On a century of extragalactic novae and the rise of the rapid recurrent novae

Darnley, M. J.; Henze, M.

doi:10.1016/j.asr.2019.09.044

Cited by 23 publications

(29 citation statements)

References 207 publications

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“…Finally, in Section 7 the most remarkable and extreme nova yet discovered is featured. It is hoped that this article compliments a pair of recent comprehensive reviews of extragalactic novae [25,26].…”

Section: Introductionmentioning

confidence: 79%

“…Using M 31 and the Milky Way as examples, the RN population only accounts for a few percent of the known nova population [29]. However, there are clear and substantial selection effects at play with regard to both the RN population size and the range of observed periods [26]. For example, the RN population of the extensively observed Large Magellanic Cloud (LMC) makes up a much larger proportion of the host's overall nova population [30].…”

Section: Recurrent Novae and The Mmrdmentioning

confidence: 99%

“…[24]) allow us to interpret the positioning of a nova in the MMRD phase space. The traditional MMRD relationship spans from bright-fast novae that contain high mass WDs accreting at a low rate, to faint-slow novae with low mass WDs and highṀ [26] 2 . The faint-fast novae, therefore, arise from high mass WDs with highṀ.…”

Section: Recurrent Novae and The Mmrdmentioning

confidence: 99%

“…Many of the eight long orbital period Galactic RNe (see Section 4) can be classified as faint-fast novae, but to-date, only one (see Section 7) of their faint-fast M 31 and M 87 counterparts has been observed to recur. Recently, [26] proposed that the apparently empty bright-slow MMRD phase space -expected to be occupied by low mass WDs with lowṀ -might be occupied by 'SPRITES' (eSPecially Red Intermediate-luminosity Transient Events; [45]), which populate the infrared luminosity space between novae and SNe. This led [26] to propose that exploration of a 'Bolometric MMRD' could have the potential to restore the usefulness of the MMRD.…”

Section: Recurrent Novae and The Mmrdmentioning

confidence: 99%

“…The Galactic RNe naturally separate into three distinct classes: the symbiotic RNe, the five (four confirmed; V2487 Ophiuchi suspected) with red giant donors, often referred to as the RS Ophiuchi-class; the three with sub-giant donors, or the U Scorpiiclass; and the T Pyxidis-class, those with short CN-like orbital periods. We summarise some of the properties of these novae in Table 1, which draws from data published in [10,26,50,63,64].…”

Section: Galactic Recurrent Novaementioning

confidence: 99%

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Accrete, Accrete, Accrete… Bang! (and repeat): The remarkable Recurrent Novae

Darnley¹

2021

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects v — PoS(GOLDEN2019)

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All novae recur, but only a handful have been observed in eruption more than once. These systems, the recurrent novae (RNe), are among the most extreme examples of novae. RNe have long been thought of as potential type Ia supernova progenitors, and their claim to this 'accolade' has recently been strengthened. In this short review RNe will be presented within the framework of the maximum magnitude-rate of decline (MMRD) phase-space. Recent work integrating Heflashes into nova models, and the subsequent growth of the white dwarf, will be explored. This review also presents an overview of the Galactic and extragalactic populations of RNe, including the newly identified 'rapid recurrent nova' subset-those with recurrence periods of ten years, or less. The most exciting nova system yet discovered-M31N 2008-12a, with its annual eruptions and vast nova super-remnant, is introduced. Throughout, open questions regarding RNe, and some of the expected challenges and opportunities that the near future will bring are addressed.

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Section: Introductionmentioning

confidence: 79%

Section: Recurrent Novae and The Mmrdmentioning

confidence: 99%

Section: Recurrent Novae and The Mmrdmentioning

confidence: 99%

Section: Recurrent Novae and The Mmrdmentioning

confidence: 99%

Section: Galactic Recurrent Novaementioning

confidence: 99%

See 3 more Smart Citations

Accrete, Accrete, Accrete… Bang! (and repeat): The remarkable Recurrent Novae

Darnley¹

2021

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects v — PoS(GOLDEN2019)

Self Cite

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Population synthesis of accreting white dwarfs: rates and evolutionary pathways of H and He novae

Kemp

Karakas

Casey

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Novae are some of the most commonly detected optical transients and have the potential to provide valuable information about binary evolution. Binary population synthesis codes have emerged as the most effective tool for modelling populations of binary systems, but such codes have traditionally employed greatly simplified nova physics, precluding detailed study. In this work, we implement a model treating H and He novae as individual events into the binary population synthesis code binary_c. This treatment of novae represents a significant improvement on the ‘averaging’ treatment currently employed in modern population synthesis codes. We discuss the evolutionary pathways leading to these phenomena and present nova event rates and distributions of several important physical parameters. Most novae are produced on massive white dwarfs, with approximately 70 and 55 per cent of nova events occurring on O/Ne white dwarfs for H and He novae, respectively. Only 15 per cent of H-nova systems undergo a common-envelope phase, but these systems are responsible for the majority of H nova events. All He-accreting He-nova systems are considered post-common-envelope systems, and almost all will merge with their donor star in a gravitational-wave-driven inspiral. We estimate the current annual rate of novae in M31 (Andromeda) to be approximately 41 ± 4 for H novae, underpredicting the current observational estimate of $65^{+15}_{-16}$, and 0.14 ± 0.015 for He novae. When varying common-envelope parameters, the H nova rate varies between 20 and 80 events per year.

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The impact of metallicity on nova populations

Kemp

Karakas

Casey

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The metallicity of a star affects its evolution in a variety of ways, changing stellar radii, luminosities, lifetimes, and remnant properties. In this work, we use the population synthesis code binary_c to study how metallicity affects novae in the context of binary stellar evolution. We compute a 16-point grid of metallicities ranging from Z = 10−4 to 0.03, presenting distributions of nova white dwarf masses, accretion rates, delay-times, and initial system properties at the two extremes of our 16-point metallicity grid. We find a clear anticorrelation between metallicity and the number of novae produced, with the number of novae at Z = 0.03 roughly half that at Z = 10−4. The white dwarf mass distribution has a strong systematic variation with metallicity, while the shape of the accretion rate distribution is relatively insensitive. We compute a current nova rate of approximately 33 novae per year for the Milky Way, a result consistent with observational estimates relying on extra-Galactic novae but an under-prediction relative to observational estimates relying on Galactic novae. However, the shape of our predicted Galactic white dwarf mass distribution differs significantly to existing observationally derived distributions, likely due to our underlying physical assumptions. In M31, we compute a current nova rate of approximately 36 novae per year, under-predicting the most recent observational estimate of $65^{+15}_{-16}$. Finally, we conclude that when making predictions about currently observable nova rates in spiral galaxies, or stellar environments where star formation has ceased in the distant past, metallicity can likely be considered of secondary importance compared to uncertainties in binary stellar evolution.

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On a century of extragalactic novae and the rise of the rapid recurrent novae

Cited by 23 publications

References 207 publications

Accrete, Accrete, Accrete… Bang! (and repeat): The remarkable Recurrent Novae

Accrete, Accrete, Accrete… Bang! (and repeat): The remarkable Recurrent Novae

Population synthesis of accreting white dwarfs: rates and evolutionary pathways of H and He novae

The impact of metallicity on nova populations

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