Metallicity and effective temperature of the secondary of RS Ophiuchi

Pavlenko, Ya. V.; Evans, A.; Kerr, T. H.; Yakovina, L. A.; Woodward, C. E.; Lynch, D. K.; Rudy, R. J.; Pearson, R.L.; Russell, R. W.

doi:10.1051/0004-6361:20078622

Cited by 26 publications

(43 citation statements)

References 30 publications

(24 reference statements)

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“…The count rate on day 26.1 is significantly lower than that on day 13.8, and the shape of the continuum is different. On day 26.1, a new component is observed longward of ∼ 20 Å (Nelson et al 2008) that could be associated with the SSS spectrum that was clearly detected three days later with Swift (Osborne et al 2008). However, the spectral shape of this new component on day 26.1 is quite different from the spectra observed on days 39.7, 54.0, and 66.9 (next three panels).…”

Section: Description Of Spectramentioning

confidence: 79%

“…The SSS phase was observed after day ∼ 30 and ended before day ∼ 100 after outburst (Osborne et al 2008). Three highresolution X-ray spectra were taken during this phase which are described by Ness et al (2007).…”

Section: Introductionmentioning

confidence: 99%

“…In contrast to classical novae, the resulting blast wave is expected to result in copious early X-ray emission (Bode & Kahn 1985). The composition of the red giant was studied by Pavlenko et al (2008), who found that the overall metallicity does not seem to be significantly different from solar ([Fe/H] HIGH-RESOLUTION X-RAY SPECTROSCOPY 3415 (Shore et al 1996). Lines of C were observed, but no detailed abundance analyses were carried out by Shore et al (1996).…”

Section: Introductionmentioning

confidence: 99%

“…Contini et al (1995) found significant underabundance of O/H and Ne/H of ∼10% solar but high abundance ratios of Mg/Fe = 5.4 and Si/Fe = 7.2. During the first month after outburst, intense hard X-ray emission, that originated from the shock, was observed with Swift and the Rossi X-ray Timing Explorer (RXTE; Bode et al 2006;Osborne et al 2008;Sokoloski et al 2006). Swift X-Ray Telescope (XRT) observations carried out between days 3 and 26 were analyzed by Bode et al (2006) who applied singletemperature Mewe-Kaastra-Liedahl (MEKAL) models to the X-ray spectra.…”

Section: Introductionmentioning

confidence: 99%

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High-Resolution X-Ray Spectroscopy of the Evolving Shock in the 2006 Outburst of Rs Ophiuchi

Ness¹,

Drake²,

Starrfield³

et al. 2009

The Astronomical Journal

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The evolution of the 2006 outburst of the recurrent nova RS Ophiuchi was followed with 12 X-ray grating observations with Chandra and XMM-Newton. We present detailed spectral analyses using two independent approaches. From the best data set, taken on day 13.8 after outburst, we reconstruct the temperature distribution and derive elemental abundances. We find evidence for at least two distinct temperature components on day 13.8 and a reduction of temperature with time. The X-ray flux decreases as a power law, and the powerlaw index changes from −5/3 to −8/3 around day 70 after outburst. This can be explained by different decay mechanisms for the hot and cool components. The decay of the hot component and the decrease in temperature are consistent with radiative cooling, while the decay of the cool component can be explained by the expansion of the ejecta. We find overabundances of N and of α elements, which could either represent the composition of the secondary that provides the accreted material or that of the ejecta. The N overabundance indicates CNO-cycled material. From comparisons to abundances for the secondary taken from the literature, we conclude that 20%-40% of the observed nitrogen could originate from the outburst. The overabundance of the α elements is not typical for stars of the spectral type of the secondary in the RS Oph system, and white dwarf material might have been mixed into the ejecta. However, no direct measurements of the α elements in the secondary are available, and the continuous accretion may have changed the observable surface composition.

