Spectra of Individual Symbiotic Stars

Oliversen, N. A.; Anderson, Christopher M.

doi:10.1007/978-94-009-7834-8_9

Cited by 7 publications

(4 citation statements)

References 4 publications

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“…Therefore, Balmer lines tend to deviate from pure case B recombination; due to that, the derereddened Hα/Hβ ratio clearly disagrees from case B recombination. A similar effect is seen in symbiotic stars (Oliversen & Anderson 1982).…”

Section: Extinctionsupporting

confidence: 74%

Spectroscopic analysis of two peculiar emission-line stars: RJHA 49 and SS73 21

Pereira

Marcolino

Machado

et al. 2007

A&A

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Aims. We investigate the spectra and the evolutionary stages of two peculiar emission-line stars: RJHA 49 and SS73 21. Methods. We used low and high resolution optical data. Line identifications and measurements were performed for several features in their spectra.Results. For each object, we derived the extinction and the excitation temperature from a set of [Fe ii] lines and the electron density from [N ii] lines. For RJHA 49, no detailed spectroscopic study has been done so far. Our low resolution spectrum have confirmed the main characteristics found in previous works on SS73 21. On the other hand, from our high resolution data, we find that the Hα line presents a double peak, in contrast with the suggestion in the literature that it should reveal a P-Cygni profile. Surprisingly, we found a few He i transitions resembling P-Cygni profiles (e.g. He i λ5876), directly suggesting that mass loss is active in SS73 21. We also discuss the nature of these two objects based on data obtained. Although the evolutionary status of SS73 21 seems well established from previous studies (a proto-planetary nebula), the situation for RJHA 49 is not very clear mainly due to its unknown distance.However, from the strength of [N ii] λ5754 relative to [O i] λ6300, the possibility of RJHA 49 being a LBV object is reduced, and a B[e]-supergiant or a proto-planetary nebula status is more plausible.

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Section: Extinctionsupporting

confidence: 74%

Spectroscopic analysis of two peculiar emission-line stars: RJHA 49 and SS73 21

Pereira

Marcolino

Machado

et al. 2007

A&A

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“…Additional confirmation of the accuracy of the scans is provided by comparison with similar observations of the PN NGC 1535 and Vy 2-2 by Johnson (1976Johnson ( , 1977, who used the CTIO Fabry-Perot, and with the echelle spectra of V1016 Cyg and several of the symbiotic stars obtained by Anderson, Oliversen, and Nordsieck (1980), Anderson and Oliversen (1981), and Oliversen and Anderson (1982) at the University of Wisconsin's Pine Bluff Observatory. These comparisons will be made explicitly in the following sections.…”

Section: A Instrumentation and Data Reductionmentioning

confidence: 64%

“…Recently published studies of a number of individual symbiotic stars (referenced below) have revealed variations in the intensities and profiles of the Ha emission lines in those objects; high-resolution spectro-scopic monitoring of Ha (as well as other emission lines) should provide significant information as to the nature of the eruptive phenomena and as to whether these objects are single or binary stars. We present here only single examples of the Ha profiles for Z Andromedae, CH Cygni, and AG Pegasi (primarily for comparison with the profiles for V1016 Cyg and HM Sge), plus two profiles for the less-studied YY Herculis; we would refer to the extensive observations of Anderson et al (1980), Anderson andOliversen (1981), and Oliversen and Anderson (1982) for detailed consideration of the line profiles in a number of symbiotic stars. The great width of the Ha profiles of the symbiotic stars and the presence of a stronger continuum than is present for the PN lead to order overlapping and possible contamination from parasitic light, which may spuriously raise the line wings of some of the profiles presented here for the symbiotic stars (and for V1016 Cyg and HM Sge as well).…”

Section: B Symbiotic Starsmentioning

confidence: 99%

Emission-line profiles for selected planetary nebulae and symbiotic stars, V1016 Cygni, and HM Sagittae

Welty¹

1983

PASP

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“…The W's of those emission lines are expressed with respect to the bottom of the stellar absorption line, not to that outside continuum. Oliversen & Anderson (1981) remarked that the only emission lines present on their spectrograms were Hα and Hβ, but on some occasions they had completely disappeared, so it is possible that the spectrum has changed since Sanford's observations in 1943-1949. Oliversen & Anderson noted that, when present, the Hα main peak was accompanied by a small subsidiary peak roughly 50 km s −1 to the red.…”

Section: The Spectrum Of Uv Aur Amentioning

confidence: 99%

The Carbon Mira Uv Aurigae and Its Companion

Herbig¹

2009

The Astronomical Journal

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The carbon Mira UV Aur (photometric period 394 days) and its companion present several interesting spectroscopic issues. The late B-type companion, at a separation of 3. 36, is seen through at least two shells expanding from the C9-type primary, as evidenced by a series of narrow, displaced absorption features at the D 1,2 lines of Na i. The (projected) expansion velocity of the fastest shell is about 116 km s −1 , much larger than the typical outflow velocity of about 15 km s −1 seen in C-type giants, but reminiscent of the velocities observed in the envelope of another C-type Mira, V Hya. Emission lines of H, Ca ii, and Na i are present in UV Aur A; its Balmer emission lines are heavily mutilated by overlying C-type absorptions (much as is seen in Me-type Miras), so they must be formed at a lower level. UV Aur B offers the opportunity to test a speculation that the carriers of the diffuse interstellar bands (DIBs), believed to be a family of carbon-containing polyatomic molecules, may be formed in cool, carbon-rich stars. Moderately strong DIBs are indeed present in the spectrum of UV Aur B at about the same strength and velocity seen in nearby (in the sky) B-type stars. But the essential question is, are DIBs present in the outflow from UV Aur A, at the velocities of the Na i shell components? The answer is no, at least at the level permitted by the signal-to-noise ratio of these Keck/HIRES spectrograms.

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Spectra of Individual Symbiotic Stars

Cited by 7 publications

References 4 publications

Spectroscopic analysis of two peculiar emission-line stars: RJHA 49 and SS73 21

Spectroscopic analysis of two peculiar emission-line stars: RJHA 49 and SS73 21

Emission-line profiles for selected planetary nebulae and symbiotic stars, V1016 Cygni, and HM Sagittae

The Carbon Mira Uv Aurigae and Its Companion

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