Symbiotic Stars as Possible Progenitors of SNe Ia: Binary Parameters and Overall Outlook

Mikołajewska, Joanna

doi:10.1017/s1743921312014925

Cited by 7 publications

(3 citation statements)

References 6 publications

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“…Such variability is particularly useful to identify symbiotics previously misclassified as PNe and was used to determine orbital periods for 5 S-types and Mira pulsation periods for 3 D-types. The lightcurve of the eclipsing 003.46-01.92 also shows ellipsoidal variations, which makes this object of interest to monitor for nova-like activity (Mikołajewska 2013). Unfortunately, we noticed no nova-like outbursts amongst our sample, suggesting they are rare over timescales of ∼7-15 years.…”

Section: Representative Observationsmentioning

confidence: 70%

A remarkable sample of new symbiotic stars towards the Galactic Bulge

Miszalski,

Mikołajewska,

Udalski

2013

Preprint

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Symbiotic stars are the longest orbital period interacting binaries, where nova-like outbursts are generated by the accretion of a high mass loss rate red giant wind onto a white dwarf companion. Long-term photometric monitoring surveys such as OGLE and MACHO are ideal platforms to identify nova-like events in symbiotic stars, however there are only a handful of known systems within the small footprint of these surveys. We introduce a systematic Halpha emission line object survey for new symbiotic stars covering 35 deg 2 towards the Galactic Bulge that combines deep 2dF/AAOmega spectroscopy with OGLE and MACHO photometry. This powerful combination has uncovered nearly two dozen new symbiotic stars, more than a dozen probable symbiotic stars, and several other unusual Hα emission line stars. While we don't find any nova-like activity, the lightcurves do exhibit semi-regular and Mira pulsations, orbital variations and slower changes due to dust. Here we introduce a few of the new symbiotics, including H1-45, only the fourth known carbon symbiotic Mira. This remarkable discovery may be the first luminous carbon star belonging to the Galactic Bulge, according to its period-luminosity relation distance of 6.2 ± 1.4 kpc, potentially shedding new light on the puzzling lack of luminous carbon stars in the Bulge. We also present two old novae captured in the nebular phase, complementing other surveys to better characterise the old nova population.

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Section: Representative Observationsmentioning

confidence: 70%

A remarkable sample of new symbiotic stars towards the Galactic Bulge

Miszalski,

Mikołajewska,

Udalski

2013

Preprint

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“…Kepler's Supernova Remnant, a remnant of SN Ia, has dust features consistent with a SD scenario and a massive AGB donor (Williams et al 2012). It's progenitor could had been very similar to the SySt V407 Cyg (Chiotellis et al 2012;Miko lajewska 2013). V407 Cyg is a SySt containing a massive Mira donor on AGB (Tatarnikova et al 2003a,b) and a massive WD (e.g.…”

Section: Introductionmentioning

confidence: 99%

Wind Roche lobe overflow as a way to make Type Ia supernovae from the widest symbiotic systems

Iłkiewicz

Mikołajewska

Belczyński

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Symbiotic stars are interacting binaries with one of the longest orbital periods. Since they can contain a massive white dwarf with a high accretion rate they are considered a promising type Ia supernovae (SNe Ia) progenitors. Among symbiotic binaries there are systems containing a Mira donor, which can have orbital periods of a few tens of years and more. This subclass of symbiotic stars due to their very large separation usually was not considered promising SNe Ia progenitors. We analysed evolution of one of the well studied symbiotic star with a Mira donor, V407 Cyg. We showed that the standard evolution model predicts that the system will not become a SN Ia. However, by simply adding a Wind Roche Lobe Overflow as one of the mass transfer modes we predict that the white dwarf in V407 Cyg will reach the Chandrasekhar limit in 40-200 Myr.

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“…These problems make it difficult to obtain well-determined orbital elements. Currently, spectroscopic orbits for about 40 of the cool giant components in the S-type symbiotics have been determined (Mikołajewska 2011;Jorissen et al 2012). Thus, of the nearly 200 symbiotic systems listed in the catalog of Belczyński et al (2000), at present only about 20% have had spectroscopic orbital elements determined for the cool giant component.…”

Section: Introductionmentioning

confidence: 99%

Infrared Spectroscopy of Symbiotic Stars. X. Orbits for Three S-Type Systems: V1044 Centauri, Hen 3-1213, and Ss 73-96

Fekel

Hinkle

Wood

2015

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Employing new infrared radial velocities, we have computed orbits of the cool giants in three southern S-type symbiotic systems. The orbit for V1044 Cen, an M5.5 giant, has a period of 985 days and a modest eccentricity of 0.16. Hen 3-1213 is a K4 giant, yellow symbiotic with an orbital period of 533 days and a similar eccentricity of 0.18. For the M2 giant SS 73-96 the orbital period is 828 days, and this system has a somewhat larger eccentricity of 0.26. Measurement of the H I Paschen δ emission lines, which may at least partially reflect the motion of the secondary in SS 73-96, results in a mass ratio of 2.4 for the M giant relative to the presumed white dwarf. The estimated orbital inclinations of V1044 Cen and Hen 3-1213 are low, about 40°. However, for SS 73-96 the predicted inclination is 90°, and so an ephemeris for eclipses of the secondary or the hot nebula surrounding it is provided. A search of the orbital velocity residuals of V1044 Cen and SS 73-96 for pulsation periods produced no realistic or convincing period for either star.

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Symbiotic Stars as Possible Progenitors of SNe Ia: Binary Parameters and Overall Outlook

Cited by 7 publications

References 6 publications

A remarkable sample of new symbiotic stars towards the Galactic Bulge

A remarkable sample of new symbiotic stars towards the Galactic Bulge

Wind Roche lobe overflow as a way to make Type Ia supernovae from the widest symbiotic systems

Infrared Spectroscopy of Symbiotic Stars. X. Orbits for Three S-Type Systems: V1044 Centauri, Hen 3-1213, and Ss 73-96

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