Chemical abundance analysis of symbiotic giants – III. Metallicity and CNO abundance patterns in 24 southern systems

Gałan, C.; Mikołajewska, Joanna; Hinkle, Kenneth H.; Joyce, R. R.

doi:10.1093/mnras/stv2365

Cited by 15 publications

(9 citation statements)

References 109 publications

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“…Detailed photospheric abundance analysis for this system resulted in a slightly subsolar metallicity, [Fe/H] ≈ −0.5 and [α/Fe] = +0.27 (where α represents the average of the Mg, Si, and Ca elements), and an [α/Fe] versus [Fe/H] relation close to the mean one without any notable peculiarity to this object (Hinkle et al 2019). Similar α-element and Fe abundances were found in many symbiotic giants with white dwarf companions (Gałan et al 2016(Gałan et al , 2017. Bottom: the 15-50 keV daily-averaged count rate from the Neil Gehrels Swift BAT.…”

Section: Metallicitysupporting

confidence: 60%

The Donor of the Black Hole X-Ray Binary MAXI J1820+070

Mikołajewska

Zdziarski

Ziółkowski

et al. 2022

ApJ

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We estimate the parameters of the donor of the accreting black hole binary MAXI J1820+070. The measured values of the binary period, rotational and radial velocities, and constraints on the orbital inclination imply the donor is a subgiant with the mass of M 2 ≈ 0.49 − 0.10 + 0.10 M ☉ and the radius of R 2 ≈ 1.19 − 0.08 + 0.08 R ☉ . We reanalyze the previously obtained optical spectrum from the Gran Telescopio Canarias and found it yields a strict lower limit on the effective temperature of T > 4200 K. We compile optical and infrared fluxes observed during the quiescence of this system. From the minima r- and i-band fluxes found in Pan-STARSS1 Data Release 2 prediscovery imaging and for a distance of D ≈ 3 kpc, reddening of E(B – V) = 0.23, and R 2 ≈ 1.11R ⊙, we find T ≲ 4230 K, very close to the above lower limit. For a larger distance, the temperature can be higher, up to about 4500 K (corresponding to a K5 spectral type, preferred by previous studies) at D = 3.5 kpc, allowed by the Gaia parallax. We perform evolutionary calculations for the binary system and compare them to the observational constraints. Our model fitting the above temperature and radius constraints at D ≈ 3 kpc has a mass of 0.4M ⊙, T ≈ 4200 K, and solar metallicity. Two alternative models require D ≳ 3.3–3.4 kpc at 0.4M ⊙, T ≈ 4500 K and half-solar metallicity, and 0.5M ⊙, T ≈ 4300 K, and solar metallicity. These models yield mass-transfer rates of ∼10−10 M ⊙ yr−1, compatible with those based on the estimated accreted mass of ≈2 × 1025 g and the time between the 2018 discovery and the 1934 historical outburst.

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Section: Metallicitysupporting

confidence: 60%

The Donor of the Black Hole X-Ray Binary MAXI J1820+070

Mikołajewska

Zdziarski

Ziółkowski

et al. 2022

ApJ

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“…Although N is also enhanced in the atmosphere of the red giant component of RS Oph ([N/H]=0.6±0.3), its moderate C/N=0.16 (Pavlenko et al 2008) indicates this N enhancement is not as strong as that in the nova ejecta. Systematic studies of photospheric abundances of a few dozens symbiotic giants revealed N/O 0.5 and C/N 0.2, and they are consistent with moderate enhancement of N and depletion of C as expected for their evolutionary stage (Ga lan et al 2016(Ga lan et al , 2017.…”

Section: Uv and Optical Spectroscopysupporting

confidence: 70%

The Massive CO White Dwarf in the Symbiotic Recurrent Nova RS Ophiuchi

Mikołajewska

Shara

2017

ApJ

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If accreting white dwarfs (WD) in binary systems are to produce type Ia supernovae (SNIa), they must grow to nearly the Chandrasekhar mass and ignite carbon burning. Proving conclusively that a WD has grown substantially since its birth is a challenging task. Slow accretion of hydrogen inevitably leads to the erosion, rather than the growth of WDs. Rapid hydrogen accretion does lead to growth of a helium layer, due to both decreased degeneracy and the inhibition of mixing of the accreted hydrogen with the underlying WD. However, until recently, simulations of helium-accreting WDs all claimed to show the explosive ejection of a helium envelope once it exceeded ∼ 10 −1 M ⊙ . Because CO WDs cannot be born with masses in excess of ∼ 1.1 M ⊙ , any such object, in excess of ∼ 1.2 M ⊙ , must have grown substantially. We demonstrate that the WD in the symbiotic nova RS Oph is in the mass range 1.2-1.4 M ⊙ . We compare UV spectra of RS Oph with those of novae with ONe WDs, and with novae erupting on CO WDs. The RS Oph WD is clearly made of CO, demonstrating that it has grown substantially since birth. It is a prime candidate to eventually produce an SNIa.

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“…The [α/Fe] versus [Fe/H] is close to the mean relation (Lambert 1987) and shows no notable peculiarity for this star. The α element and Fe abundances are similar to the abundances of many other SySt giants (Ga lan et al 2016(Ga lan et al , 2017. Casares et al (2017) report that in LMXB many of the low-mass stars show enhancements of Fe and α elements.…”

Section: Stellar Evolutionsupporting

confidence: 69%