On orbital period changes in nova outbursts

Martin, Rebecca G.; Livio, Mario; Schaefer, Bradley E.

doi:10.1111/j.1365-2966.2011.18835.x

Cited by 14 publications

(13 citation statements)

References 35 publications

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“…With this, the sign of ΔP is ambiguous. As such, the mechanism proposed by Martin et al (2011) is now required not, it is certainly operating at some level, and it might yet be the dominating effect.…”

Section: Period Change Across the 1999 Eruptionmentioning

confidence: 99%

“…An early report on the ΔP value from my eclipse times (Martin et al 2011) quotes a negative value, with this being hard to understand because ΔP drag must be negligibly small. For this early report, I had not appreciated the effects of allowing for a non-zeroṖ .…”

Section: Period Change Across the 1999 Eruptionmentioning

confidence: 99%

“…Martin et al (2011) proposes one reasonable mechanism. For this paper, I will only consider the effects of the mass loss and frictional drag.…”

Section: Appendix B Period Changes and The O − C Curvementioning

confidence: 99%

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The Change of the Orbital Periods Across Eruptions and the Ejected Mass for Recurrent Novae Ci Aquilae and U Scorpii

Schaefer

2011

ApJ

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I report on the cumulative results from a program started 24 years ago designed to measure the orbital period change of recurrent novae (RNe) across an eruption. The goal is to use the orbital period change to measure the mass ejected during each eruption as the key part of trying to measure whether the RNe white dwarfs are gaining or losing mass over an entire eruption cycle, and hence whether they can be progenitors for Type Ia supernovae. This program has now been completed for two eclipsing RNe: CI Aquilae ( eruptions. The eclipse times during the tails of eruptions are systematically and substantially shifted with respect to the ephemerides from the eclipses in quiescence, with this being caused by shifts of the center of light during the eruption. These eclipse times are plotted on an O − C diagram and fitted to models with a steady period change (Ṗ ) between eruptions (caused by, for example, conservative mass transfer) plus an abrupt period change (ΔP ) at the time of eruption. The primary uncertainty arises from the correlation between ΔP withṖ , such that a more negativeṖ makes for a more positive ΔP . For CI Aql, the best fit is ΔP = −3.7 +9.2 −7.3 × 10 −7 . For U Sco, the best fit is ΔP = (+43 ± 69) × 10 −7 days. These period changes can directly give a dynamical measure of the mass ejected (M ejecta ) during each eruption with negligible sensitivity to the stellar masses and no uncertainty from distances. For CI Aql, the 1σ upper limit is M ejecta < 10 × 10 −7 M . For U Sco, I derive M ejecta = (43 ± 67) × 10 −7 M .

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Section: Period Change Across the 1999 Eruptionmentioning

confidence: 99%

Section: Period Change Across the 1999 Eruptionmentioning

confidence: 99%

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The Change of the Orbital Periods Across Eruptions and the Ejected Mass for Recurrent Novae Ci Aquilae and U Scorpii

Schaefer

2011

ApJ

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“…19). (3) The third known effect is material in the ejected shell being forced to corotate with the white dwarf due to being entrained in its magnetic field for the initial part of its ejection, with this carrying away rotational angular momentum that then gets transferred to cause a loss of the orbital angular momentum (Martin et al 2011). This effect has a strong dependence on the mass ratio, where the total period change can be negative only for q <0.4 or so, while the required effect (for our observed ∆P/P and for even 10 −6 M ejected) requires a mass ratio of q=0.002 even for high magnetic fields.…”

Section: Evolution Of V1017 Sgrmentioning

confidence: 99%

Accurate pre- and post-eruption orbital periods for the dwarf/classical nova V1017 Sgr

Salazar

LeBleu

Schaefer

et al. 2017

Monthly Notices of the Royal Astronomical Society

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V1017 Sgr is a classical nova (in 1919) that displayed an earlier dwarf nova eruption (in 1901), and two more dwarf nova events (in 1973 and 1991). Previous work on this bright system in quiescence (V=13.5) has only been a few isolated magnitudes, a few spectra, and an ambiguous claim for an orbital period of 5.714 days as based on nine radial velocities. To test this period, we have collected 2896 magnitudes (plus 53 in the literature) in the UBVRIJHKL bands from 1897 to 2016, making an essentially complete photometric history of this unique cataclysmic variable. We find that the light curve in all bands is dominated by the ellipsoidal modulations of a G giant companion star, with a post-eruption (after the 1919 nova event) orbital period of 5.786290±0.000032 days. This is the longest period for any classical nova, the accretion must be powered by the nuclear evolution of the companion star, and the dwarf nova events occur only because the outer parts of the large disk are cool enough to be unstable. Furthermore, we measure the pre-eruption orbital period (from 1907 to 1916), and there is a small steady period change in quiescence. The orbital period has decreased by 273±61 parts-per-million across the 1919 eruption, with the significance of the period change being at the 5.7-sigma confidence level. This is startling and mystifying for nova-theory, because the three known period change effects cannot account for a period decrease in V1017 Sgr, much less one of such a large size.

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“…A possible test of this hypothesis is that the process should result in a detectable orbital period change of order ΔP/P ∼ M THEA /M binary ∼ 10 −4 over the epoch of the creation of the reservoir. Such period changes have been studied before in CVs with some success (Schaefer & Patterson 1983) in spite of significant uncertainties caused by effects from the accretion disk (Pringle 1975), and the situation continues to improve (Martin, Livio, & Schaefer 2011).…”

Section: Features Of Feros Spectramentioning

confidence: 99%

Episodic Mass Transfer: A Trigger for Nova Outbursts?

Williams

2011

Proc. IAU

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Abstract. High resolution spectra of post-outburst novae show multiple components of ejected gas that are kinematically distinct. We interpret the observations in terms of episodes of enhanced mass transfer originating from the secondary star that result in the formation of discrete components of circumbinary gas and accretion onto the white dwarf (WD) that trigger nova outbursts. In this picture the concordance between absorption line velocities and emission line widths in most novae occurs as a result of the collision of the expanding nova ejecta with a larger mass of surrounding circumbinary gas. One implication of this model is that much of the accreted gas remains on the WD, leading to a secular increase in WD mass over each outburst event. Alternative scenarios to explain nova spectral evolution are possible that do not invoke circumbinary gas and a possible test of different models is proposed.

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On orbital period changes in nova outbursts

Cited by 14 publications

References 35 publications

The Change of the Orbital Periods Across Eruptions and the Ejected Mass for Recurrent Novae Ci Aquilae and U Scorpii

The Change of the Orbital Periods Across Eruptions and the Ejected Mass for Recurrent Novae Ci Aquilae and U Scorpii

Accurate pre- and post-eruption orbital periods for the dwarf/classical nova V1017 Sgr

Episodic Mass Transfer: A Trigger for Nova Outbursts?

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