A radio survey of symbiotic stars

Seaquist, E. R.; Taylor, A. R.; Button, S.

doi:10.1086/162399

Cited by 160 publications

(130 citation statements)

References 0 publications

Supporting

Mentioning

125

Contrasting

Order By: Relevance

“…RA and declination (J2000.0), taken from radio VLA positions ( [117,280,281]) if available, and if not from the SIMBAD database but corrected in a few cases were obvious mistakes have been spotted. If position was taken from somewhere else then comment is given in Sect.…”

Section: 4mentioning

confidence: 99%

See 1 more Smart Citation

A catalogue of symbiotic stars

Belczyński

Mikołajewska

Munari

et al. 2000

Astron. Astrophys. Suppl. Ser.

378

407

View full text Add to dashboard Cite

Abstract. We present a new catalogue of symbiotic stars. In our list we include 188 symbiotic stars as well as 30 objects suspected of being symbiotic. For each star, we present basic observational material: coordinates, V and K magnitudes, ultraviolet (UV), infrared (IR), X-ray and radio observations. We also list the spectral type of the cool component, the maximum ionization potential observed, references to finding charts, spectra, classifications and recent papers discussing the physical parameters and nature of each object. Moreover, we present the orbital photometric ephemerides and orbital elements of known symbiotic binaries, pulsational periods for symbiotic Miras, Hipparcos parallaxes and information about outbursts and flickering.

show abstract

Section: 4mentioning

confidence: 99%

“…If more than one detection has been reported, only one is included and the priority is given to the most extensive radio survey of symbiotics at 3.6 cm [279]. Other extensive surveys of symbiotic stars which were searched for radio detection include [280,319,281,112,117].…”

mentioning

confidence: 99%

A catalogue of symbiotic stars

Belczyński

Mikołajewska

Munari

et al. 2000

Astron. Astrophys. Suppl. Ser.

378

407

View full text Add to dashboard Cite

show abstract

“…The absorbed PSPC count rate has been determined from simulations using a blackbody spectrum with kT = 30 eV, SMC reduced metallicities (-0.6 dex), a foreground galactic column of 3 × 10 20 cm −2 and an inclination of 60 • to 90 • . For each data point of the observed lightcurve the column density of neutral and ionized hydrogen has been calculated using a threshold for the ionization parameter ξ = L n s 2 of 1.0, with the luminosity L (Kallman & McCray 1982, see also Seaquist et al 1984 for an approach to calculate the ionization front in a symbiotic X-ray binary). In the ionized gas phase an additional neutral (e.g.…”

Section: The X-ray Eclipsementioning

confidence: 99%

The hot and cool component of the symbiotic nova SMC 3

Kahabka

2004

A&A

View full text Add to dashboard Cite

Abstract. The ∼6 year supersoft X-ray lightcurve of the symbiotic nova SMC 3 (=RX J0048.4−7332) in the Small Magellanic Cloud is derived from archival ROSAT PSPC and HRI data. It shows one deep X-ray eclipse during which the count rate decreased by a factor of > ∼ 80. In MACHO B-band data sinusoidal variation is found with a quasi-periodicity of ∼4 years. The minimum of the B-band flux occurs during the X-ray eclipse. In OGLE II I-band observations performed after the ROSAT observations we detect 110 ± 2 day oscillations which we interpret as pulsations of the M0 giant star in the symbiotic system. The observed duration of the supersoft X-ray eclipse of ∼0.4-1.8 years is explained by the occultation of the white dwarf by the giant companion with an orbital period of ∼(4.0-4.8) years and a strong wind blown from its surface with a mass loss rate of ∼(2.6−8.2) × 10 −7 M yr −1 , assuming that ∼(1−3.5)% of the ionized phase is neutral (e.g. due to dust) and assuming a terminal velocity of ∼30 km s −1 . The ∼4 year quasi-periodicity found in the optical is explained as the binary orbital period of the system. It is less likely that it reflects the activity (or mass-loss) time scale of the red giant star. A ∼(700-800) day quasi-periodicity found in the OGLE II and MACHO data is explained as the first harmonic of a binary orbital cycle. SMC 3 therefore may be classified as a small-amplitude red variable star (SARV). The hot star most likely is in a state of steady nuclear burning with an accretion rate somewhat below the upper critical value of ∼10 −7 M yr −1 .

show abstract

“…Seaquist et al 1984). A typical signature of the quiescent phase is a wave-like orbitally related variation in the LCs.…”

Section: Introductionmentioning

confidence: 99%

Recent photometry of symbiotic stars

et al. 2012

View full text Add to dashboard Cite

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.

show abstract

A radio survey of symbiotic stars

Cited by 160 publications

References 0 publications

A catalogue of symbiotic stars

A catalogue of symbiotic stars

The hot and cool component of the symbiotic nova SMC 3

Recent photometry of symbiotic stars

Contact Info

Product

Resources

About