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LIN 358: A symbiotic binary accreting above the steady hydrogen fusion limit | | J. Kuuttila
; M. Gilfanov
; T. E. Woods
; I. R. Seitenzahl
; A. J. Ruiter
; | | Date: |
5 Nov 2020 | | Abstract: | Symbiotic binaries are long period interacting binaries consisting of a white
dwarf (WD) accreting material from a cool evolved giant star via stellar winds.
In this paper we study the symbiotic binary LIN 358 located in the SMC. We have
observed LIN 358 with the integral field spectrograph WiFeS and obtained its
line emission spectrum. With the help of the plasma simulation and spectral
synthesis code Cloudy, we have constructed a 2D photo-ionisation model of LIN
358. From comparison with the observations, we have determined the colour
temperature of the WD in LIN 358 to be 19 eV, its bolometric luminosity $L =
(1.02 pm 0.15) imes 10^{38}$ erg s$^{-1}$, and the mass-loss rate from the
donor star to be $ 1.2 imes 10^{-6}$ M$_{odot}$ yr$^{-1}$. Assuming a solar
H to He ratio in the wind material, a lower limit to the accreted mass fraction
in LIN 358 is 0.31. The high mass-accretion efficiency of a wind Roche lobe
overflow implies that the WD is accreting above the upper boundary of stable
hydrogen fusion and thus growing in mass with the maximal rate of $approx 4
imes 10^{-7}$ M$_{odot}$ yr$^{-1}$. This causes the WD photosphere to
expand, which explains its low colour temperature. Our calculations show that
the circumstellar material in LIN 358 is nearly completely ionized except for a
narrow cone around the donor star, and that the WD emission is freely escaping
the system. However, due to its low colour temperature, this emission can be
easily attenuated by even moderate amounts of neutral ISM. We speculate that
other symbiotic systems may be operating in a similar regime, thus explaining
the paucity of observed systems. | | Source: | arXiv, 2011.02864 | | Services: | Forum | Review | PDF | Favorites | |
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