5.1.2.1 Long period Cepheids - C

Duerbeck, H. W.; Seitter, W. C.

doi:10.1007/10201975_53

Cited by 8 publications

(18 citation statements)

References 28 publications

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“…The evolution of colors is another challenging subject that attracts many researchers, who have attempted to identify common behavior among various types of novae. For example, Duerbeck & Seitter (1979) noted that the color evolutions of six novae are remarkably similar in the intrinsic (B − V ) 0 versus (U − B) 0 color-color diagram, regardless of their different nova speed classes. These six novae, however, traced similar but different paths in the colorcolor diagram (see Figures 2-7 of Duerbeck & Seitter 1979).…”

Section: Introductionmentioning

confidence: 99%

“…For example, Duerbeck & Seitter (1979) noted that the color evolutions of six novae are remarkably similar in the intrinsic (B − V ) 0 versus (U − B) 0 color-color diagram, regardless of their different nova speed classes. These six novae, however, traced similar but different paths in the colorcolor diagram (see Figures 2-7 of Duerbeck & Seitter 1979). van den Bergh & Younger (1987) derived the general trends of color evolution in nova light curves, i.e., (B − V ) 0 = 0.23 ± FIG.…”

Section: Introductionmentioning

confidence: 99%

“…These different trends in nova color evolution may represent different sides of the true color evolution, which we do not yet fully understand observationally or theoretically. The aim of this paper is to find a general path of nova color evolution, as Duerbeck & Seitter (1979) tried to do 30 yr ago. First, in Section 2 we analyze the moderately-fast nova FH Ser in the (B − V ) 0 -(U − B) 0 diagram and find a new sequence along which novae evolve when the photospheric emission dominates the optical spectrum.…”

Section: Introductionmentioning

confidence: 99%

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THEUBVCOLOR EVOLUTION OF CLASSICAL NOVAE. I. NOVA-GIANT SEQUENCE IN THE COLOR-COLOR DIAGRAM

Hachisu

Kato

2014

ApJ

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We identified a general course of classical nova outbursts in the B − V versus U − B color-color diagram. It is reported that novae show spectra similar to those of A-F supergiants near optical light maximum. However, they do not follow the supergiant sequence in the color-color diagram, neither the blackbody nor the mainsequence sequence. Instead, we found that novae evolve along a new sequence in the pre-maximum and nearmaximum phases, which we call "the nova-giant sequence." This sequence is parallel to but ∆(U − B) ≈ −0.2 mag bluer than the supergiant sequence. This is because the mass of a nova envelope is much (∼ 10 −4 times) less than that of a normal supergiant. After optical maximum, its color quickly evolves back blueward along the same nova-giant sequence and reaches the point of free-free emission (B − V = −0.03, U − B = −0.97), which coincides with the intersection of the blackbody sequence and the nova-giant sequence, and remains there for a while. Then the color evolves leftward (blueward in B − V but almost constant in U − B), owing mainly to the development of strong emission lines. This is the general course of nova outbursts in the colorcolor diagram, which was deduced from eight well-observed novae in various speed classes. For a nova with unknown extinction, we can determine a reliable value of the color excess by matching the observed track of the target nova with this general course. This is a new and convenient method for obtaining the color excesses of classical novae. Using this method, we redetermined the color excesses of 20 well-observed novae. The obtained color excesses are in reasonable agreement with the previous results, which in turn support the idea of our general track of nova outbursts. Additionally, we estimated the absolute V magnitudes of about 30 novae using a method for time-stretching nova light curves to analyze the distance-reddening relations of the novae.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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THEUBVCOLOR EVOLUTION OF CLASSICAL NOVAE. I. NOVA-GIANT SEQUENCE IN THE COLOR-COLOR DIAGRAM

Hachisu

Kato

2014

ApJ

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“…Slovak & Vogt (1979) estimated the distance to be 3.3 kpc. Duerbeck et al (1980) obtained a much smaller distance of d = 2.3 kpc based on the same stars. It is very difficult to estimate the distance because of the small number of stars and the very patchy A V (r) relation in the direction of the nova (see Hachisu & Kato 2006).…”

Section: Distance From Uv Light-curve Fittingmentioning

confidence: 84%

“…In V1500 Cyg, which is one of the brightest novae, the temporal evolution of the spectrum and the fluxes are well understood as blackbody emission during the first three days and as free-free emission after that (Gallagher & Ney 1976;Ennis et al 1977;Duerbeck & Seitter 1979). In the modeling of the super-Eddington phase we divide the optical light curve into three phases .…”

Section: Optical Light Curvementioning

confidence: 99%

Modeling of the Super‐Eddington Phase for Classical Novae: FiveIUENovae

Kato

Hachisu

2007

ApJ

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We present a light curve model for the super-Eddington luminosity phase of five classical novae observed with IUE. Optical and UV light curves are calculated based on the optically thick wind theory with a reduced effective opacity for a porous atmosphere. Fitting a model light curve with the UV 1455 Å light curve, we determine the white dwarf mass and distance to be (1.3 M ⊙ , 4.4 kpc) for V693 CrA, (1.05 M ⊙ , 1.8 kpc) for V1974 Cyg, (0.95 M ⊙ , 4.1 kpc) for V1668 Cyg, (1.0 M ⊙ , 2.1 kpc) for V351 Pup, and (1.0 M ⊙ , 4.3 kpc) for

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Complex Velocity Fields in the Shell of T Pyxidis

Margon

Deutsch

1998

The Astrophysical Journal

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We present spatially-resolved, moderate-resolution spectrophotometry of the recurrent nova T Pyx and a portion of the surrounding shell. The spectrum extracted from a strip of width 10'' centered on the star shows well-known, strong emission lines typical of old novae, plus a prominent, unfamiliar emission line at 6590 Angstroms. This line, and a weaker companion at 6540 Angstroms which we also detect, have been previously reported by Shahbaz et al., and attributed to Doppler-shifted H alpha emission from a collimated jet emerging from T Pyx. We demonstrate that these lines are instead due to [NII] 6548, 6584 from a complex velocity field in the surrounding nebula. The comments of past workers concerning the great strength of HeII 4686 in T Pyx itself are also reiterated.Comment: 8 pages including 2 figures; Accepted for publication in The Astrophysical Journal Letter

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5.1.2.1 Long period Cepheids - C

Cited by 8 publications

References 28 publications

THEUBVCOLOR EVOLUTION OF CLASSICAL NOVAE. I. NOVA-GIANT SEQUENCE IN THE COLOR-COLOR DIAGRAM

THEUBVCOLOR EVOLUTION OF CLASSICAL NOVAE. I. NOVA-GIANT SEQUENCE IN THE COLOR-COLOR DIAGRAM

Modeling of the Super‐Eddington Phase for Classical Novae: FiveIUENovae

Complex Velocity Fields in the Shell of T Pyxidis

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