SALT observations of southern post-novae

Tomov, T.; Swierczynski, E.; Mikołajewski, M.; Iłkiewicz, Krystian

doi:10.1051/0004-6361/201424709

Cited by 17 publications

(32 citation statements)

References 108 publications

(242 reference statements)

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“…The optical spectrum (see Bianchini et al 1991, and Liu & Hu (2000) shows weak hydrogen and HeII 4686 emission lines. A recent SALT spectrum of GI Mon (Tomov et al 2015) also shows weak HeII 4686 and H-beta emission lines. The equivalent width of H-alpha suggests a moderately low inclination.…”

Section: Comments On the Inclination Of Individual Objectsmentioning

confidence: 98%

A UV and optical study of 18 old novae with Gaia DR2 distances: mass accretion rates, physical parameters, and MMRD

Selvelli

Gilmozzi²

2019

A&A

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We combine the results of our earlier study of the UV characteristics of 18 classical novae (CNe) with data from the literature and with the recent precise distance determinations from the Gaia satellite to investigate the statistical properties of old novae. All final parameters for the sample include a detailed treatment of the errors and their propagation. The physical properties reported here include the absolute magnitudes at maximum and minimum, a new maximum magnitude versus rate of decline (MMRD) relation, and the inclination-corrected 1100-6000-Å accretion disk luminosity. Most importantly, these data have allowed us to derive a homogenous set of accretion rates in quiescence for the 18 novae. All novae in the sample were super-Eddington during outburst, with an average absolute magnitude at maximum of −7.5 ± 1.0. The average absolute magnitude at minimum corrected for inclination is 3.9 ± 1.0. The median mass accretion rate is logṀ 1M = −8.52 (using 1M as WD mass for all novae) or logṀ M WD = −8.48 (using the individual WD masses). These values are lower than those assumed in studies of CNe evolution and appear to attenuate the need for a hibernation hypothesis to interpret the nova phenomenon. We identified a number of correlations among the physical parameters of the quiescent and eruptive phases, some already known but others new and even surprising. Several quantities correlate with the speed class t 3 including, unexpectedly, the mass accretion rate (Ṁ). This rate correlates also with the absolute magnitude at minimum corrected for inclination, and with the outburst amplitude, providing new and simple ways to estimateṀ through its functional dependence on (more) easily observed quantities. There is no correlation betweenṀ and the orbital period.It should be stressed, however, that reliable statements abouṫ M -the non plus ultra of binary evolution according to Patterson (2011) -can be found only for objects with welldetermined distance and reddening, and by observations covering the satellite UV range (hereafter, simply UV) because the bulk of the accretion luminosity is emitted in this spectral region (Wade & Hubeny 1998). The homogeneous UV data on spectral energy distributions (SEDs) in Paper I are therefore of high relevance for this topic, and since old novae are (unlike other CVs, e.g., DNe) nearly stable accretors (Honeycutt et al 1998;Retter & Naylor 2000;Puebla et al 2007) their accretion luminosity anḋ M can be determined with higher precision.We note that throughout this paper accretion rate is used to indicate the mass transfer rate through the disk (the one that we derive from the observed disk luminosity). Other kinds of accretion rates that may be at play in these systems, for example the mass-loss rate from the donor, the accretion rate on to the WD, or the mass loss from the disk (e.g., via a wind or outflow through the boundary layer) cannot be determined from our data, and should not be confused with the accretion through the disk.In Paper I (Selvelli and Gilmozzi, 2013), we stud...

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Section: Comments On the Inclination Of Individual Objectsmentioning

confidence: 98%

A UV and optical study of 18 old novae with Gaia DR2 distances: mass accretion rates, physical parameters, and MMRD

Selvelli

Gilmozzi²

2019

A&A

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“…Tarasova & Shakhovskoi (2013) reported that the spectral energy distribution (SED) of their pre-maximum spectrum, taken on Aug. 15.8, was similar to a late-A or early-F-type spectrum. The line spectrum, which was dominated by P Cyg-type hydrogen lines with a pronounced absorption component (see Shore et al 2013a;Tomov et al 2013;Tarasova 2013;Munari et al 2013b), also suggested that the effective temperature of the envelope probably is 10 4 K. During Aug. 19, observed a significant weakening of the H i absorption components, while those of the Fe ii, He i, and O i profiles were still clearly present. This evolution indicated a distinctive cooling of the expanding envelope.…”

