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

Brandi, E.; Mikołajewska, Joanna; Quiroga, C.; Belczyński, Krzysztof; Ferrer, O. E.; García, Lía Guillermina; Pereira, C. B.

doi:10.1051/0004-6361:20042552

Cited by 22 publications

(23 citation statements)

References 23 publications

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“…Having determined our orbit for the M giant, we examined our 22 KPNO spectra of the 1 μm region, which have both H I Paschen δ and He II emission lines. Neither show the very strong wings that are seen in the profiles of Hα and to a lesser extent the He II 4686 Å line (Quiroga et al 2002;Brandi et al 2005). However, many of the Paschen δ emission profiles of SS 73-96 have well defined, double peaked structure, resembling profiles seen for Hα in other symbiotics as noted previously.…”

Section: Emission Line Spectrummentioning

confidence: 59%

“…Mikołajewska et al (1989) stated that the He II emission should follow the orbit of the hot component. Additional analyses by Quiroga et al (2002) and Brandi et al (2005), who measured a variety of emission lines in the 4000-7300 Å range, found that the wings of the Hα, Hβ, and He II lines do seem to follow the hot component. The Hα profiles of several symbiotics, including FG Ser, AR Pav, and FN Sgr, show a double peaked emission feature that has central absorption (Mürset et al 2000;Quiroga et al 2002;Brandi et al 2005).…”

Section: Spectroscopic Orbitmentioning

confidence: 97%

“…Additional analyses by Quiroga et al (2002) and Brandi et al (2005), who measured a variety of emission lines in the 4000-7300 Å range, found that the wings of the Hα, Hβ, and He II lines do seem to follow the hot component. The Hα profiles of several symbiotics, including FG Ser, AR Pav, and FN Sgr, show a double peaked emission feature that has central absorption (Mürset et al 2000;Quiroga et al 2002;Brandi et al 2005). Attempts to model the emission (e.g., Robinson et al 1994) have been mostly unsatisfactory, and there is no agreement yet as to whether the Hα emission comes from an accretion disk around the white dwarf companion or results from an extended wind from the giant .…”

Section: Spectroscopic Orbitmentioning

confidence: 97%

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Infrared Spectroscopy of Symbiotic Stars. X. Orbits for Three S-Type Systems: V1044 Centauri, Hen 3-1213, and Ss 73-96

Fekel

Hinkle

Wood

2015

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Employing new infrared radial velocities, we have computed orbits of the cool giants in three southern S-type symbiotic systems. The orbit for V1044 Cen, an M5.5 giant, has a period of 985 days and a modest eccentricity of 0.16. Hen 3-1213 is a K4 giant, yellow symbiotic with an orbital period of 533 days and a similar eccentricity of 0.18. For the M2 giant SS 73-96 the orbital period is 828 days, and this system has a somewhat larger eccentricity of 0.26. Measurement of the H I Paschen δ emission lines, which may at least partially reflect the motion of the secondary in SS 73-96, results in a mass ratio of 2.4 for the M giant relative to the presumed white dwarf. The estimated orbital inclinations of V1044 Cen and Hen 3-1213 are low, about 40°. However, for SS 73-96 the predicted inclination is 90°, and so an ephemeris for eclipses of the secondary or the hot nebula surrounding it is provided. A search of the orbital velocity residuals of V1044 Cen and SS 73-96 for pulsation periods produced no realistic or convincing period for either star.

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Section: Emission Line Spectrummentioning

confidence: 59%

Section: Spectroscopic Orbitmentioning

confidence: 97%

Section: Spectroscopic Orbitmentioning

confidence: 97%

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Infrared Spectroscopy of Symbiotic Stars. X. Orbits for Three S-Type Systems: V1044 Centauri, Hen 3-1213, and Ss 73-96

