Discovery of a planetary nebula surrounding the symbiotic star DT Serpentis

Munari, U.; Corradi, R. L. M.; Siviero, A.; Baldinelli, L.; Maitan, A.

doi:10.1051/0004-6361/201321883

Cited by 6 publications

(3 citation statements)

References 29 publications

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“…Central stars of ∼20% of known PNe are reported to be close binaries (e.g., Bond 2000;Miszalski et al 2009), and it is increasing with deeper sky surveys like Kepler and Gaia (e.g., Barker et al 2018;Jacoby et al 2021;Chornay et al 2021;Chornay & Walton 2022). Mass-accreting WD binaries have been already observed as the central stars in some known PNe (Bode et al 1987;Guerrero et al 2004;Wesson et al 2008;Munari et al 2013;Maitra & Haberl 2022). Some WDs might accrete mass from their non-degenerate companions (Hamann et al 2003;Guerrero et al 2019;Jones et al 2019), a process that might explain some puzzles, like the luminosity function of PNe (Ciardullo 2016;Davis et al 2018;Souropanis et al 2023).…”

Section: Introductionmentioning

confidence: 99%

Accretion-induced Collapse from Magnetic White Dwarf Binaries and Formation of Binary Millisecond Pulsars: Redbacks and Black Widows

Ablimit

2019

ApJ

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Redbacks (RBs) and black widows (BWs) are two peculiar classes of eclipsing millisecond pulsars (MSPs). The accretion-induced collapse (AIC) of an oxygen/neon/magnesium composition white dwarf to a neutron star has been suggested as one possible formation pathway for those two classes of MSPs. However, it is difficult to produce all known MSPs with the traditional AIC scenario. In this study by using the MESA stellar evolution code, we investigate the detailed pre-AIC evolution of magnetized white dwarf binaries with the magnetic confinement model where the high magnetic field strength of the white dwarf can confine the accreted matter in the polar caps. We find that the initial donor mass and orbital periods in our model can be lower than that of previous traditional AIC models. We also present post-AIC evolution models to form RBs and BWs with and without the spin down luminosity evaporation of MSPs. Under the magnetic confinement model and evaporative winds (with corresponding angular momentum loss from the surface of the donor star), the companion masses and orbital periods of all known RBs can be covered and a number of binaries can evolve to become BWs.

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Section: Introductionmentioning

confidence: 99%

Accretion-induced Collapse from Magnetic White Dwarf Binaries and Formation of Binary Millisecond Pulsars: Redbacks and Black Widows

Ablimit

2019

ApJ

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“…This question is not rhetorical, as several direct and indirect observational evidence indicate that mass accretion takes place in several binary central stars of PNe. For instance, binary systems related to accreting WDs such as classical novae (Bode et al 1987;Wesson et al 2008), symbiotic stars (Guerrero et al 2004;Santander-García et al 2004;Corradi et al 2011;Munari et al 2013;Iłkiewicz et al 2018;Akras et al 2019) and supersoft X-ray sources (Kahabka et al 2008;Hutchings et al 2001;Mereghetti et al 2010;Maitra & Haberl 2022) have been observed to be hosted in the centres of PNe. Mass accretion processes have also been suggested to take place at the central stars of the PNe N66 (Hamann et al 2003) and the Eskimo Nebula (Guerrero et al 2019) as a plausible explanation for the two optical outbursts and the variable X-ray emission observed at the centre of the two nebulae, respectively.…”

Section: Introductionmentioning

confidence: 99%

Planetary nebulae hosting accreting white dwarfs: a possible solution for the mysterious cut-off of planetary nebula luminosity function?

Souropanis

Chiotellis

Boumis

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Many binary companions to the central stars of planetary nebulae (PNe) are found to be inflated, perhaps indicating that accretion onto the central star might occur during the PN phase. The discovery of a handful of nova eruptions and supersoft X-ray sources inside PNe supports this hypothesis. In this paper, we investigate the impact that hosting a steadily-accreting WD would have on the properties and evolution of a PN. By pairing the published accreting nuclear-burning WD models with radiation transfer simulations, we extract the time evolution of the emission line spectra and ionization properties of a PN that surrounds a 0.6$\rm M_{\odot }$ steadily nuclear-burning WD as a function of the mass accretion rate. We find that accreting WDs are able to form very extended, high excitation, [O iii]-bright PNe, which are characterised by high nebular electron temperatures. Their properties remain almost invariant with time and their visibility time can be much longer compared to PNe powered by single WDs. We discuss the implications of our findings in explaining specific characteristics observed in PNe. Finally, we examine how accreting WDs affect the planetary nebula luminosity function (PNLF) by covering WD masses in the range of 0.5-0.8$\rm M_{\odot }$ and for various accretion rates within the steady accretion regime. We find that for all but the lowest accretion rates, the [O iii]-luminosities are almost constant and clustered very close to the PNLF cut-off value. Our results suggest that mass-accreting WDs in interacting binaries might play a role in understanding the invariant cut-off of the PNLF.

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“…),Parker et al (2012b),Miszalski et al (2013),Aller et al (2013), Blanco Cárdenas et al (2013,Frew et al (2013),Munari et al (2013, see Frew et al 2014c),Yuan & Liu (2013),Miranda et al (2014),Miszalski & Miko lajewska (2014),Chhetri et al (2015) andKanarek et al (2016).…”

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confidence: 97%

Challenges faced by current Galactic planetary nebula surveys

Frew

2016

Proc. IAU

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Determining the demographics of the Galactic planetary nebula (PN) population is an important goal to further our understanding of this intriguing phase of stellar evolution. The Galactic population has more than doubled in number over the last 15 years, particularly from narrowband \ha\ surveys along the plane. In this review I will summarise these results, with emphasis on the time interval since the last IAU Symposium. These primarily optical surveys are not without their limitations and new surveys for PNe in the infrared similarly face a number of challenges. I will discuss the need for multi-wavelength approaches to discovery and analysis. The desire to have accurate volume-limited samples of Galactic PNe at our disposal is emphasised, which will be impacted with new data from the Gaia satellite mission. We need robust surveys of PNe and their central stars, especially volume-limited surveys, in order to clarify and quantify their evolutionary pathways.Comment: 8 pages, 3 figures, Invited Review given at IAU Symposium 323, held in Beijing, China, October 201

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Discovery of a planetary nebula surrounding the symbiotic star DT Serpentis

Cited by 6 publications

References 29 publications

Accretion-induced Collapse from Magnetic White Dwarf Binaries and Formation of Binary Millisecond Pulsars: Redbacks and Black Widows

Accretion-induced Collapse from Magnetic White Dwarf Binaries and Formation of Binary Millisecond Pulsars: Redbacks and Black Widows

Planetary nebulae hosting accreting white dwarfs: a possible solution for the mysterious cut-off of planetary nebula luminosity function?

Challenges faced by current Galactic planetary nebula surveys

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