A Universal Decline Law of Classical Novae. III. GQ Muscae 1983

Hachisu, Izumi; Kato, Mariko; Cassatella, A.

doi:10.1086/591415

Cited by 35 publications

(87 citation statements)

References 64 publications

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“…The nova is a known super soft X-ray source (Schwarz et al 2011, and references therein). Hachisu et al (2008) estimate the mass of the white dwarf in the system to be 0.7 ± 0.05 M . A spectrum of the remnant, obtained in 1994, is A119, page 6 of 24 shown by Diaz et al (1995).…”

Section: Gq Musmentioning

confidence: 97%

SALT observations of southern post-novae

Tomov

Swierczynski

Mikołajewski

et al. 2015

A&A

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Aims. We report on recent optical observations of the stellar and the nebular remnants of 22 southern post-novae. Methods. In this study, for each of our targets, we obtained and analysed long-slit spectra in the spectral range 3500-6600 Å and inResults. The changes in the emission lines' equivalent widths with the time since the outburst agree with earlier published results of other authors. We estimated an average value α = 2.37 for the exponent of the power law fitted to the post-novae continua. Our observations clearly show the two-component structure of the V842 Cen expanding nebulae, owing to the different velocities of the ejected matter. We discovered an expanding shell around V382 Vel with an outer diameter of about 12 .

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Section: Gq Musmentioning

confidence: 97%

SALT observations of southern post-novae

Tomov

Swierczynski

Mikołajewski

et al. 2015

A&A

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“…Mass measurements of astronomical objects are notoriously difficult and highly uncertain, but are still worth considering. Most of our mass measurements come from a series of light curve model papers by I. Hachisu and M. Kato [Hachisu & Kato(2004), Hachisu & Kato(2005), Hachisu & Kato(2006), , Hachisu et al(2008b), Hachisu et al(2008a), ), Hachisu & Kato(2010, Kato & Hachisu(2003), , , Kato & Hachisu(2011)]. In our time-limited sample, we have 27 CNe with M WD measurements, and of those 27, seven have M WD ≥ 1.2M , for 26%.…”

Section: Characteristics Of Recurrent Novaementioning

confidence: 99%

Recurrent Novae: A Masquerade

Pagnotta¹

2017

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects - III — PoS(Golden2015)

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Due to low discovery efficiencies, there must be some number of classical novae (CNe) that are in fact recurrent novae (RNe) for which only one eruption has so far been observed. We collect all available information on the light curves, spectra, and quiescent characteristics of a time-limited sample of 237 Galactic CNe and the ten known Galactic RNe, and identify seven characteristics that are indicative of a short recurrence time: (1) outburst amplitude smaller than 14.5 − 4.5 × log(t 3 ), (2) orbital period >0.6 days, (3) infrared colors of J − H > 0.7 mag and H − K > 0.1 mag, (4) FWHM of Hα > 2000 km s −1 , (5) high excitation lines, such as Fe X or He II, near peak, (6) eruption light curves with a plateau, and (7) white dwarf mass greater than 1.2M . We use these characteristics to identify good RN candidates from among the list of known CNe and to draw conclusions about the population of Galactic RNe, specifically related to whether there are enough RNe to provide the observed Type Ia supernova rate, as RNe are good candidate progenitors. We find that 25% ± 10% of CNe are likely RNe with only one eruption observed so far, and that RNe could perhaps provide up to one half of the Type Ia supernovae. and collects information on novae that were not included in the original paper but were of interest to other conference attendees.

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“…Similar values were reported by Krautter et al (1984) and Hassall et al (1990), who found E(B − V ) = 0.45 and 0.50, respectively, on the basis of the 2175 Å feature in the early IUE spectra. Hachisu et al (2008) obtained E(B − V ) = 0.55 ± 0.05 on the basis of the 2175Å feature and various line ratios. redetermined the color excess to be E(B − V ) = 0.45 ± 0.05 by fitting the general tracks with that of GQ Mus in the UBV color-color diagram.…”

Section: V705 Cas 1993mentioning

confidence: 99%

“…As far as the free-free emission dominates the continuum spectra, we can expect that novae follow the universal decline law. Even if there are wavy-structured or dust-blackout shapes, the overall light curves follow the universal decline law (e.g., , 2010Hachisu et al 2008; ). On the other hand, if photospheric emission dominates the nova continuum spectra, light curves do not follow the universal decline law.…”

Section: Analysis On Various Light Curve Shapes Of Classical Novaementioning

confidence: 99%

“…also found that their UV 1455 Å model light curves (Cassatella et al 2002), interpreted as photospheric blackbody emission, are also time-normalized by the same factor as in the optical and NIR light curves. Using the fact that the time-scaling factor is closely related to the WD mass, the authors determined the WD mass and other parameters for a number of well-observed novae (e.g., , 2010Hachisu et al 2008;). …”

Section: Introductionmentioning

confidence: 99%

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Light curve analysis of classical novae: free-free emission vs photospheric emission

Hachisu¹,

Kato²

2017

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects - III — PoS(Golden2015)

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We analyzed light curves of seven relatively slower novae, PW Vul, V705 Cas, GQ Mus, RR Pic, V5558 Sgr, HR Del, and V723 Cas, based on an optically thick wind theory of nova outbursts. For fast novae, free-free emission dominates the spectrum in optical bands rather than photospheric emission and nova optical light curves follow the universal decline law. Faster novae blow stronger winds with larger mass loss rates. Since the brightness of free-free emission depends directly on the wind mass loss rate, faster novae show brighter optical maxima. In slower novae, however, we must take into account photospheric emission because of their lower wind mass loss rates. We calculated three model light curves of free-free emission, photospheric emission, and the sum of them for various WD masses with various chemical compositions of their envelopes, and fitted reasonably with observational data of optical, near-IR (NIR), and UV bands. From light curve fittings of the seven novae, we estimated their absolute magnitudes, distances, and WD masses. In PW Vul and V705 Cas, free-free emission still dominates the spectrum in the optical and NIR bands. In the very slow novae, RR Pic, V5558 Sgr, HR Del, and V723 Cas, photospheric emission dominates the spectrum rather than free-free emission, which makes a deviation from the universal decline law. We have confirmed that the absolute brightnesses of our model light curves are consistent with the distance moduli of four classical novae with known distances (GK Per, V603 Aql, RR Pic, and DQ Her). We also discussed the reason why the very slow novae are about ∼ 1 mag brighter than the proposed maximum magnitude vs. rate of decline relation.

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A Universal Decline Law of Classical Novae. III. GQ Muscae 1983

Cited by 35 publications

References 64 publications

SALT observations of southern post-novae

SALT observations of southern post-novae

Recurrent Novae: A Masquerade

Light curve analysis of classical novae: free-free emission vs photospheric emission

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