Multiwavelength observations of V407 Lupi (ASASSN-16kt) – a very fast nova erupting in an intermediate polar

Aydi, E.; Orio, Marina; Beardmore, A. P.; Ness, J. U.; Page, K. L.; Kuin, N. P. M.; Walter, Frederick M.; Buckley, D.; Mohamed, S.; Whitelock, P. A.; Osborne, J. P.; Strader, Jay; Chomiuk, Laura; Darnley, M. J.; Dobrotka, A.; Kniazev, A. Y.; Miszalski, B.; Myers, Gordon; Ospina, N.; Henze, M.; Starrfield, S.; Woodward, C. E.

doi:10.1093/mnras/sty1759

Cited by 35 publications

(26 citation statements)

References 133 publications

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“…During burning, the surface of the magnetic caps, heated also from above by accretion, may be at a higher temperature than the rest of the WD surface. This may have been the case of the intermediate polar nova V407 Lup, observed with Chandra (Aydi et al 2018). Another interesting possibility proposed for V407 Lup and other SSS is that the burning was confined to the magnetic polar regions for a certain period of time (Orio & Shaviv 1993;King et al 2002;Aydi et al 2018).…”

Section: Timing Analysis Of the Chandra Light Curvementioning

confidence: 86%

The Supersoft X-Ray Transient ASASSN-16oh as a Thermonuclear Runaway without Mass Ejection

Hillman

Orio

Prialnik

et al. 2019

ApJL

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The supersoft X-ray and optical transient ASASSN-16oh has been interpreted by Maccarone et al. (2019) as having being induced by an accretion event on a massive white dwarf, resembling a dwarf nova super-outburst. These authors argued that the supersoft X-ray spectrum had a different origin than in an atmosphere heated by shell nuclear burning, because no mass was ejected. We find instead that the event's timescale and other characteristics are typical of non-mass ejecting thermonuclear runaways, as already predicted by Shara et al. (1977) and the extensive grid of nova models by Yaron et al. (2005). We suggest that the low X-ray and bolometric luminosity in comparison to the predictions of the models of nuclear burning are due to an optically thick accretion disk, hiding most of the white dwarf surface. If this is the case, we calculated that the optical transient can be explained as a non-ejective thermonuclear event on a WD of 1.1M accreting at the rate of 3.5−5×10 −7 M yr −1 . We make predictions that should prove whether the nature of the transient event was due to thermonuclear burning or to accretion; observational proof should be obtained in the next few years, because a new outburst should occur within 10-15 years of the event.

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Section: Timing Analysis Of the Chandra Light Curvementioning

confidence: 86%

The Supersoft X-Ray Transient ASASSN-16oh as a Thermonuclear Runaway without Mass Ejection

Hillman

Orio

Prialnik

et al. 2019

ApJL

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“…Periodic variations in the UVOT data have been used to identify orbital periods in some novae (for example, Beardmore et al, 2012;Aydi et al, 2018b;Bode et al, 2016). Given its orbit of ∼ 1.5 hr, Swift can measure timescales close to a day which are generally difficult to do from the ground.…”

Section: X-ray and Uv Variabilitymentioning

confidence: 99%

“…However, assuming SSS emission originates from an extended nuclear-burning atmosphere, asymmetries would be required to produce modulations. In the case of magnetic WDs, hot spots could be caused by material funnelling into the poles, enhancing the nuclear burning in these regions; indeed, Aydi et al (2018b) (Piano et al, 2018). In addition, the earlier nova V1324 Sco (Nova Sco 2012) was also seen in the γ-rays by the LAT (Ackermann et al, 2014), but was never detected in the X-ray band by Swift (Page et al, 2012c;; V5856 Sgr (ASASSN-16ma; Nova Sgr 2016 No.…”

Section: Open Questionsmentioning

confidence: 99%

Neil Gehrels Swift Observatory studies of supersoft novae

Page

Beardmore

Osborne

2020

Advances in Space Research

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The rapid response capabilities of the Neil Gehrels Swift Observatory, together with the daily planning of its observing schedule, make it an ideal mission for following novae in the X-ray and UV bands, particularly during their early phases of rapid evolution and throughout the supersoft source interval. Many novae, both classical and recurrent, have been extensively monitored by Swift throughout their supersoft phase and later decline. We collect here results from observations of novae with outbursts which occurred between the start of 2006 and the end of 2017.

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“…The orbital period of the system is not known. Baklanov et al (2008) detected a modulation with a period of 0.09580(5) days between 10 and 20 days after the outburst, that has not been measured again in more recent works (Shugarov et al 2010;Page et al 2010;Darnley et al 2011).…”

Section: V2491 Cygmentioning

confidence: 69%

Optical observations of ‘hot’ novae returning to quiescence

Zemko

Ciroi

Orio

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We have monitored the return to quiescence of novae previously observed in outburst as supersoft X-ray sources, with optical photometry of the intermediate polar (IP) V4743 Sgr and candidate IP V2491 Cyg, and optical spectroscopy of these two and seven other systems. Our sample includes classical and recurrent novae, short period (few hours), intermediate period (1-2 days) and long period (symbiotic) binaries. The light curves of V4743 Sgr and V2491 Cyg present clear periodic modulations. For V4743 Sgr, the modulation occurs with the beat of the rotational and orbital periods. If the period measured for V2491 Cyg is also the beat of these two periods, the orbital one should be almost 17 hours. The recurrent nova T Pyx already shows fragmentation of the nebular shell less than 3 years after the outburst. While this nova still had strong [O iii] at this post-outburst epoch, these lines had already faded after 3 to 7 years in all the others. We did not find any difference in the ratio of equivalent widths of high ionization/excitation lines to that of the Hβ line in novae with short and long orbital period, indicating that irradiation does not trigger high mass transfer rateṁ from secondaries with small orbital separation. An important difference between the spectra of RS Oph and V3890 Sgr and those of many symbiotic persistent supersoft sources is the absence of forbidden coronal lines. With the X-rays turn-off, we interpret this as an indication that mass transfer in symbiotics recurrent novae is intermittent.

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Multiwavelength observations of V407 Lupi (ASASSN-16kt) – a very fast nova erupting in an intermediate polar

Cited by 35 publications

References 133 publications

The Supersoft X-Ray Transient ASASSN-16oh as a Thermonuclear Runaway without Mass Ejection

The Supersoft X-Ray Transient ASASSN-16oh as a Thermonuclear Runaway without Mass Ejection

Neil Gehrels Swift Observatory studies of supersoft novae

Optical observations of ‘hot’ novae returning to quiescence

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