A systematic search for rapid photometric variability in southern symbiotic stars I. V648 Car

Angeloni, R.; Mille, F. Di; Lopes, C. E. Ferreira; Masetti, N.

doi:10.1017/s1743921312019503

Cited by 3 publications

(2 citation statements)

References 4 publications

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“…Systematic searches for flickering variability in symbiotic stars and related objects (Angeloni et al ; Dobrzycka et al ; Gromadzki et al ; Sokoloski et al ; Stoyanov ) have shown that, among the more than 200 symbiotic stars known, only in 10 objects flickering activity is detected: that is, RS Oph, T CrB, MWC 560, Z And, V2116 Oph, CH Cyg, RT Cru, o Cet, V407 Cyg, and V648 Car.…”

Section: Introductionmentioning

confidence: 99%

Discovery of optical flickering from the symbiotic star EF Aquilae

et al. 2017

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We report optical CCD photometry of the recently identified symbiotic star EF Aql. Our observations in Johnson V and B bands clearly show the presence of stochastic light variations with an amplitude of about 0.2 mag on a time scale of minutes. The observations point toward a white dwarf (WD) as the hot component in the system. It is the 11-th object among more than 200 symbiotic stars known with detected optical flickering. Estimates of the mass accretion rate onto the WD and the mass loss rate in the wind of the Mira secondary star lead to the conclusion that less than 1 per cent of the wind is captured by the WD. Eight further candidates for the detection of flickering in similar systems are suggested.Comment: 5 pages, submitted to A

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Section: Introductionmentioning

confidence: 99%

Discovery of optical flickering from the symbiotic star EF Aquilae

et al. 2017

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“…Systematic searches for flickering variability in symbiotic stars and related objects (Dobrzycka, Kenyon & Milone 1996;Sokoloski, Bildsten & Ho 2001;Gromadzki et al 2006;Angeloni et al 2013) have shown that optical flickering is a rarely detectable phenomenon in symbiotic stars. Among more than 200 symbiotic stars known, only in 11 objects flickering activity is visible.…”

Section: Introductionmentioning

confidence: 99%

Flickering of the jet‐ejecting symbiotic star MWC 560

et al. 2020

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We analyse optical photometric data of short term variability (flickering) of the accreting white dwarf in the jet-ejecting symbiotic star MWC 560. The observations are obtained in 17 nights during the period November 2011 -October 2019. The colour-magnitude diagram shows that the hot component of the system becomes redder as it gets brighter. For the flickering source we find that it has colour 0.14 < B − V < 0.40, temperature in the range 6300 < T f l < 11000 K, and radius 1.2 < R f l < 18 R ⊙ . We find a strong correlation (correlation coefficient 0.76, significance < 0.001) between B band magnitude and the average radius of the flickering source -as the brightness of the system increases the size of the flickering source also increases. The estimated temperature is similar to that of the bright spot of cataclysmic variables. In 2019 the flickering is missing, and the B-V colour of the hot component becomes bluer.

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Taking a break: Paused accretion in the symbiotic binary RT Cru

Pujol

Luna

Mukai

et al. 2023

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Symbiotic binaries sometimes hide their symbiotic nature for significant periods of time. There is mounting observational evidence that, in symbiotics that are powered solely by the accretion of the red giant's wind material onto a white dwarf, without any quasisteady shell burning on the surface of the white dwarf, the characteristic emission lines in the optical spectrum can vanish, leaving the semblance of an isolated red giant spectrum. Here we present compelling evidence that this disappearance of optical emission lines from the spectrum of RT Cru in 2019 was due to a decrease in the accretion rate, which we derived by modeling the X-ray spectrum. This drop in accretion rate leads to a lower flux of ionizing photons and thus to faint or absent photoionization emission lines in the optical spectrum. We observed the white dwarf symbiotic RT Cru with XMM-Newton and Swift in X-rays and UV and collected ground-based optical spectra and photometry obtained over the last 33 years. This long-term coverage shows that, during most of the year 2019, the accretion rate onto the white dwarf was so low, Ṁ = (3.2 ± 0.06) ×10 −11 M ⊙ yr −1 (d/2.52 kpc) 2 , that the historically detected hard X-ray emission almost vanished, the UV flux faded by roughly 5 magnitudes, the U, B, and V flickering amplitude decreased, and the Balmer lines virtually disappeared from 2019 January through March. Long-lasting low-accretion episodes such as the one reported here may hamper the chances of RT Cru experiencing a nova-type outburst despite the high mass of the accreting white dwarf.

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A systematic search for rapid photometric variability in southern symbiotic stars I. V648 Car

Cited by 3 publications

References 4 publications

Discovery of optical flickering from the symbiotic star EF Aquilae

Discovery of optical flickering from the symbiotic star EF Aquilae

Flickering of the jet‐ejecting symbiotic star MWC 560

Taking a break: Paused accretion in the symbiotic binary RT Cru

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