Spectroscopy From the Hubble Space Telescope Cosmic Origins Spectrograph  of the Southern Nova-Like Bb Doradus in an Intermediate State

Godon, Patrick; Sion, E. M.; Gänsicke, B. T.; Hubený, I.; Martino, D. de; Pala, A. F.; Rodríguez‐Gil, P.; Szkody, Paula; Toloza, Odette

doi:10.3847/1538-4357/833/2/146

Cited by 4 publications

(3 citation statements)

References 37 publications

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“…Our spectral modeling tools and technique have been previously described extensively in numerous works such as Godon et al (2012Godon et al ( , 2016, as a consequence, we limit ourselves here to a brief description of the modeling but include a comprehensive account of the recent improvements we made over our previous UV spectral analysis of T Pyx in (Godon et al 2014).…”

Section: Modelingmentioning

confidence: 99%

The Long-term Secular Mass Accretion Rate of the Recurrent Nova T Pyxidis*

Godon

Sion

Williams

et al. 2018

ApJ

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We present Hubble Space Telescope ultraviolet spectroscopy of the recurrent nova T Pyxidis obtained more than 5 years after its 2011 outburst indicating that the system might not have yet reached its deep quiescent state. The ultraviolet data exhibit a 20% decline in the continuum flux from the preoutburst deep quiescence state to the post-outburst near quiescent state. We suggest that a decline across each recurring nova eruption might help explain the proposed 2 mag steady decline of the system since 1866 (Schaefer et al. 2010). Using an improved version of our accretion disk model as well as International Ultraviolet Explorer ultraviolet and optical data, and the 4.8 kpc distance derived by Sokoloski et al. (2013) (and confirmed by De Gennaro Aquino et al. ( 2014)), we corroborate our previous findings that the quiescent mass accretion rate in T Pyx is of the order of 10 −6 M ⊙ yr −1 . Such a large mass accretion rate would imply that the mass of the white dwarf is increasing with time. However, with the just-release Gaia DR 2 distance of ∼ 3.3 kpc (after submission of the first version of this manuscript), we find a mass accretion more in line with the estimate of Patterson et al. (2017), of the order of 10 −7 M ⊙ yr −1 . Our results predict powerful soft X-ray or extreme ultraviolet emission from the hot inner region of the high accretion rate disk. Using constraining X-ray observations and assuming the accretion disk doesn't depart too much from the standard model, we are left with two possible scenarios. The disk either emits mainly extreme ultraviolet radiation which, at a distance of 4.8 kpc, is completely absorbed by the interstellar medium, or the hot inner disk, emitting soft X-rays, is masked by the bulging disk seen at a higher inclination.

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Section: Modelingmentioning

confidence: 99%

The Long-term Secular Mass Accretion Rate of the Recurrent Nova T Pyxidis*

Godon

Sion

Williams

et al. 2018

ApJ

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“…Our fitting procedure to the dereddened COS spectrum, consists of independently fitting the spectrum with both a white dwarf and accretion disc model. A similar procedure was carried out for spectral analysis of the COS spectrum of the VY Scl novalike BB Dor Godon et al (2016), obtained in an intermediate state as part of the ongoing campain to study the accreting WD of dwarf novae and novalikes (Pala et al 2017). The best-fitting models were determined based upon a visual inspection of the model fit, consistency with the continuum slope and the Lyα region, as well as a scale-factored derived distance consistent with the published distances between 200 and 300 pc.…”

Section: Synthetic Spectra Analysismentioning

confidence: 99%

“…The WD photosphere models were constructed using temperatures of 17,000K to 30,000K in steps of 1,000K with a projected stellar rotational velocity ranging from 200km/s to 500km/s in steps of 100km/s. Additional details on our method can be found in Godon et al (2016).…”

Section: Synthetic Spectra Analysismentioning

confidence: 99%

Hubble COS Spectroscopy of the Dwarf Nova CW Mon: The White Dwarf in Quiescence?^*

Hause

Sion

Godon

et al. 2017

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We present a synthetic spectral analysis of the HST COS spectrum of the U Geminorum-type dwarf nova CW Mon, taken during quiescence as part of our COS survey of accreting white dwarfs in Cataclysmic Variables. We use synthetic photosphere and optically thick accretion disk spectra to model the COS spectrum as well as archival IUE spectra obtained decades ago when the system was in an even deeper quiescent state. Assuming a reddening of E(B-V)=0.06, an inclination of 60° (CW Mon has eclipses of the accretion disk, and a white dwarf mass of 0.8, our results indicate the presence of a 22-27,000 K white dwarf and a low mass accretion rate [Formula: see text], for a derived distance o ~200 to ~300 pc.

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VY Scl-type cataclysmic variable SDSS J154453.60+255348.8: stellar and disc parameters

Rodriguez

Zharikov

Kára

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present a new study of the eclipsing cataclysmic variable SDSS J154453.60+255348.8 to determine the object’s nature and its system parameters together with the probe of the accretion flow structure in the system. Based on analyses of new simultaneous time-resolved photometric and spectroscopic observations of SDSS J154453.60+255348.8 and using our light-curve modeling techniques and the Doppler tomography method, we found that the system contains a white dwarf with the mass of MWD = 0.62(7) M⊙ and an evolved red dwarf as a secondary. The system inclination is close to 90 deg and the mass ratio is q = 0.49(2). The secondary has an effective temperature T2 = 3 400(40) K and a radius about 1.35(15) times larger than a zero-age main sequence star with similar mass. From observation of the system in high and low brightness states, we conclude that SDSS J154453.60+255348.8 is a long orbital period VY Scl-type system. The accretion disk in the high state is about two times less than the truncation radius, and is completely missing during the low state of the system.

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Spectroscopy From the Hubble Space Telescope Cosmic Origins Spectrograph of the Southern Nova-Like Bb Doradus in an Intermediate State

Cited by 4 publications

References 37 publications

The Long-term Secular Mass Accretion Rate of the Recurrent Nova T Pyxidis*

The Long-term Secular Mass Accretion Rate of the Recurrent Nova T Pyxidis*

Hubble COS Spectroscopy of the Dwarf Nova CW Mon: The White Dwarf in Quiescence?^*

VY Scl-type cataclysmic variable SDSS J154453.60+255348.8: stellar and disc parameters

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Spectroscopy From the Hubble Space Telescope Cosmic Origins Spectrograph of the Southern Nova-Like Bb Doradus in an Intermediate State

Cited by 4 publications

References 37 publications

The Long-term Secular Mass Accretion Rate of the Recurrent Nova T Pyxidis*

The Long-term Secular Mass Accretion Rate of the Recurrent Nova T Pyxidis*

Hubble COS Spectroscopy of the Dwarf Nova CW Mon: The White Dwarf in Quiescence?*

VY Scl-type cataclysmic variable SDSS J154453.60+255348.8: stellar and disc parameters

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Product

Resources

About

Hubble COS Spectroscopy of the Dwarf Nova CW Mon: The White Dwarf in Quiescence?^*