Discovery of a bipolar and highly variable mass outflow from the symbiotic binary StH<i>α</i>190

Munari, U.; Tomov, T.; Yudin, B. F.; Marrese, P. M.; Zwitter, T.; Gratton, R.; Bonanno, G.; Bruno, P.; Cali, Antonio; Claudi, R.; Cosentino, R.; Desidera, S.; Farisato, G.; Martorana, G.; Marino, G.; Rebeschini, M.; Scuderi, S.; Timpanaro, M. C.

doi:10.1051/0004-6361:20010210

Cited by 18 publications

(22 citation statements)

References 9 publications

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“…Stephenson (1986) discovered StHα 190 at V ∼ 10.5, Robertson & Jordan (1989) re-discovered it (as RJHα 120) at V ∼ 10.1 and Downes & Keyes (1988) measured it at V = 10.5. Thus over the last 15 years the system mean brightness has remained fairly constant, and similarly went for the optical spectra very similar one to the other (Downes & Keyes 1988;Whitelock et al 1995;Munari & Zwitter 2001), with no report of outbursts. Variability has been instead firmly established in the infrared by Whitelock et al (1995) who reported ∆K = 0.16.…”

Section: V471supporting

confidence: 77%

“…In the GCVS it is reported as a long period variable varying between 14.4 ≤ B ≤ 13.1. Kenyon (1986) suggested its possible symbiotic nature but Bond (1978) and Munari & Zwitter (2001) UU Her. After the initial discovery by Reinmuth (1926) reporting the object to vary between 16.0 ≤ m pg ≤ 14.6, not much else has appeared in literature.…”

Section: V471mentioning

confidence: 99%

“…Variability has been instead firmly established in the infrared by Whitelock et al (1995) who reported ∆K = 0.16. Munari et al (2001b) have recently discovered a fast evolving and complex mixture of spectral signatures produced by high variable bipolar jets and PCyg profiles, with indication of a high orbital inclination and a possible 171 day orbital period. Therefore, searches for flickering and eclipses in the bluest photometric bands could pay dividends over a single observing season.…”

Section: V471mentioning

confidence: 99%

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${\vec{UBV(RI)}}_{\rm C}$ photometric comparison sequences for symbiotic stars. II.

Henden

Munari

2001

A&A

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Section: V471supporting

confidence: 77%

Section: V471mentioning

confidence: 99%

Section: V471mentioning

confidence: 99%

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${\vec{UBV(RI)}}_{\rm C}$ photometric comparison sequences for symbiotic stars. II.

Henden

Munari

2001

A&A

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“…Our spectroscopic monitoring of BF Cyg revealed for the first time the emergence of satellite-emission components to the Hα and Hβ emission lines from 2009. To date, similar emissions in the optical spectra of symbiotic stars have only been discovered for Hen 3-1341 (Tomov et al 2000), StHα 190 (Munari et al 2001), and Z And (Skopal & Pribulla 2006), although a few jets have been discovered by other methods. In this contribution we present the evolution of these jet features from their emergence in 2009 to 2012 and determine their basic parameters.…”

Section: Introductionmentioning

confidence: 90%

Discovery of collimated ejection from the symbiotic binary BF Cygni

Skopal

Tomov

Tomova

2013

A&A

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Context. Detection of collimated ejection from white dwarfs (WD) in symbiotic binaries is very rare and has employed a variety of methods in X-ray, radio, optical imagery, and spectroscopy. To date, its signature in the optical spectra has only been recorded for four objects (MWC 560, Hen 3-1341, StHα 190, and Z And). Aims. We present the first observational evidence of highly-collimated bipolar ejection from the symbiotic binary BF Cyg, which developed during its current (2006-12) active phase, and determine their physical parameters. Methods. We monitored the outburst with the optical high-resolution spectroscopy and multicolour UBVR C I C photometry. Results. During 2009, three years after the 2006-eruption of BF Cyg, satellite components to Hα and Hβ lines emerged in the spectrum. During 2012, they became stable and were located symmetrically with respect to the main emission core of the line. Spectral properties of these components suggest bipolar ejection collimated within an opening angle of < ∼ 15• , whose radiation is produced by an optically thin medium with the emission measure of 1−2 × 10 59 (d/3.8 kpc) 2 cm −3 . Conclusions. Formation of the collimated ejection a few years after the eruption and its evolution on a time scale of years at a constant optical brightness can aid us in better understanding the accretion process during the active phases of symbiotic stars.

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“…In the past years several studies allowed the distinctive features of D' types to be highlighted: for instance, both Smith et al (2001) and Munari et al (2001) showed that these stars display enhancements of the s-process elements that are synthesised via slow neutron captures during stellar evolution along the asymptotic giant branch (AGB). Moreover, when measuring the rotational velocity of the cool star, Pereira et al (2005, hereafter P05) and Zamanov et al (2006, hereafter Z06), point out that in the D' type SS the cool component rotates faster than the isolated giants, at a substantial fraction of the critical velocity (e.g.…”

Section: Introductionmentioning

confidence: 99%

Gas and dust spectra of the D' type symbiotic star HD 330036

Angeloni

Contini

Ciroi

et al. 2007

A&A

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Aims. We present a comprehensive and self-consistent modelling of the D' type symbiotic star (SS) HD 330036 from radio to UV. Methods. Within a colliding-wind scenario, we analyse the continuum, line, and dust spectra by means of SUMA, a code that simulates the physical conditions of an emitting gaseous cloud under the coupled effect of ionisation from an external radiation source and shocks. Results. We find that the UV lines are emitted from high-density gas between thestars downstream of the reverse shock, while the optical lines are emitted downstream of the shock propagating outwards from the system. As regards the continuum SED, three shells are identified in the IR, at 850 K, 320 K, and 200 K with radii r = 2.8 × 10 13 cm, 4 × 10 14 cm, and 10 15 cm, respectively, after adopting a distance to Earth of d = 2.3 kpc. Interestingly, all these shells appear to be circumbinary. Analysis of the unexploited ISO-SWS spectrum reveals that both PAHs and crystalline silicates coexist in HD 330036, with PAHs associated to the internal shell at 850 K, and crystalline silicates stored in the cool shells at 320 K and 200 K. Strong evidence that crystalline silicates are shaped in a disk-like structure is derived on the basis of the relative band strengths. Finally, we suggest that shocks can be a reliable mechanism for activating the annealing and the consequent crystallisation processes. Conclusions. We show that a consistent interpretation of gas and dust spectra emitted by SS can be obtained by models that account for the coupled effect of the photoionising flux and of shocks. The VLTI/MIDI proposal recently accepted by ESO aims to verify and better constrain some of our results by means of IR interferometric observations.

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Discovery of a bipolar and highly variable mass outflow from the symbiotic binary StHα190

Cited by 18 publications

References 9 publications

${\vec{UBV(RI)}}_{\rm C}$ photometric comparison sequences for symbiotic stars. II.

${\vec{UBV(RI)}}_{\rm C}$ photometric comparison sequences for symbiotic stars. II.

Discovery of collimated ejection from the symbiotic binary BF Cygni

Gas and dust spectra of the D' type symbiotic star HD 330036

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