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Section: Description Of Spectramentioning

confidence: 79%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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High-Resolution X-Ray Spectroscopy of the Evolving Shock in the 2006 Outburst of Rs Ophiuchi

Ness¹,

Drake²,

Starrfield³

et al. 2009

The Astronomical Journal

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“…Livio & Truran 1994;Schwarz et al 2001Schwarz et al , 2007. Although N is also enhanced in the atmosphere of the red giant component of RS Oph ([N/H]=0.6±0.3), its moderate C/N=0.16 (Pavlenko et al 2008) indicates this N enhancement is not as strong as that in the nova ejecta. Systematic studies of photospheric abundances of a few dozens symbiotic giants revealed N/O 0.5 and C/N 0.2, and they are consistent with moderate enhancement of N and depletion of C as expected for their evolutionary stage (Ga lan et al 2016(Ga lan et al , 2017.…”

Section: Uv and Optical Spectroscopymentioning

confidence: 96%

The Massive CO White Dwarf in the Symbiotic Recurrent Nova RS Ophiuchi

Mikołajewska

Shara

2017

ApJ

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If accreting white dwarfs (WD) in binary systems are to produce type Ia supernovae (SNIa), they must grow to nearly the Chandrasekhar mass and ignite carbon burning. Proving conclusively that a WD has grown substantially since its birth is a challenging task. Slow accretion of hydrogen inevitably leads to the erosion, rather than the growth of WDs. Rapid hydrogen accretion does lead to growth of a helium layer, due to both decreased degeneracy and the inhibition of mixing of the accreted hydrogen with the underlying WD. However, until recently, simulations of helium-accreting WDs all claimed to show the explosive ejection of a helium envelope once it exceeded ∼ 10 −1 M ⊙ . Because CO WDs cannot be born with masses in excess of ∼ 1.1 M ⊙ , any such object, in excess of ∼ 1.2 M ⊙ , must have grown substantially. We demonstrate that the WD in the symbiotic nova RS Oph is in the mass range 1.2-1.4 M ⊙ . We compare UV spectra of RS Oph with those of novae with ONe WDs, and with novae erupting on CO WDs. The RS Oph WD is clearly made of CO, demonstrating that it has grown substantially since birth. It is a prime candidate to eventually produce an SNIa.

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Multiwavelength modeling the SED of supersoft X-ray sources. II. RS Ophiuchi: From the explosion to the SSS phase

Skopal

2015

New Astronomy

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Physical parameters of the nova RS Oph were determined from its X-ray/IR spectrum. -The model revealed the presence of a strong stellar and nebular component. -The luminosity was super-Eddington during the whole burning phase. -The high luminosity was sustained by a super-critical accretion.Abstract RS Oph is a recurrent symbiotic nova that undergoes nova-like outbursts on a time scale of 20 years. Its two last eruptions (1985 and 2006) were subject of intensive multiwavelengths observational campaign from the X-rays to the radio. This contribution aims to determine physical parameters and the ionization structure of the nova from its explosion to the first emergence of the supersoft X-rays (day 26) by using the method of multiwavelength modelling the SED. From the very beginning of the eruption, the model SED revealed the presence of both a strong stellar and nebular component of radiation in the spectrum. During the first 4 days, the nova evinced a biconical ionization structure. The ∼ 8200 K warm and 160-200 R⊙ extended pseudophotosphere encompassed the white dwarf (WD) around its equator to the latitude > 40 • . The remaining space around the WD's poles was ionized, producing a strong nebular continuum with the emission measure EM ∼ 2.3 × 10 62 cm −3 via the fast wind from the WD. The luminosity of the burning WD was highly super-Eddington for the whole investigated period. The wind mass loss at rates of 10 −4 − 10 −5 M⊙ yr −1 and the presence of jets suggest an accretion throughout a disk at a high rate, which can help to sustain the super-Eddington luminosity of the accretor for a long time.

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Metallicity and effective temperature of the secondary of RS Ophiuchi

Cited by 26 publications

References 30 publications

High-Resolution X-Ray Spectroscopy of the Evolving Shock in the 2006 Outburst of Rs Ophiuchi

High-Resolution X-Ray Spectroscopy of the Evolving Shock in the 2006 Outburst of Rs Ophiuchi

The Massive CO White Dwarf in the Symbiotic Recurrent Nova RS Ophiuchi

Multiwavelength modeling the SED of supersoft X-ray sources. II. RS Ophiuchi: From the explosion to the SSS phase

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