The orbital period and system parameters of the recurrent nova T Pyx

Uthas, H.; Knigge, Christian; Steeghs, D.

doi:10.1111/j.1365-2966.2010.17046.x

Cited by 49 publications

(92 citation statements)

References 33 publications

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“…2 In their orbital solution of T Pyx using the He II 4686 Å emission line during quiescence, Uthas et al (2010) were unable to derive a definitive systematic velocity for the nova but all of their solutions were at a velocity lower than +20 km s −1 . We suggest that there may be a residual uncertainty caused by the profile of the He II line and/or shell emission that compromises the center-of-mass velocity but not the amplitude of the variations, 17.9 ± 1.6 km s −1 .…”

Section: Distance and Extinction Estimatesmentioning

confidence: 99%

“…Using the Galactic rotation curve for the third quadrant (Brand & Blitz 1993) we find a minimum distance consistent with previous estimates, 4.0 kpc, for Θ 0 = 220 km s −1 based on the radial velocity v rad of the interstellar CH 4300 Å line. The center of mass velocity of the binary is still uncertain and may be variable (Uthas et al 2010) but there may be another way of obtaining it. In the JD 55 712 spectrum, the emission lines (e.g., Fe II RMT 42, H Balmer) show two nearly symmetric emission peaks, and the same holds for the weak emergent [O I] 5577, 6300 Å emission lines with a separation of about 700 km s −1 and mean velocity of +60 ± 3 km s −1 2 .…”

Section: Distance and Extinction Estimatesmentioning

confidence: 99%

“…14.29 (JD 2 455 665.79,IAUC 9205). The orbital period was determined by Uthas et al (2010) to be 1.83 h by Appendices are available in electronic form at http://www.aanda.org spectroscopy during the hiatus interval. They derived a WD mass of M WD = 0.7 ± 0.2 M .…”

Section: Introductionmentioning

confidence: 99%

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The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst

Shore

Augusteijn

Ederoclite

et al. 2011

A&A

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Aims. We aim to derive the physical properties of the recurrent nova T Pyx and the structure of the ejecta during the early stages of expansion of the 2011 outburst. Methods. The nova was observed with high resolution spectroscopy (R ≈ 65 000), from one day after discovery of the outburst and until the last visibility of the star at the end of May 2011. The interstellar absorption lines of Na I, Ca II, CH, CH + , and archival H I 21 cm emission line observations were used to determine a kinematical distance. Interstellar diffuse absorption features have been used to determine the extinction independent of previous assumptions. Sample Fe-peak line profiles show the optical depth and radial velocity evolution of the discrete components. Results. We propose a distance to T Pyx ≥ 4.5 kpc, with a strict lower limit of 3.5 kpc (the previously accepted distance). We derive an extinction, E(B − V) ≈ 0.5 ± 0.1, that is higher than previous estimates. The first observation, Apr. 15, displayed He I, He II, C III, and N III emission lines and a maximum velocity derived from the P Cyg profiles of the Balmer and He I lines of ≈2500 km s −1 that is characteristic of the fireball stage. These ions were undetectable in the second spectrum, Apr. 23, and we use the recombination time to estimate the mass of the ejecta, 10 −5 f M for a filling factor f . Numerous absorption-line systems were detected in the Balmer, Fe-peak, Ca II, and Na I lines, mirrored in broader emission-line components, that showed an "accelerated" displacement in velocity. We also show that the time sequence of these absorptions, which are common to all lines and arise only in the ejecta, can be described by a recombination front moving outward in the expanding gas without either a stellar wind or circumstellar collisions. By the end of May, the ejecta were showing signs of turning optically thin in the ultraviolet.

