Wind mass transfer in S-type symbiotic binaries

Skopal, A.; Cariková, Z.

doi:10.1051/0004-6361/201424779

Cited by 24 publications

(46 citation statements)

References 61 publications

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“…Also, focusing of the wind from normal giants in Stype symbiotic binaries towards the orbital plane can be caused by their slow rotation, as suggested by Skopal & Cariková (2015). However, simplifying assumptions in the model by Skopal & Cariková (2015) cannot describe the column density distribution of the circumstellar material around the giant in detail in the same way as we measure in the real case (see Appendix A).…”

Section: Focusing Of the Windmentioning

confidence: 87%

Wind mass transfer in S-type symbiotic binaries

Shagatova

Skopal

Cariková

2016

A&A

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Context. The wind mass transfer from a giant to its white dwarf companion in symbiotic binaries is not well understood. For example, the efficiency of wind mass transfer of the canonical Bondi-Hoyle accretion mechanism is too low to power the typical luminosities of the accretors. However, recent observations and modelling indicate a considerably more efficient mass transfer in symbiotic binaries. Aims. We determine the velocity profile of the wind from the giant at the near-orbital-plane region of eclipsing S-type symbiotic binaries EG And and SY Mus, and derive the corresponding spherical equivalent of the mass-loss rate. With this approach, we indicate the high mass transfer ratio. Methods. We achieved this aim by modelling the observed column densities taking into account ionization of the wind of the giant, whose velocity profile is derived using the inversion of Abel's integral operator for the hydrogen column density function. Results. Our analysis revealed the spherical equivalent of the mass-loss rate from the giant to be a few times 10 −6 M yr −1 , which is a factor of > ∼ 10 higher than rates determined by methods that do not depend on the line of sight. This discrepancy rules out the usual assumption that the wind is spherically symmetric. As our values were derived from near-orbital-plane column densities, these values can be a result of focusing the wind from the giant towards the orbital plane. Conclusions. Our findings suggests that the wind from giants in S-type symbiotic stars is not spherically symmetric, since it is enhanced at the orbital plane and, thus, is accreted more effectively onto the hot component.

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Section: Focusing Of the Windmentioning

confidence: 87%

Wind mass transfer in S-type symbiotic binaries

Shagatova

Skopal

Cariková

2016

A&A

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“…Podsiadlowski and Mohamed (2007) proposed that if the red giant does not fill its Roche lobe, its wind does and the wind is collimated toward the L1 point of the orbit that may yield an accretion disk around the white dwarf. Other accretion modes are proposed to overcome the small efficiency of wind Roche-lobe overflow as in Skopal and Cariková (2015), where the wind from the giant in some symbiotics can be focused by rotation of the giant, following the wind compression disk model from Bjorkman and Cassinelli (1993).…”

Section: White Dwarf Symbioticsmentioning

confidence: 99%

Accretion flows in nonmagnetic white dwarf binaries as observed in X-rays

Balman

2020

Advances in Space Research

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Cataclysmic Variables (CVs) are compact binaries with white dwarf (WD) primaries. CVs and other accreting WD binaries (AWBs) are useful laboratories for studying accretion flows, gas dynamics, outflows, transient outbursts, and explosive nuclear burning under different astrophysical plasma conditions. They have been studied over decades and are important for population studies of galactic X-ray sources. Recent space-and ground-based high resolution spectral and timing studies, along with recent surveys indicate that we still have observational and theoretical complexities yet to answer. I review accretion in nonmagnetic AWBs in the light of X-ray observations. I present X-ray diagnostics of accretion in dwarf novae and the disk outbursts, the nova-like systems, and the state of the research on the disk winds and outflows in the nonmagnetic CVs together with comparisons and relations to classical and recurrent nova systems, AM CVns and Symbiotic systems. I discuss how the advective hot accretion flows (ADAF-like) in the inner regions of accretion disks (merged with boundary layer zones) in nonmagnetic CVs explain most of the discrepancies and complexities that have been encountered in the X-ray observations. I stress how flickering variability studies from optical to X-rays can be probes to determine accretion history and disk structure together with how the temporal and spectral variability of CVs are related to that of LMXBs and AGNs. Finally, I discuss the nature of accretion in nonmagnetic WDs in terms of ADAF-like accretion flows, and elaborate on the solutions it brings and its complications, constructing an observational framework to motivate new theoretical calculations that introduce this flow-type in disks, outflow and wind models together with disk-instability models of outbursts and nova outbursts in AWBs and WD physics, in general.

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“…Systems harbouring NSs are a recent addition to this class of celestial objects (Masetti et al 2006(Masetti et al , 2007a(Masetti et al ,b, 2011Bozzo et al 2018;Yungelson, Kuranov & Postnov 2019) and constitute a few per cent of the known total (Merc, Gális & Wolf 2019a), the vast majority E-mail: ulisse.munari@oapd.inaf.it containing WDs (Mukai et al 2016;Sokoloski et al 2017;Akras et al 2019). For some time, a main-sequence star accreting from the RG at very high rates (10 −6 to 10 −4 M yr −1 ) was considered a viable scenario for SySt in general (Kenyon & Webbink 1984), but this has been progressively abandoned in the light of expanding observational data, especially in the far-ultraviolet (UV) and X-rays (Skopal et al 2006;Sokoloski et al 2006;Mohamed & Podsiadlowski 2012;Luna et al 2013;Skopal & Cariková 2015;Lutovinov et al 2020).…”

Section: Introductionmentioning

confidence: 99%

The GALAH survey and symbiotic stars – I. Discovery and follow-up of 33 candidate accreting-only systems

Munari

Traven

Masetti

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We have identified a first group of 33 new candidates for symbiotic stars (SySt) of the accreting-only variety among the 600 255 stars so far observed by the GALAH high-resolution spectroscopic survey of the Southern Hemisphere, more than doubling the number of those previously known. GALAH aims to high latitudes and this offers the possibility to sound the Galaxy for new SySt away from the usual Plane and Bulge hunting regions. In this paper we focus on SySt of the M spectral type, showing an Hα emission with a peak in excess of 0.5 above the adjacent continuum level, and not affected by coherent radial pulsations. These constraints will be relaxed in future studies. The 33 new candidate SySt were subjected to an array of follow-up confirmatory observations (X–ray/UV observations with the Swift satellite, search for optical flickering, presence of a near-UV upturn in ground-based photometric and spectroscopic data, radial velocity changes suggestive of orbital motion, variability of the emission line profiles). According to Gaia eDR3 parallaxes, the candidate new SySt are located at the tip of the Giant Branch, sharing the same distribution in M(KS) of the well established SySt. The accretion luminosities of the candidate new StSt are in the range 1−10 L⊙, corresponding to mass-accretion rates of 0.1-1 10−9 M⊙ yr−1 for WDs of 1 M⊙. The M giant of one of them presents a large Lithium over-abundance.

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Wind mass transfer in S-type symbiotic binaries

Cited by 24 publications

References 61 publications

Wind mass transfer in S-type symbiotic binaries

Wind mass transfer in S-type symbiotic binaries

Accretion flows in nonmagnetic white dwarf binaries as observed in X-rays

The GALAH survey and symbiotic stars – I. Discovery and follow-up of 33 candidate accreting-only systems

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