A photometric study of the eclipsing symbiotic binary AR Pavonis

Skopal, A.; Djurašević, G.; Jones, A. F.; Drechsel, H.; Rovithis‐Livaniou, H.; Rovithis, P.

doi:10.1046/j.1365-8711.2000.03040.x

Cited by 14 publications

(36 citation statements)

References 16 publications

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“…The error in the distance (Table 3) is again dominated by the uncertainty of the red giant radius R c . The above distance is in good agreement with previous estimates which range from 3.8 kpc to 5.8 kpc (Thackeray & Hutchings 1974;Kenyon & Webbink 1984;Skopal et al 2000).…”

Section: Luminosity Mass and Distancesupporting

confidence: 93%

“…It is indeed quite instructive to see that only direct observations of the stellar absorbtion features of the M star enable a proper interpretion of emission line radial velocities. An even higher mass for the hot companion was suggested by Skopal et al (2000), working with the same mass function as Thackeray & Hutchings (1974). They assumed that the system undergoes Roche lobe overflow.…”

Section: Discussionmentioning

confidence: 99%

“…The same mass function was adopted by Skopal et al (2000) when they analysed the 1889-1998 light curve to arrive at M hot = 4.5 M , M cool = 1.8 M . Thackeray & Hutchings (1974) do find less clear velocity patterns in Fig.…”

Section: Introductionmentioning

confidence: 99%

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High resolution spectroscopy of symbiotic stars

Schild

Dumm

Mürset

et al. 2001

A&A

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Abstract. We present new dynamical parameters of the AR Pav binary system. Our observations consist of a series of high resolution optical/NIR spectra from which we derive the radial velocity curve of the red giant as well as its rotation velocity. Assuming co-rotation, we determine the stellar radius (130 R ) of the red giant. Based on this we derive the red giant's luminosity and mass (2.0 M ) as well as the distance of the system (4.9 kpc). The binary mass function finally yields the companion's mass (0.75 M ) and the binary separation (1.95 AU). We find that the red giant does not fill its Roche lobe. We review the radial velocity data of Thackeray & Hutchings (1974), and compare it with our red giant's orbit. We find that their RV curves of the blue absorption system and the permitted emission lines are in anti-phase with the red giant, and that the forbidden emission lines are shifted by a quarter of a period. The blue absorptions and the permitted emission lines are associated with the hot companion but not in a straightforward way. The blue absorption system only tracks the hot component's orbital motion whilst it is in front of the red giant, whereas at other phases line blanketing by interbinary material leads to perturbations. We finally present UV light curves based on IUE archive spectra. We clearly detect eclipses in the continuum at all wavelengths. The eclipse light curves are unusual in that they show a slow and gradual decline prior to eclipse which is followed by a sharp increase after eclipse.

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Section: Luminosity Mass and Distancesupporting

confidence: 93%

Section: Discussionmentioning

confidence: 99%

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High resolution spectroscopy of symbiotic stars

Schild

Dumm

Mürset

et al. 2001

A&A

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“…These values are much lower than the radius of the eclipsed object, R h,ecl ∼ 0.1 A (46 R ), derived from optical eclipses (Skopal et al 2000a;Andrews 1974). Unfortunately, our method does not allow to measure accurately the wing positions for b < ∼ 6Å because of the presence of strong central absorption.…”

Section: The M Giant the Hot Companion And The Geometry Of Ar Pav Symentioning

confidence: 74%

“…They suggested variations in the mass transfer rate from the red giant to the hot component as the most satisfying explanation. Skopal et al (2000a) noted that the AR Pav light curve has a characteristic shape similar to those of dwarf novae in quiescent phase; whereas during the active phases the profile of the light curve changes considerably.…”

Section: Introductionmentioning

confidence: 97%

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

Quiroga

Mikołajewska

Brandi

et al. 2002

A&A

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Abstract. We analyze optical and near infrared spectra of intermediate and high resolution of the eclipsing symbiotic system AR Pavonis. We have obtained the radial velocity curves for the red and the hot component from the M-giant absorption lines and from the wings of Hα, Hβ and He II λ4686 emission profiles, respectively. From the orbital elements we have derived the masses, Mg = 2.5 M and M h = 1.0 M , for the red giant and the hot component, respectively. We also present and discuss radial velocity patterns in the blue cF absorption spectrum as well as various emission lines. In particular, we confirm that the blue absorption lines are associated with the hot component. The radial velocity curve of the blue absorption system, however, does not track the hot companion's orbital motion in a straightforward way, and its departures from an expected circular orbit are particularly strong when the hot component is active. We suggest that the cF-type absorption system is formed in material streaming from the giant presumably in a region where the stream encounters an accretion disk or an extended envelope around the hot component. The broad emission wings originate from the inner accretion disk or the envelope around the hot star. We also suggest that the central absorption in H profiles is formed in a neutral portion of the cool giant's wind which is strongly concentrated towards the orbital plane. The nebula in AR Pav seems to be bounded by significant amount of neutral material in the orbital plane. The forbidden emission lines are probably formed in low density ionized regions extended in polar directions and/or the wind-wind interaction zone.

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Recent photometry of symbiotic stars

Skopal¹,

Vaňko

Pribulla

et al. 2007

Astron Nachr

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We present new photometric observations of 15 symbiotic stars covering their last orbital cycle(s) from 2003.9 to 2007.2. We obtained our data by both classical photoelectric and CCD photometry. Main results are: EG And brightened by ∼0.3 mag in U from 2003. A ∼0.5 mag deep primary minimum developed in the U light curve (LC) at the end of 2006. ZAnd continues its recent activity that began during the 2000 autumn. A new small outburst started in summer of 2004 with a peak U magnitude of ∼ 9.2. During the spring of 2006 the star entered a massive outburst. It reached its historical maximum at U ∼ 8.0 in 2006 July. AEAra erupted in 2006 February with Δmvis ∼ 1.2 mag. BF Cyg entered a new active stage in 2006 August. A brightness maximum (U ∼ 9.4) was measured during 2006 September. CH Cyg persists in a quiescent phase. During 2006 June–December a ∼ 2 mag decline in all colours was measured. CI Cyg started a new active phase during 2006 May–June. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

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A photometric study of the eclipsing symbiotic binary AR Pavonis

Cited by 14 publications

References 16 publications

High resolution spectroscopy of symbiotic stars

High resolution spectroscopy of symbiotic stars

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

Recent photometry of symbiotic stars

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