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Section: Distance and Extinction Estimatesmentioning

confidence: 99%

Section: Distance and Extinction Estimatesmentioning

confidence: 99%

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The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst

Shore

Augusteijn

Ederoclite

et al. 2011

A&A

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“…They find that after day 28 the AMBER K-band and PIONIER-H band visibilities are consistent with a two-component bipolar plus central point source model with very low inclination. In light of the uncertainties in the orbital inclination from Uthas et al (2010), we set our constraints based on the interferometry.…”

Section: Modeling the Structure Of The Ejectamentioning

confidence: 99%

The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst

Shore

Schwarz

Aquino

et al. 2013

A&A

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“…For a nonmagnetic CV, the virial temperature in the inner parts of the accretion disk (kT virial = μm p GM WD /3R WD ) is kT virial = 20−29 keV for a 0.7−1.0 M WD (WD mass is from Uthas et al 2010;and Toffelmeier et al 2013). The X-ray temperatures in Table 1 show that the flow is already virialized.…”

Section: The Chandra Spectrum Of the Total Observationmentioning

confidence: 99%

Pre-outburstChandraobservations of the recurrent nova T Pyxidis

Balman

2014

A&A

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Aims. I study the spectral, temporal, and spatial characteristics of the quiescent X-ray emission (not in outburst) of the recurrent nova T Pyx. Methods. I performed the spectral analysis of the X-ray data obtained using the Chandra Observatory, Advanced CCD Imaging Spectrometer (ACIS-S3) detector. I fit the spectra with several models that describe plasma emission characteristics. In addition, I calculated the light curve of the data and performed power spectral analysis using Fourier transform. Finally, I did high-resolution imaging analysis of the data at the subpixel level and produced radial surface brightness profiles.Results. I present a total of 98.8 ks (∼3 × 30 ks) observation of T Pyx obtained with the ACIS-S3 detector onboard the Chandra Observatory obtained during the quiescent phase, about 2−3 months before its outburst in April 2011. The total Chandra spectrum of the source T Pyx gives a maximum temperature kT max > 37.0 keV (2σ lower limit) with (0.9−1.5) × 10 −13 erg s −1 cm −2 and (1.3−2.2) × 10 32 erg s −1 (at 3.5 kpc) in the 0.1−50 keV range using a multitemperature plasma emission model with a power-law distribution of temperatures (i.e., CEVMKL in XSPEC). I find a ratio of (L x /L disk ) (2−7) × 10 −4 and the ratio is smaller if L disk is higher than 3 × 10 35 erg s −1 indicating considerable inefficiency of emission in the boundary layer. There is no soft X-ray blackbody emission from T Pyx with a 2σ upper limit on the blackbody temperature and the flux/luminosity as kT BB < 25 eV and L soft < 2.0 × 10 33 erg s −1 in the 0.1−10.0 keV band. All fits yield only interstellar N H during quiescence. I suggest that T Pyx has an optically thin boundary layer merged with an advection-dominated accretion flow and/or X-ray corona in the inner disk indicating ongoing quasi-spherical accretion at (very) high rates during quiescent phases. Such a boundary layer structure may be excessively heating the white dwarf, influencing the thermonuclear runaway leading to the recurrent nova events. The orbital period of the system is detected in the power spectrum of the Chandra light curves with no energy dependence over the orbit. The central source (i.e., the binary system) emission and its spectrum is deconvolved from any possible extended emission with a long and detailed procedure at the subpixel level revealing an extended emission with S /N ∼ 6−10. The derived shape looks like an elliptical nebula with a semi-major axis ∼1.0 arcsec and a semi-minor axis ∼0.5 arcsec, also indicating an elongation towards south. The calculated approximate count rate of the extended emission is 0.0013−0.0025 c s −1 . The luminosity (within errors) of the nebula is ∼(0.6−30.0) × 10 31 erg s −1 (at 3.5 kpc) mostly correct towards the lower end of the range. The nebulosity seems consistent with an interaction of the outflow/ejecta from the 1966 outburst.

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The orbital period and system parameters of the recurrent nova T Pyx

Cited by 49 publications

References 33 publications

The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst

The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst

The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst

Pre-outburstChandraobservations of the recurrent nova T Pyxidis

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