PW Vulpeculae - A nova with nearly solar abundances

Saizar, P; Starrfield, S.; Ferland, Gary J.; Wagner, R. M.; Truran, J. W.; Kenyon, Scott J.; Sparks, W. M.; Williams, Robert E.; Stryker, L. L.

doi:10.1086/169630

Cited by 29 publications

(23 citation statements)

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“…The Therefore, we again discuss previous reddening estimates pinpointing PW Vul. The reddening of PW Vul was estimated as E(B − V ) = A V /3.1 = (1.78 ± 0.05)/3.1 = 0.57 ± 0.02 from the Paβ and Paγ line strengths compared with Hβ and Hγ line strengths by Williams et al (1996), E(B − V ) = 0.58 ± 0.06 from the He II λ1640/λ4686 ratio, and E(B − V ) = 0.55 ± 0.1 from the interstellar absorption feature at 2200 Å both by Andreä et al (1991), E(B − V ) = 0.60 ± 0.06 according to Saizar et al (1991) from the He II λ1640/λ4686 ratio. The simple arithmetic mean of these four values is E(B − V ) = 0.57 ± 0.1.…”

Section: Pw Vul 1984#1mentioning

confidence: 91%

The Ubv Color Evolution of Classical Novae. Ii. Color–magnitude Diagram

Hachisu

Kato

2016

ApJS

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We have examined the outburst tracks of 40 novae in the color-magnitude diagram (intrinsic B − V color versus absolute V magnitude). After reaching the optical maximum, each nova generally evolves toward blue from the upper-right to the lower-left and then turns back toward the right. The 40 tracks are categorized into one of six templates: very fast nova V1500 Cyg; fast novae V1668 Cyg, V1974 Cyg, and LV Vul; moderately fast nova FH Ser; and very slow nova PU Vul. These templates are located from the left (blue) to the right (red) in this order, depending on the envelope mass and nova speed class. A bluer nova has a less massive envelope and faster nova speed class. In novae with multiple peaks, the track of the first decay is more red than that of the second (or third) decay, because a large part of the envelope mass had already been ejected during the first peak. Thus, our newly obtained tracks in the color-magnitude diagram provide useful information to understand the physics of classical novae. We also found that the absolute magnitude at the beginning of the nebular phase is almost similar among various novae. We are able to determine the absolute magnitude (or distance modulus) by fitting the track of a target nova to the same classification of a nova with a known distance. This method for determining nova distance has been applied to some recurrent novae and their distances have been recalculated.

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Section: Pw Vul 1984#1mentioning

confidence: 91%

The Ubv Color Evolution of Classical Novae. Ii. Color–magnitude Diagram

Hachisu

Kato

2016

ApJS

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“…(8) Williams (1994). (9) mean value from Stickland et al (1981) and Gehrz et al (1980); (10) Mason et al (1998); (11) Schwarz et al (1997a), see text; (12) Gehrz et al (1988); (13) Saizar et al (1991).…”

Section: Discussionmentioning

confidence: 99%

Classical novae in outburst: evolution of the ultraviolet emission lines in CO novae

Cassatella

Altamore

González‐Riestra

2005

A&A

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Abstract.A comparative study is made of the temporal changes of the ionization level in seven CO novae well monitored with the IUE satellite at low resolution. The investigation is based on the evolution of the fluxes in eight strong ultraviolet emission lines covering a wide range of ionization potentials, from Mg  (7.6 eV) to N  (77.5 eV). We find that the rate of increase of the ionization conditions in the emitting regions is uniform in the sample of novae considered, provided the time scale is normalized to the optical decay time t 3 . The implications of this result for the nova ejected masses and for the nuclear turnoff time are discussed.

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“…Finally, if the accretion rate is low, then the outburst will occur above the CEI and, undershooting will not be able to mix down through the helium layer and dredge-up core material. This could explain why some slow novae, such as PW Vul (Saizar et al 1991;Andreä et al 1994;Schwarz et al 1997b) eject material strongly enriched only in helium.…”

Section: W H E R E I S T H E ' M I S S I N G ' M a S S ?mentioning

confidence: 99%

Evolutionary sequences for Nova V1974 Cygni using new nuclear reaction rates and opacities

Starrfield

Truran

Wiescher

et al. 1998

Monthly Notices of the Royal Astronomical Society

190

240

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The outburst of Nova V1974 Cyg 1992 is arguably the best observed of this century, with realistic estimates now available for the amount of mass ejected, the composition of the ejecta and the total energy budget. These data strongly support the conclusion that this was indeed a ‘neon’ nova that occurred on an oxygen, neon, magnesium white dwarf. In addition, X‐ray studies of its outburst imply that the mass of the white dwarf is about 1.25 M⊙. We, therefore, report on the results of new calculations of thermonuclear runaways on 1.25‐M⊙ oxygen, neon, magnesium white dwarfs, using our one‐dimensional, fully implicit, hydrodynamic stellar evolution code that includes a large nuclear reaction network. We have updated the nuclear reaction network, with the inclusion of new and improved experimental and theoretical determinations of the nuclear reaction rates. We have also incorporated the OPAL carbon rich tables and have investigated the effects of changes in convective efficiency on the evolution. Our results show that the changes in the reaction rates and opacities that we have introduced produce important changes with respect to our previous studies. For example, relevant to nucleosynthesis considerations, a smaller amount of 26Al is produced, while the abundances of 31P and 32S increase by factors of more than two. This change is attributed to the increased proton‐capture reaction rates for some of the intermediate mass nuclei near 26Al and beyond, such that nuclear fusion to higher mass nuclei is enhanced. The characteristics of our models are then compared to observations of the outburst of V1974 Cyg 1992 and we find that the predicted amount of mass ejected is at least a factor of 10 less than observed. The low values for the amount of ejected mass are a consequence of the fact that the OPAL opacities are larger than those we previously used, which results in less mass being accreted on to the white dwarf. This is a general problem with respect to the comparison of observations and theory for ONeMg novae and we suggest a possible resolution of this discrepancy.

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PW Vulpeculae - A nova with nearly solar abundances

Cited by 29 publications

References 0 publications

The Ubv Color Evolution of Classical Novae. Ii. Color–magnitude Diagram

The Ubv Color Evolution of Classical Novae. Ii. Color–magnitude Diagram

Classical novae in outburst: evolution of the ultraviolet emission lines in CO novae

Evolutionary sequences for Nova V1974 Cygni using new nuclear reaction rates and opacities

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