A long term spectroscopic and photometric study of the old nova HR Delphini

Friedjung, M.; Dennefeld, M.; Voloshina, I.

doi:10.1051/0004-6361/200913936

Cited by 9 publications

(12 citation statements)

References 21 publications

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“…The highṀ is close to the value (10 −7 · M yr −1 ) that would correspond to the steady-burning regime (see Fujimoto 1982;Nomoto 1982;Nomoto et al 2007;Iben & Fujimoto in Bode & Evans 2008). The reason for this continuing activity is not clear, but continuing weak thermonuclear burning may be involved (Friedjung et al 2010). This peculiar behavior was pointed out by Selvelli & Friedjung (2007) who interpreted the presence of a strong P Cyg profile in the CIV λ 1550 resonance doublet as indicative of a strong steady outflow driven by the high disk luminosity.…”

Section: Comments On Individual Objectsmentioning

confidence: 99%

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 Individual Objectsmentioning

confidence: 99%

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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“…de Young & Schmidt 1994) and in post common envelope binaries (e.g Somers et al 1996). As discussed by Friedjung et al (2010), it is very likely that, in the case of HR Del, the photometric variations in the WASP data are due to irradiation of the cool secondary by the white dwarf.…”

Section: Data and Resultsmentioning

confidence: 97%

“…Friedjung, Dennefeld & Voloshina (2010) have carried out a photometric study of this object; their observations, in the UBV bands, were carried out intermittently over the period 2002–2008. For B ‐band data obtained around 1990 they found a ∼0.1 mag amplitude variation with period at the orbital period, which they attributed to orbital modulation.…”

Section: Data and Resultsmentioning

confidence: 99%

Novae in the SuperWASP data base

McQuillin

Evans

Wilson

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We present the results of trawling through the SuperWASP data base for classical and recurrent novae. We report light curves for a nova in eruption, and for classical novae and a recurrent nova in quiescence. For five objects in quiescence, we report periodicity, arising in most cases from orbital modulation of the light from the cool secondary star. The stability of the SuperWASP system means that these data have huge potential for the study not only of novae in eruption, but also of the long-term modulations of light during quiescence.

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“…Results from a preliminary study were presented by Friedjung et al (2005). Here we present mainly the results of our complete photometric observations of this object.…”

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confidence: 92%

A progress report on the study of the optical variability of the old nova HR Del

Voloshina¹

2009

cia

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The cataclysmic variable and old nova HR Del has been studied using ground-based photometry and spectroscopy over a period of more than 6 years. Some long term variations have been found, but no clear correlation established up to now between photometric, and spectroscopic changes. HR Del (or Nova Del 1967) was a bright classical nova with however unusual properties. It brightened in July 1967 to a magnitude near 5 m .5 from pre-outburst magnitude of about 12 m . After remaining 5 months near this magnitude, it brightened to a maximum mv ∼ 3.5, followed by an extremely slow irregular decline. The unusual nature of this nova might be due to the presence of a wind which was optically thin in the continuum before maximum, and whose velocity decreased during that stage, unlike that of the optically thick winds normally seen after maximum of classical novae (Friedjung 1992). The mass of the white dwarf component is low -(0.55 ÷ 0.75)M -, while the orbital period is 0 d .214165 (Kürster & Barwig 1988). HR Del was unusually bright both before and long after its outburst (Selvelli & Friedjung 2003). Two kinds of photometric observations were made:• To construct the overall light curve, daily estimates of HR Del's magnitude were made with the UBV photometer on the 60-cm telescope of the Sternberg Astronomical Institute in Crimea (time resolution 10 s). They covered the years 2001 -2006, with more than 1000 measurements in 3 bands.• To study the short-term variability of HR Del, observations with an Ap47 CCD detector on the same telescope were obtained in 2005 -2006, covering 23 nights, and containing more than 3500 measurements, with a time resolution of 30 s in the V band.• High-resolution spectroscopic observations of the region of the Hα line were obtained with the 152-cm telescope of the Haute Provence Observatory.

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A long term spectroscopic and photometric study of the old nova HR Delphini

Cited by 9 publications

References 21 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

Novae in the SuperWASP data base

A progress report on the study of the optical variability of the old nova HR Del

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