The relationship between X-ray luminosity and duty cycle for dwarf novae and their specific frequency in the inner Galaxy

Britt, C. T.; Maccarone, Thomas J.; Pretorius, Magaretha L.; Hynes, R. I.; Jonker, P. G.; Torres, M. A. P.; Knigge, Christian; Johnson, C. Olivia; Heinke, C.; Steeghs, D.; Greiss, S.; Nelemans, G.

doi:10.1093/mnras/stv256

Cited by 20 publications

(21 citation statements)

References 63 publications

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“…This suggests a correlation also with the long-term average accretion rate that is driven by the secular evolution of the system. Consistent with this, there is also a correlation between the quiescent X-ray luminosity and the outburst duty cycle, where duty cycle is defined as the proportion of time spent in outburst (Britt et al 2015).…”

Section: X-ray Luminositiesmentioning

confidence: 53%

Distances of cataclysmic variables and related objects derived fromGaiaData Release 1

Ramsay

Schreiber

Gänsicke

et al. 2017

A&A

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We consider the parallaxes of sixteen cataclysmic variables and related objects that are included in the TGAS catalogue, which is part of the Gaia first data release, and compare these with previous parallax measurements. The parallax of the dwarf nova SS Cyg is consistent with the parallax determination made using the VLBI, but with only one of the analyses of the HST Fine Guidance Sensor (FGS) observations of this system. In contrast, the Gaia parallaxes of V603 Aql and RR Pic are broadly consistent, but less precise than the HST/FGS measurements. The Gaia parallaxes of IX Vel, V3885 Sgr, and AE Aqr are consistent with, but much more accurate than the Hipparcos measurements. We take the derived Gaia distances and find that absolute magnitudes of outbursting systems show a weak correlation with orbital period. For systems with measured X-ray fluxes we find that the X-ray luminosity is a clear indicator of whether the accretion disc is in the hot and ionised or cool and neutral state. We also find evidence for the X-ray emission of both low and high state discs correlating with orbital period, and hence the long-term average accretion rate. The inferred mass accretion rates for the nova-like variables and dwarf novae are compared with the critical mass accretion rate predicted by the Disk Instability Model. While we find agreement to be good for most systems there appears to be some uncertainty in the system parameters of SS Cyg. Our results illustrate how future Gaia data releases will be an extremely valuable resource in mapping the evolution of cataclysmic variables.

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Section: X-ray Luminositiesmentioning

confidence: 53%

Distances of cataclysmic variables and related objects derived fromGaiaData Release 1

Ramsay

Schreiber

Gänsicke

et al. 2017

A&A

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“…Moreover, the WZSge type stars, i.e., dwarf novae with extremely long quiescent intervals, cannot be explained with DIM with α∼0.01 that works for shorter recurrence period dwarf novae. Finally, Britt et al (2015) discovered a correlation between the quiescent X-ray luminosity and the duty cycle of dwarf novae. While this does not immediately contradict DIM, there does not appear to be a ready explanation for it, either.…”

Section: Quiescent Dwarf Novaementioning

confidence: 96%

X-Ray Emissions from Accreting White Dwarfs: A Review

Mukai

2017

PASP

245

212

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Interacting binaries in which a white dwarf accretes material from a companion-cataclysmic variables (CVs) in which the mass donor is a Roche-lobe filling star on or near the main sequence, and symbiotic stars in which the mass donor is a late type giant-are relatively commonplace. They display a wide range of behaviors in the optical, X-rays, and other wavelengths, which still often baffle observers and theorists alike. Here I review the existing body of research on X-ray emissions from these objects for the benefits of both experts and newcomers to the field. I provide introductions to the past and current X-ray observatories, the types of known X-ray emissions from these objects, and the data analysis techniques relevant to this field. I then summarize of our knowledge regarding the X-ray emissions from magnetic CVs, non-magnetic CVs and symbiotic stars, and novae in eruption. I also discuss space density and the X-ray luminosity functions of these binaries and their contribution to the integrated X-ray emission from the Galaxy. I then discuss open questions and future prospects.

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“…Assuming the X-ray flux of this source in quiescence is larger than ∼1.2×10 −13 erg/cm 2 /s (see Table 5), we could estimate the distance to AX J1549.8-5416 to be < ∼ 1.0 kpc. We note that neither the duty cycle nor the X-ray luminosity in quiescence are able to entirely reliably trace the mass accretion rate of the system (Britt et al 2015).…”

Section: Duty Cyclementioning

confidence: 77%

“…The observations 1, 2, 3, 5, 6 and 7 (in Table-2) are shown in black, light blue, red, green, purple and blue, respectively. (Wheatley et al 2003;Collins & Wheatley 2010;Britt et al 2015). We therefore also used an isobaric cooling flow model, mkcflow, to fit the X-ray emission from the source (Mushotzky & Szymkowiak 1988).…”

Section: X-ray Spectral Analysismentioning

confidence: 99%

“…The new optical light curves support the estimated high duty cycle in AX J1549.8-5416. Britt et al (2015) recently measured the duty cycles for an existing sample of well-observed, nearby DNe and derived a quantitative empirical relation between the duty cycle of DNe outbursts and the X-ray luminosity of the system in quiescence. If we assume this relationship also applies to AX J1549.8-5416, the estimated ∼50% duty cycle suggests the X-ray luminosity of this system should be larger than 10 32 erg/s in quiescence.…”

Section: Duty Cyclementioning

confidence: 99%

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Multiwavelength monitoring of a very active dwarf nova AX J1549.8−5416 with an unusually high duty cycle

Zhang¹,

Gelfand

Russell³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the results of our analysis of new optical, ultraviolet (UV) and X-ray observations of a highly variable source − AX J1549.8-5416. Both the detection of several fast rise, exponential decay outbursts in the optical light curve and the lack of He II emission lines in the optical spectra suggest AX J1549.8-5416 is a cataclysmic variable of the dwarf nova (DN) type. The multiwavelength analysis of three mini-outbursts and one normal outburst represent one of the most complete multiwavelength studies of a DN and help to refine the relationship between the X-ray, UV and optical emission in this system. We find that the UV emission is delayed with respect to the optical by 1.0−5.4 days during the rising phase of the outburst. The X-ray emission is suppressed during the peak of the optical outburst and recovers during the end of the outburst. From our analysis of archival Swift, Chandra and XMM-Newton observations of AX J1549.8-5416, we estimate this DN has a high duty cycle (∼ 50%), suggesting a quiescent X-ray luminosity larger than 10 32 erg/s. We also find the X-ray and UV flux are roughly anti-correlated. Furthermore, we find that, at low X-ray fluxes, the X-ray spectrum is well described by a single temperature thermal plasma model, while at high X-ray fluxes, an isobaric cooling flow model also works. We find that the maximum temperature of the plasma in quiescence is significantly higher than that in outburst.

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The relationship between X-ray luminosity and duty cycle for dwarf novae and their specific frequency in the inner Galaxy

Cited by 20 publications

References 63 publications

Distances of cataclysmic variables and related objects derived fromGaiaData Release 1

Distances of cataclysmic variables and related objects derived fromGaiaData Release 1

X-Ray Emissions from Accreting White Dwarfs: A Review

Multiwavelength monitoring of a very active dwarf nova AX J1549.8−5416 with an unusually high duty cycle

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