Infrared Spectroscopy of Symbiotic Stars. III. First Orbits for Three S-Type Systems

Fekel, Francis C.; Hinkle, Kenneth H.; Joyce, R. R.; Skrutskie, Michael F.

doi:10.1086/319966

Cited by 39 publications

(56 citation statements)

References 33 publications

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“…In addition, the light minima of the 2007.9 and 2010.0 eclipses were shifted by about +20 days with respect to the spectroscopic conjunction of the giant according to the Fekel's et al (2001) ephemeris. The abnormally long-lasting high level of the BF Cyg brightness requires continuation of its photometric and spectroscopic monitoring.…”

Section: Bf Cygmentioning

confidence: 95%

Recent photometry of symbiotic stars

et al. 2012

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We present new multicolour (UBVRCIC) photometric observations of classical symbiotic stars, EG And, Z And, BF Cyg, CH Cyg, CI Cyg, V1329 Cyg, TX CVn, AG Dra, Draco C1, AG Peg, and AX Per, carried out between 2007.1 and 2011.9. The aim of this paper is to present new data of our monitoring programme, to describe the main features of their light curves (LC) and to point problems for their future investigation. The data were obtained by the method of the classical photoelectric and CCD photometry.

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Section: Bf Cygmentioning

confidence: 95%

Recent photometry of symbiotic stars

et al. 2012

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“…where R is in solar radii, v is the rotational velocity in km s-l, and P is the orbital period in days. With orbital elements from our published (Fekel et al 2000a,b;Fekel et al 2001) and unpublished results plus masses taken from the literature or in some cases canonical values of 1.5 and 0.5 Mev for the cool and hot components, respectively, the separation of the two stars follows from Kepler's third law. This leads to the computation of an effective Roche lobe radius from Eq.…”

Section: Measurements and Inferences About Mass Exchangementioning

confidence: 99%

Rotational Velocities of S-Type Symbiotic Stars

Fekel

Hinkle

Joyce

2004

Symp. - Int. Astron. Union

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Abstract. We obtained high-resolution spectroscopic observations at 2.226 J-Lm of 13 S-type symbiotic binaries using the Phoenix infrared spectrograph on Kitt Peak telescopes. From an empirical calibration we determined v sin i values for the giant components. Combined with information from a program to determine orbits, the rotational velocities have been used to estimate the sizes of these stars and the fraction of their Roche lobes that they fill. Measurements and Inferences About Mass ExchangeIn each spectrum the full-width at half-maximum was measured for 3 or 4 isolated atomic features. The instrumental broadening was adopted from the width of several water vapor lines in the wavelength region. For the late-type giants with known v sin i values, we determined an empirical broadening relationship with a procedure similar to that of Fekel (1997). Using that empirical infrared calibration and an adopted macroturbulence of 3 km s-1, we obtained projected rotational velocities for the late-type giants in our observed symbiotic systems. Velocity uncertainties are estimated to be 1 km s-1 except for BF Cyg and V1329 Cyg, where the uncertainty is 2 km s-1. Nearly all symbiotics with well-determined orbital elements have circular orbits. From the work of Zahn (1977) and following Schmutz et al. (1994), we assume that if the orbit of the symbiotic binary is circular or nearly so, the late-type giant in such a system is synchronously rotating and its rotational and orbital axes are aligned. With an estimate of the inclination taken from the literature the projected rotational velocity is converted to an equatorial rotational velocity. Then the radius R of the late-type star can be determined 168 use, available at https://www.cambridge.org/core/terms. https://doi

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“…However, as we note in Sections 5.5 and 6.5, there are almost no photometric observations for V455 Sco and SS 73-90, so we have no information about the periods of their pulsational variability. Comparing the results for the two systems in this paper with our symbiotic orbits with the smallest velocity residuals (Fekel et al 2000b(Fekel et al , 2001, we estimate that up to half of the rms error found for the radial-velocity orbital solutions of V455 Sco and SS 73-90 is due to pulsation. Thus, we examined the velocity residuals for periodicities.…”

Section: Pulsation Period Searchmentioning

confidence: 58%

“…As a result, of the nearly 200 symbiotic systems listed in the recent catalog of Belczyński et al (2000), only 30 systems or about 15% have had spectroscopic orbital elements determined for the cool giant component (Mikołajewska 2003;Fekel et al 2007). In five previous papers in this series (Fekel et al 2000a(Fekel et al , 2000b(Fekel et al , 2001(Fekel et al , 2007Hinkle et al 2006) we have determined the orbital elements for the late-type component in 18 systems, seven of which are first orbits.…”

Section: Introductionmentioning

confidence: 99%

Infrared Spectroscopy of Symbiotic Stars. Vi. Combined Orbits for Two S-Type Systems: V455 Scorpii and Ss 73-90

Fekel

Hinkle

Joyce

et al. 2008

The Astronomical Journal

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We have combined new infrared radial velocities and previously obtained spectropolarimetric observations to compute orbits of the M6 giants in two southern S-type symbiotic systems. The spectropolarimetric data enable the orbital inclinations of the systems to be determined, placing greater constraints on the properties of the components. V455 Sco has a circular orbit with a period of 1398 ± 6 days and an inclination of 94 • ± 1 • . The orbit of SS 73-90 has a period of 898 ± 5 days, a modest eccentricity of 0.16, and an inclination of 97 • ± 7 • . The center of mass velocity of each system is large, −77.9 km s −1 for V455 Sco and 89.5 km s −1 for SS 73-90, making them members of the old disk population. The M giant component of each system is likely on the asymptotic giant branch. From estimates of the M giants' radii we predict that both systems are eclipsing and provide ephemerides to search for the eclipses. For V455 Sco, the predicted eclipses are found in data from the Harvard College Observatory plate archives. The He ii emission feature near 1.0123 µm is associated with the hot component in both systems. However, the orbits produced from the emission-line radial velocities do not lead to masses that are consistent with other results.

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Infrared Spectroscopy of Symbiotic Stars. III. First Orbits for Three S-Type Systems

Cited by 39 publications

References 33 publications

Recent photometry of symbiotic stars

Recent photometry of symbiotic stars

Rotational Velocities of S-Type Symbiotic Stars

Infrared Spectroscopy of Symbiotic Stars. Vi. Combined Orbits for Two S-Type Systems: V455 Scorpii and Ss 73-90

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