Introducing the Condor Array Telescope – IV. A possible nova super-remnant surrounding the putative recurrent nova KT Eridani

Shara, Michael M; Lanzetta, Kenneth M; Garland, James T; Gromoll, Stefan; Valls-Gabaud, David; Walter, Frederick M; Webb, John K; Kniazev, Alexei; Townsend, Lee; Darnley, Matthew J; Healy-Kalesh, Michael; Corral-Santana, Jesus; Schmidtobreick, Linda

doi:10.1093/mnras/stad3612

Monthly Notices of the Royal Astronomical Society

2024

DOI: 10.1093/mnras/stad3612

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Introducing the Condor Array Telescope – IV. A possible nova super-remnant surrounding the putative recurrent nova KT Eridani

Michael M Shara,

Kenneth M Lanzetta,

James T Garland

et al.

Abstract: Just 10 recurrent novae (RNe) – which erupt repeatedly on time-scales shorter than one century – are known in our Galaxy. The most extreme RN known (located in the Andromeda galaxy), M31N 2008-12a, undergoes a nova eruption every year, and is surrounded by a vast nova ‘super-remnant’, 134 pc in extent. Simulations predict that all RNe should be surrounded by similar vast shells, but previous searches have failed to detect them. KT Eri has recently been suggested to be a RN, and we have used the Condor Array Te… Show more

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Cited by 4 publications

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Symbiotic stars, weird novae, and related embarrassing binaries

Merc,

Mikołajewska

2024

Nat Astron

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Symbiotic stars, weird novae, and related embarrassing binaries

Merc,

Mikołajewska

2024

Nat Astron

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Hydrodynamic simulations of the KT Eridani nova super-remnant

Healy-Kalesh,

Darnley,

Shara

et al. 2023

Monthly Notices of the Royal Astronomical Society

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A nova super-remnant (NSR) is an immense structure associated with a nova that forms when frequent and recurrent nova eruptions sweep up surrounding interstellar material (ISM) into a high density and distant shell. The prototypical NSR, measuring over 100 pc across, was discovered in 2014 around the annually erupting nova M 31N 2008-12a. Hydrodynamical simulations demonstrated that the creation of a dynamic NSR by repeated eruptions transporting large quantities of ISM is not only feasible but that these structures should exist around all novae, whether the white dwarf (WD) is increasing or decreasing in mass. But it is only the recurrent nova (RNe) with the highest WD masses and accretion rates that should host observable NSRs. KT Eridani is, potentially, the eleventh RNe recorded in the Galaxy and is also surrounded by a recently unveiled Hα shell tens of parsecs across, consistent with a NSR. Through modelling the nova ejecta from KT Eri, we demonstrate that such an observable NSR could form in approximately 50,000 years, which fits with the proper motion history of the nova. We compute the expected Hα emission from the KT Eri NSR and predict that the structure might be accessible to wide-field X-ray facilities.

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The symbiotic recurrent nova V745 Sco at radio wavelengths

Molina,

Chomiuk,

Linford

et al. 2024

Monthly Notices of the Royal Astronomical Society

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V745 Sco is a Galactic symbiotic recurrent nova with nova eruptions in 1937, 1989, and 2014. We study the behaviour of V745 Sco at radio wavelengths (0.6–37 GHz), covering both its 1989 and 2014 eruptions and informed by optical, X-ray, and $\gamma$-ray data. The radio light curves are synchrotron-dominated. Surprisingly, compared to expectations for synchrotron emission from explosive transients such as radio supernovae, the light curves spanning 0.6–37 GHz all peak around the same time ($\sim$18–26 d after eruption) and with similar flux densities (5–9 mJy). We model the synchrotron light curves as interaction of the nova ejecta with the red giant wind, but find that simple spherically symmetric models with wind-like circumstellar material (CSM) cannot explain the radio light curve. Instead, we conclude that the shock suddenly breaks out of a dense CSM absorbing screen around 20 d after eruption, and then expands into a relatively low-density wind ($\dot{M}_{out} \approx 10^{-9}\!-\!10^{-8}$ M$_{\odot }$ yr$^{-1}$ for $v_w = 10$ km s$^{-1}$) out to $\sim$1 yr post-eruption. The dense, close-in CSM may be an equatorial density enhancement or a more spherical red giant wind with $\dot{M}_{in} \approx [5\!-\!10] \times 10^{-7}$ M$_{\odot }$ yr$^{-1}$, truncated beyond several $\times 10^{14}$ cm. The outer lower-density CSM would not be visible in typical radio observations of Type Ia supernovae: V745 Sco cannot be ruled out as a Type Ia progenitor based on CSM constraints alone. Complementary constraints from the free–free radio optical depth and the synchrotron luminosity imply the shock is efficient at accelerating relativistic electrons and amplifying magnetic fields, with $\epsilon _e$ and $\epsilon _B \approx 0.01\!-\!0.1$.

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Introducing the Condor Array Telescope – IV. A possible nova super-remnant surrounding the putative recurrent nova KT Eridani

Cited by 4 publications

References 49 publications

Symbiotic stars, weird novae, and related embarrassing binaries

Symbiotic stars, weird novae, and related embarrassing binaries

Hydrodynamic simulations of the KT Eridani nova super-remnant

The symbiotic recurrent nova V745 Sco at radio wavelengths

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