The Distance and Morphology of V723 Cassiopeiae (Nova Cassiopeia 1995)

Lyke, James E.; Campbell, Randy

doi:10.1088/0004-6256/138/4/1090

Cited by 27 publications

(20 citation statements)

References 24 publications

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“…Heywood et al (2005) interpreted the light curve as arising from a spherical model and retrieved parameters, namely, the mass and distance to the nova. The spherical model was later shown to be incorrect when Lyke & Campbell (2009) concluded that the morphology of the ejecta was different in the different emission lines and suggested different ejection events. Lyke & Campbell (2009) also derived a revised distance to V723 Cas from the expansion parallax method, suggesting the object was much closer than that derived from Heywood et al (2005).…”

Section: Discussionmentioning

confidence: 99%

“…The spherical model was later shown to be incorrect when Lyke & Campbell (2009) concluded that the morphology of the ejecta was different in the different emission lines and suggested different ejection events. Lyke & Campbell (2009) also derived a revised distance to V723 Cas from the expansion parallax method, suggesting the object was much closer than that derived from Heywood et al (2005). We are now building models to account for these changes to update the parameters of V723 Cas (V. A. R. M. Ribeiro et al, in preparation).…”

Section: Discussionmentioning

confidence: 99%

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Radio Frequency Models of Novae in Eruption. I. The Free-Free Process in Bipolar Morphologies

Ribeiro

Chomiuk

Munari

et al. 2014

ApJ

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Observations of novae at radio frequencies provide us with a measure of the total ejected mass, density profile, and kinetic energy of a nova eruption. The radio emission is typically well characterized by the free-free emission process. Most models to date have assumed spherical symmetry for the eruption, although for as long as there have been radio observations of these systems, it has been known that spherical eruptions are too simplistic a geometry. In this paper, we build bipolar models of the nova eruption, assuming the free-free process, and show the effects of varying different parameters on the radio light curves. The parameters considered include the ratio of the minorto major-axis, the inclination angle, and shell thickness. We also show the uncertainty introduced when fitting spherical-model synthetic light curves to bipolar-model synthetic light curves. We find that the optically thick phase rises with the same power law (S ν ∝ t 2 ) for both the spherical and bipolar models. In the bipolar case, there is a "plateau" phase-depending on the thickness of the shell as well as the ratio of the minor-to major-axis-before the final decline, which follows the same power law (S ν ∝ t −3 ) as in the spherical case. Finally, fitting spherical models to the bipolar-model synthetic light curves requires, in the worst-case scenario, doubling the ejected mass, more than halving the electron temperature, and reducing the shell thickness by nearly a factor of 10. This implies that in some systems we have been over-predicting the ejected masses and under-predicting the electron temperature of the ejecta.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Radio Frequency Models of Novae in Eruption. I. The Free-Free Process in Bipolar Morphologies

Ribeiro

Chomiuk

Munari

et al. 2014

ApJ

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“…(1) Crampton et al (1987); (2 Kahabka (1996); (9) Tomov et al (1998) Ribeiro et al (2013b); (17) Munari et al (2013); (18) Bos et al (2001); (19) Barsukova & Goranskii (2003); (20) Hachisu et al (2004); (21) Iijima & Esenoglu (2003); (22) Ribeiro et al (2011);(23) Helton et al (2008); (24) Dobrotka et al (2008); (25) Sala et al (2008); (26) Lyke & Campbell (2009); (27) Goranskij et al (2007); (28) Shore et al (2003); (29) Della Valle et al (2002); (30) Dobrzycka & Kenyon (1994); (31) Ribeiro et al (2009);(32) Bode (1987); (33) Barry et al (2008); (34) Schaefer (1990); (35) Thoroughgood et al (2001); (36) Schaefer (2010); (37) Chesneau et al (2011);(38) Uthas et al (2010); (39) Sokoloski et al (2013); …”

Section: Referencesmentioning

confidence: 99%

Obscuration effects in super-soft-source X-ray spectra

Ness

Osborne

Henze

et al. 2013

A&A

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Context. Super-soft-source (SSS) X-ray spectra are blackbody-like spectra with effective temperatures ∼3−7 × 10 5 K and luminosities of 10 35−38 erg s −1 . Grating spectra of SSS and novae in outburst that show SSS type spectra display atmospheric absorption lines. Radiation transport atmosphere models can be used to derive physical parameters. Blue-shifted absorption lines suggest that hydrostatic equilibrium is an insufficient assumption, and more sophisticated models are required. Aims. In this paper, we bypass the complications of spectral models and concentrate on the data in a comparative, qualitative study. We inspect all available X-ray grating SSS spectra to determine systematic, model-independent trends. Methods. We collected all grating spectra of conventional SSS like Cal 83 and Cal 87 plus observations of novae during their SSS phase. We used comparative plots of spectra of different systems to find common and different features. The results were interpreted in the context of system parameters obtained from the literature.

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“…We plot this distancereddening relation of Equation (15) in Figure 27 by a blue solid line. The distance to V723 Cas was estimated by Lyke & Campbell (2009) Figure 27. Therefore, we adopt these values in this paper.…”

Section: Hr Del 1967mentioning

confidence: 99%

“…(16). The distance estimate is taken from Lyke & Campbell (2009) and the color excess is taken from .…”

Section: Brightness Confirmation Of Model Light Curvesmentioning

confidence: 99%

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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The Distance and Morphology of V723 Cassiopeiae (Nova Cassiopeia 1995)

Cited by 27 publications

References 24 publications

Radio Frequency Models of Novae in Eruption. I. The Free-Free Process in Bipolar Morphologies

Radio Frequency Models of Novae in Eruption. I. The Free-Free Process in Bipolar Morphologies

Obscuration effects in super-soft-source X-ray spectra

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

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