The spectroscopic orbits and the geometrical configuration of the symbiotic binary AR Pavonis

Quiroga, C.; Mikołajewska, Joanna; Brandi, E.; Ferrer, O. E.; García, Lía Guillermina

doi:10.1051/0004-6361:20020335

Cited by 30 publications

(49 citation statements)

References 34 publications

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“…A similar result was obtained for AR Pav, in which the eccentricity apparently increases with the hot component activity (Quiroga et al 2002). Moreover, in both FN Sgr and AR Pav the periastron longitude of the elliptical orbit solution for the hot component is near 270…”

Section: Spectroscopic Orbitssupporting

confidence: 82%

“…In this way we have applied the same method that Schneider & Young (1980) and Shafter (1983) succesfuly used in studies of cataclysmic binaries (for more details about the application of this method to symbiotic binaries, see Quiroga et al 2002). However, the Balmer line wings are at times affected by a mixture of Raman and Rayleigh scattering (Jung & Lee 2004) and it is therefore not clear if they are associated with the hot component motion.…”

Section: Spectroscopic Orbitsmentioning

confidence: 99%

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The spectroscopic orbits and other parameters of the symbiotic binary FN Sgr

Brandi

Mikołajewska

Quiroga

et al. 2005

A&A

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Abstract. We present a study of the eclipsing symbiotic binary FN Sgr with a period of 568.3 days determined photometrically and confirmed spectroscopically. The hot component underwent a 2.5 mag eruption covered by most of our spectroscopic observations. In particular, we have determined for the first time spectroscopic orbits based on the radial velocity curves for both components. A set of blue absorption lines resembling an A-F type star is present in all our spectra and they seem to be associated with the hot component. Based on the light curve, we derive the red giant's radius (140 R ) and the orbital inclination (i = 80• ). We find that FN Sgr is similar to other S-type symbiotic binaries, composed by an M 5-type giant (M g = 1.5 M ) and a hot white dwarf (M h = 0.7 M , R h = 0.2 R ) with a binary separation of ∼1.6 AU. The red giant is just filling its Roche lobe and a geometrically and optically thick accretion disk is likely to be present around the low-mass accretor. The evolution of T h and L h along the active phase argues in favour of accretion disk instabilities similar to those of Z And. We have also studied spectral changes and photometric variations as a function of both the hot component activity and the orbital motion.

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Section: Spectroscopic Orbitssupporting

confidence: 82%

Section: Spectroscopic Orbitsmentioning

confidence: 99%

The spectroscopic orbits and other parameters of the symbiotic binary FN Sgr

Brandi

Mikołajewska

Quiroga

et al. 2005

A&A

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“…For V1507 Cyg (HD 187399) we did not find reports of ultraviolet emission lines, whereas AG Peg and AR Pav are symbiotic binaries (Yoo 2008, Quiroga et al 2002. Finally, HD 207739 shows variable ultraviolet emission and probably is a transition object (Kondo, McCluskey & Parsons 1985).…”

Section: W Serpentis Stars In the Literaturementioning

confidence: 59%

Interacting binaries W Serpentids and double periodic variables

Mennickent

Otero

Kołaczkowski

2015

Monthly Notices of the Royal Astronomical Society

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W Serpentids and Double Periodic Variables (DPVs) are candidates for close interacting binaries in a non-conservative evolutionary stage; while W Serpentids are defined by high-excitation ultraviolet emission lines present during most orbital phases, and by usually showing variable orbital periods, DPVs are characterized by a long photometric cycle lasting roughly 33 times the (practically constant) orbital period. We report the discovery of 7 new Galactic DPVs, increasing the number of known DPVs in our Galaxy by 50%. We find that DPVs are tangential-impact systems, i.e. their primaries have radii barely larger than the critical Lubow-Shu radius. These systems are expected to show transient discs, but we find that they host stable discs with radii smaller than the tidal radius. Among tangential-impact systems including DPVs and semi-detached Algols, only DPVs have primaries with masses between 7 and 10 M . We find that DPVs are in a Case-B mass transfer stage with donor masses between 1 and 2 M and with primaries resembling Be stars. W Serpentids are impact and non-impact systems, their discs extend until the last non-intersecting orbit and show a larger range of stellar mass and mass ratio than DPVs. Infrared photometry reveals significant color excesses in many DPVs and W Serpentids, usually larger for the latter ones, suggesting variable amounts of circumstellar matter.

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“…For this we have used the method outlined by Schneider & Young (1980, for more details see Quiroga et al 2002). This method consists of convolving the data with two identical Gaussian bandpasses whose centers have a separation of 2b with standard deviation σ.…”

Section: Spectroscopic Orbitsmentioning

confidence: 99%

“…Mikołajewska & Kenyon (1996) failed to derive any radial velocity curve and orbital solution for the blue absorption system in Z And. In CI Cyg the radial velocities of the F-type absorption system suggest that their formation region is the material streaming from the giant near the hot component (Mikołajewska & Mikołajewski 1988), whereas a possible correlation between AR Pav's activity and the departures of the cF absorption velocities from the circular orbit suggests that this absorption system also may be affected by material streaming towards the hot component, presumably in a region where the stream encounters an accretion disk or an extended envelope around the hot component (Quiroga et al 2002). We can see in Fig.…”

Section: Spectroscopic Orbitsmentioning

confidence: 99%

Spectroscopic orbits and variations of RS Ophiuchi

Brandi

Quiroga

Mikołajewska³

et al. 2009

A&A

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110

138

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Aims. The aims of our study are to improve the orbital elements of the giant and to derive the spectroscopic orbit for the white dwarf companion of the symbiotic system RS Oph. Spectral variations related to the 2006 outburst are also studied. Methods. We performed an analysis of about seventy optical and near infrared spectra of RS Oph that were acquired between 1998 and June 2008. The spectroscopic orbits were obtained by measuring the radial velocities of the cool component absorption lines and the broad Hα emission wings, which seem to be associated with the hot component. A set of cF-type absorption lines were also analyzed for a possible connection with the hot component motion. We also confirm the presence of the Li I doublet in RS Oph and its radial velocities fit very well to the M-giant radial velocity curve. Regardless of the mechanism involved to produce lithium, its origin is most likely from within the cool giant rather than material captured by the giant at the time of the nova explosion. The quiescent spectra reveal a correlation of the H I and He I emission line fluxes with the monochromatic magnitudes at 4800 Å, indicating that the hot component activity is responsible for those flux variations. We also discuss the spectral characteristics around 54-55 and 240 days after the 2006 outburst. In April 2006 most of the emission lines present a broad pedestal with a strong and narrow component at about −20 km s −1 and two other extended emission components at −200 and +150 km s −1 . These components could originate in a bipolar gas outflow supporting the model of a bipolar shock-heated shell expanding through the cool component wind perpendicularly to the binary orbital plane. Our observations also indicate that the cF absorption system was disrupted during the outburst, and restored about 240 days after the outburst, which is consistent with the resumption of accretion.

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The spectroscopic orbits and the geometrical configuration of the symbiotic binary AR Pavonis

Cited by 30 publications

References 34 publications

The spectroscopic orbits and other parameters of the symbiotic binary FN Sgr

The spectroscopic orbits and other parameters of the symbiotic binary FN Sgr

Interacting binaries W Serpentids and double periodic variables

Spectroscopic orbits and variations of RS Ophiuchi

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