Section: Introductionmentioning

confidence: 94%

Early evolution of the extraordinary Nova Delphini 2013 (V339 Del)

Skopal

Drechsel

Тарасова

et al. 2014

A&A

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Aims. We determine the temporal evolution of the luminosity (L WD ), radius (R WD ) and effective temperature (T eff ) of the white dwarf (WD) pseudophotosphere of V339 Del from its discovery to around day 40. Another main objective was studying the ionization structure of the ejecta. Methods. These aims were achieved by modelling the optical/near-IR spectral energy distribution (SED) using low-resolution spectroscopy (3500-9200 Å), UBVR C I C and JHKLM photometry. Important insights in the physical conditions of the ejecta were gained from an analysis of the evolution of the Hα and Raman-scattered 6825 Å O vi line using medium-resolution spectroscopy (R ∼ 10 000). Results. During the fireball stage (Aug. 14. 8-19.9, 2013), T eff was in the range of 6000-12 000 K, R WD was expanding non-uniformly in time from ∼66 to ∼300 (d/3 kpc) R , and L WD was super-Eddington, but not constant. Its maximum of ∼9 × 10 38 (d/3 kpc) 2 erg s −1 occurred around Aug. 16.0, at the maximum of T eff , half a day before the visual maximum. After the fireball stage, a large emission measure of 1.0−2.0×10 62 (d/3 kpc) 2 cm −3 constrained the lower limit of L WD to be well above the super-Eddington value. The mass of the ionized region was a few ×10 −4 M , and the mass-loss rate was decreasing from ∼5.7 (Aug. 22) to ∼0.71× 10 −4 M yr −1 (Sept. 20).The evolution of the Hα line and mainly the transient emergence of the Raman-scattered O vi 1032 Å line suggested a biconical ionization structure of the ejecta with a disk-like H i region persisting around the WD until its total ionization, around day 40. On Sept. 20 (day 35), the model SED indicated a dust emission component in the spectrum. The dust was located beyond the H i zone, where it was shielded from the hard, > ∼ 10 5 K, radiation of the burning WD at that time. Conclusions. Our extensive spectroscopic observations of the classical nova V339 Del allowed us to map its evolution from the very early phase after its explosion. It is evident that the nova was not evolving according to the current theoretical prediction. The unusual non-spherically symmetric ejecta of nova V339 Del and its extreme physical conditions and evolution during and after the fireball stage represent interesting new challenges for the theoretical modelling of the nova phenomenon.

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“…We have estimated that the flux loss due to the broad line wings and the limited width of the narrow band filters is less than 10% for both bands, using previous spectroscopic observations (Tomov et al 2015). Such loss is not relevant when compared to other uncertainties in our models.…”

Section: Line Fluxes and Dereddeningmentioning

confidence: 92%

“…The major and minor axes are 9.9 arcsec and 8.9 arcsec, respectively, with a mean value of 9.4 arcsec (see figure 2). Tomov et al (2015) measured an angular diameter of 12 arcsec for the shell from their Hα+[N II] narrow band imaging with Fabry-Perot Robert Stobie Spectrograph at SALT.…”

Section: Angular Diametermentioning

confidence: 99%

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Imaging and Analysis of Neon Nova V382 Vel Shell

Takeda

Diaz

2019

PASP

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We present the detection and imaging of the spatially resolved shell of nova V382 Vel with SOAR adaptive optics module (SAM). The shell was observed in narrow band filters Hα and [O III] 5007Å revealing different structures in each filter. The shell's angular diameter obtained was 9.9 arcsec, equivalent to 2.8 × 10 17 cm, using the distance of 1.79 kpc obtained by Gaia mission. The upper limit for total shell mass derived from recombination lines is M s = 1.4 × 10 −4 M ⊙ . Our photoionization models indicate an accretion disk with T d = 60, 000 K and L=10 36 erg/s as main ionizing source.

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SALT observations of southern post-novae

Cited by 17 publications

References 108 publications

A UV and optical study of 18 old novae with Gaia DR2 distances: mass accretion rates, physical parameters, and MMRD

A UV and optical study of 18 old novae with Gaia DR2 distances: mass accretion rates, physical parameters, and MMRD

Early evolution of the extraordinary Nova Delphini 2013 (V339 Del)

Imaging and Analysis of Neon Nova V382 Vel Shell

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