational focusing is necessary (see also Shore & Wahlgren 2010;Shagatova et al 2016).…”

Section: Disk Accretionmentioning

confidence: 99%

Eg Andromedae: A New Orbit and Additional Evidence for a Photoionized Wind

Kenyon

Garcia²

2016

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We analyze a roughly 20 yr set of spectroscopic observations for the symbiotic binary EG And. Radial velocities derived from echelle spectra are best-fit with a circular orbit having orbital period P = 483.3 ± 1.6 d and semi-amplitude K = 7.34 ± 0.07 km s −1 . Combined with previous data, these observations rule out an elliptical orbit at the 10σ level. Equivalent widths of H I Balmer emission lines and various absorption features vary in phase with the orbital period. Relative to the radius of the red giant primary, the apparent size of the H II region is consistent with a model where a hot secondary star with effective temperature T h ≈ 75,000 K ionizes the wind from the red giant.

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The O I] 1641 Å line as a probe of symbiotic star winds

Cited by 8 publications

References 35 publications

An optical spectroscopic and polarimetric study of the microquasar binary system SS 433

An optical spectroscopic and polarimetric study of the microquasar binary system SS 433

The panchromatic spectroscopic evolution of the classical CO nova V339 Delphini (Nova Del 2013) until X-ray turnoff

Eg Andromedae: A New Orbit and Additional Evidence for a Photoionized Wind

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