Fekel

Hinkle

Wood

2015

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“…There exist a number of well-studied systems, which are double-eclipsing and, therefore, have inclinations above 70°, and where the giant being an AGB star is highly probable. Examples are V1329 Cyg (Schild and Schmid 1997;Pribulla et al 2003), with masses of 2:02 AE 0:41 M and 0:71 AE 0:09 M for the giant and hot compact stars, respectively, FN Sgr (Brandi et al 2005;Mikołajewska 2003) with 1:5 AE 0:2 M and 0:7 AE 0:08 M , and AR Pav (Quiroga et al 2002;Mikołajewska 2003) 2:5 AE 0:6 M and 1 AE 0:2 M . Mass determinations for these systems have much larger uncertainties than dynamical masses for other types of systems discussed above.…”

Section: Interacting Binariesmentioning

confidence: 99%

Weighing stars from birth to death: mass determination methods across the HRD

Serenelli

Weiß

Aerts

et al. 2021

Astron Astrophys Rev

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The mass of a star is the most fundamental parameter for its structure, evolution, and final fate. It is particularly important for any kind of stellar archaeology and characterization of exoplanets. There exist a variety of methods in astronomy to estimate or determine it. In this review we present a significant number of such methods, beginning with the most direct and model-independent approach using detached eclipsing binaries. We then move to more indirect and model-dependent methods, such as the quite commonly used isochrone or stellar track fitting. The arrival of quantitative asteroseismology has opened a completely new approach to determine stellar masses and to complement and improve the accuracy of other methods. We include methods for different evolutionary stages, from the pre-main sequence to evolved (super)giants and final remnants. For all methods uncertainties and restrictions will be discussed. We provide lists of altogether more than 200 benchmark stars with relative mass accuracies between ½0:3; 2% for the covered mass range of M 2 ½0:1; 16 M , 75% of which are stars burning hydrogen in their core and the other 25% covering all other evolved stages. We close with a recommendation how to combine various methods to arrive at a ''mass-ladder'' for stars.

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“…LCs of FN Sgr, Z And, AX Per of Brandi et al 2005;Leibowitz & Formiggini 2008 with signatures of a mass outflow (e.g., Fernández-Castro et al 1995;Esipov et al 2000;Sokoloski et al 2006;McKeever et al 2011). They are called 'Z And-type' outbursts, because they were observed in the past for a prototype of the class of symbiotic stars -Z And (Kenyon 1986).…”

Section: Introductionmentioning

confidence: 99%

Repeated Transient Jets from a Warped Disk in the Symbiotic Prototype Z And: A Link to the Long-lasting Active Phase

Skopal

Тарасова

Wolf

et al. 2018

ApJ

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Active phases of some symbiotic binaries survive for a long time from years to decades. The accretion process onto a white dwarf (WD) sustaining long-lasting activity, and sometimes leading to collimated ejection, is not well understood. We present the repeated emergence of highly collimated outflows (jets) from the symbiotic prototype Z And during its 2008 and 2009-10 outbursts and suggest their link to the current long-lasting (from 2000) active phase. We monitored Z And with the high-resolution spectroscopy, multicolor U BV R C -and high-time-resolution-photometry. The well-pronounced bipolar jets were ejected again during the 2009-10 outburst together with the simultaneous emergence of the rapid photometric variability (∆m ≈ 0.06 mag) on the timescale of hours, showing similar properties as those during the 2006 outburst. These phenomena and the measured disk-jets connection could be caused by the radiation-induced warping of the inner disk due to a significant increase of the burning WD luminosity. Ejection of transient jets by Z And around outburst maxima signals a transient accretion at rates above the upper limit of the stable hydrogen burning on the WD surface. The enhanced accretion through the disk warping, supplemented by the accretion from the giant's wind, can keep a high luminosity of the WD for a long time, until depletion of the disk. In this way, the jets provide a link to long-lasting active phases of Z And.

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

Cited by 22 publications

References 23 publications

Infrared Spectroscopy of Symbiotic Stars. X. Orbits for Three S-Type Systems: V1044 Centauri, Hen 3-1213, and Ss 73-96

Infrared Spectroscopy of Symbiotic Stars. X. Orbits for Three S-Type Systems: V1044 Centauri, Hen 3-1213, and Ss 73-96

Weighing stars from birth to death: mass determination methods across the HRD

Repeated Transient Jets from a Warped Disk in the Symbiotic Prototype Z And: A Link to the Long-lasting Active Phase

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