Discovery of an eclipsing dwarf nova in the ancient nova shell Te 11

Miszalski, B.; Woudt, P. A.; Littlefair, S. P.; Warner, Brian D.; Boffin, H. M. J.; Corradi, R. L. M.; Jones, David; Motsoaledi, Mokhine; Rodríguez‐Gil, P.; Sabin, L.; Santander-García, M.

doi:10.1093/mnras/stv2689

Cited by 33 publications

(30 citation statements)

References 63 publications

(61 reference statements)

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“…One scenario 12 predicted that novalike binaries undergo a transition to become dwarf novae several centuries 13 after classical nova eruptions. The few known examples 14,15,16,17 of this post-nova-to-dwarf nova metamorphosis lack robust and independent determinations of the date of the associated classical nova 18,19 , and hence the time required to undergo the high-to-low mass transfer transition. Here we report the recovery of the binary underlying the classical nova of 11 March 1437 A.D. 20,21 whose age is independently confirmed by proper motion-dating, and show that in the 20 th century it exhibits dwarf nova eruptions.…”

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confidence: 99%

Proper-motion age dating of the progeny of Nova Scorpii AD 1437

Shara

Iłkiewicz

Mikołajewska

et al. 2017

Nature

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'Cataclysmic variables' are binary star systems in which one star of the pair is a white dwarf, and which often generate bright and energetic stellar outbursts. Classical novae are one type of outburst: when the white dwarf accretes enough matter from its companion, the resulting hydrogen-rich atmospheric envelope can host a runaway thermonuclear reaction that generates a rapid brightening. Achieving peak luminosities of up to one million times that of the Sun, all classical novae are recurrent, on timescales of months to millennia. During the century before and after an eruption, the 'novalike' binary systems that give rise to classical novae exhibit high rates of mass transfer to their white dwarfs. Another type of outburst is the dwarf nova: these occur in binaries that have stellar masses and periods indistinguishable from those of novalikes but much lower mass-transfer rates, when accretion-disk instabilities drop matter onto the white dwarfs. The co-existence at the same orbital period of novalike binaries and dwarf novae-which are identical but for their widely varying accretion rates-has been a longstanding puzzle. Here we report the recovery of the binary star underlying the classical nova eruption of 11 March AD 1437 (refs 12, 13), and independently confirm its age by proper-motion dating. We show that, almost 500 years after a classical-nova event, the system exhibited dwarf-nova eruptions. The three other oldest recovered classical novae display nova shells, but lack firm post-eruption ages, and are also dwarf novae at present. We conclude that many old novae become dwarf novae for part of the millennia between successive nova eruptions.

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confidence: 99%

Proper-motion age dating of the progeny of Nova Scorpii AD 1437

Shara

Iłkiewicz

Mikołajewska

et al. 2017

Nature

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“…a high volume filling factor) suggests a greater ionized mass and different origin, cf. [40]. The bipolar nebula around CK Vul is seen to have a mass comparable to a nova shell, but its origin remains uncertain [35].…”

Section: Discussionmentioning

confidence: 99%

“…We also plot a range of nova shells where we utilize the rather heterogeneous data compiled by [31][32] [33]. Finally, we add the faint bipolar nebula surrounding CK Vul [34] [35], the bowshock nebulae around the nova-like cataclysmic variables (CVs) BZ Cam [36][37] and V341 Ara [15] [38], as well as the peculiar object Te 11 [39] [40].…”

Section: Other Emission Nebulaementioning

confidence: 99%

The Hα surface brightness — radius plane as a diagnostic tool for photoionized nebulae

Frew

Bojičić

Parker

2016

J. Phys.: Conf. Ser.

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The Hα surface brightness -radius (SHα-r) relation is a robust distance indicator for planetary nebulae (PNe), further enhanced by different populations of PNe having distinct loci in SHα-r space. Other types of photoionized nebulae also plot in quite distinct regions in the SHα-r plane, allowing its use as a diagnostic tool. In particular, the nova shells and massive star ejecta (MSE) plot on relatively tight loci illustrating their evolutionary sequences. For the MSE, there is potential to develop a distance indicator for these objects, based on their trend in SHα-r space. As high-resolution, narrowband surveys of the nearest galaxies become more commonplace, the SHα-r plane is a potentially useful diagnostic tool to help identify the various ionized nebulae in these systems.

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“…The DNA nuclease domain then nonspecifically degrades invader DNA, and the RNA nuclease domain cleaves the invader RNA sequence specified by the RNA guide. The Palm domain is also required for immunity 4 , but the details of this are unclear. Type III immunity also relies on a standalone nuclease called Csm6, which slows infection 5 by nonspecifically degrading viral RNA, giving the interference complex time to degrade the viral DNA.…”

Section: K a I T L I N J O H N S O N And S C O T T B A I L E Ymentioning

confidence: 99%

“…On page 558, Shara et al 3 report the identification of the cataclysmic variable that produced the observed nova, known as Nova Scorpii 1437. Although several such systems have previously been found 4,5 , the authors' analysis provides a wealth of information about the state of a cataclysmic variable hundreds of years after a nova.…”

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confidence: 99%