2019
DOI: 10.1002/asna.201913662
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New online database of symbiotic variables: Symbiotics in X‐rays

Abstract: Symbiotic variable stars belong to an interesting class of interacting binary systems.Since the beginning of this century, the systematic search for these objects has begun, and such surveys have led to discoveries of many new objects and dozens of candidates in the Milky Way and the Local Group. As the latest catalogue of symbiotic binaries is almost two decades old, we decided to prepare a new, online database of the galactic and extragalactic symbiotic systems. These objects are also known for their X-ray e… Show more

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Cited by 16 publications
(10 citation statements)
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“…Symbiotic stars (SySt) are interacting binaries where a red giant (RG) fuels a white dwarf (WD) or a neutron star (NS) companion via accretion (either through Roche lobe overflow or wind intercept). 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%
“…Symbiotic stars (SySt) are interacting binaries where a red giant (RG) fuels a white dwarf (WD) or a neutron star (NS) companion via accretion (either through Roche lobe overflow or wind intercept). 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 connection between AMXPs and MSRPs seems to be supported by the discovery of the so-called "transitional millisecond radio pulsars" (tMSRPs); these are Table 3 A catalog of identified Galactic SyXBs and SyXB candidates. Table partially based on [168], see also [135,169]. "NS/BH" indicates nature of the compact object (via detection of Type I X-ray bursts or pulsations).…”
Section: Magnetically-channeled Accretion In Lmxbs: X-ray Pulsarsmentioning
confidence: 99%
“…Quasi-steady shell burning of the hydrogen-rich material on the surface of WD is probably also the source of super-soft X-ray emission of AG Dra. There are 58 other symbiotic stars which have been detected in X-rays (Merc et al, 2019c). Nine sources, AG Dra among them, show the super-soft emission which have been classified as the α type in the scheme introduced by Muerset et al (1997) and extended by Luna et al (2013).…”
Section: Ag Dra In the New Online Databasementioning
confidence: 99%