Lichtkurve und Farbe der Nova Herculis 1960 = V 446 Her

Bronkalla, W.; Notni, P.

doi:10.1002/asna.19612860406

Cited by 7 publications

(6 citation statements)

References 4 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The orbital period of 4.97 hr was detected by Thorstensen & Taylor (2000). The B − V data of the IAU Circular, Knipe (1960), and Bronkalla & Notni (1961) are systematically 0.1 mag redder than those of Ross (1960), so we shift them by 0.1 mag toward blue. As a result, the B − V color curve becomes smooth as shown in Figure 17(b).…”

Section: Color-magnitude Diagrams For Various Novaementioning

confidence: 71%

“…As a result, the B − V color curve becomes smooth as shown in Figure 17(b). We also shift the U − B data of the IAU Circular and Bronkalla & Notni (1961) by 0.1 mag toward blue, so the U − B color curve also becomes smooth as shown in Figure 17(c).…”

Section: Color-magnitude Diagrams For Various Novaementioning

confidence: 98%

“…These light curve data are the same as those in Figure 42 of Paper I, but we reanalyzed the data as mentioned below. The data are taken from Antal (1961), Bronkalla & Notni (1961), Knipe (1960), Ross (1960), and IAU Circular No.1730. The orbital period of 4.97 hr was detected by Thorstensen & Taylor (2000).…”

Section: V446 Her 1960mentioning

confidence: 99%

See 2 more Smart Citations

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

Hachisu

Kato

2016

ApJS

View full text Add to dashboard Cite

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.

show abstract

Section: Color-magnitude Diagrams For Various Novaementioning

confidence: 71%

Section: Color-magnitude Diagrams For Various Novaementioning

confidence: 98%

See 1 more Smart Citation

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

Hachisu

Kato

2016

ApJS

View full text Add to dashboard Cite

show abstract

“…The reddening toward V446 Her was determined to be E(B − V ) = 0.45 ± 0.1 from the galactic absorption (Bronkalla & Notni 1961), E(B − V ) = A V /3.1 = (1.7 ± 0.5)/3.1 = 0.55 ± 0.15 from the galactic absorption (Duerbeck 1981 0.46 ± 0.04 from the value at the stabilization stage (Miroshnichenko 1988), E(B − V ) = A V /3.1 = 1.12/3.2 = 0.35 from the 2200Å feature (Gilmozzi et al 1994), E(B − V ) = 0.25 from the depth of the interstellar bump at 2175Å (Selvelli 2004). These reddening estimates range from 0.25 to 0.55 and we obtained a simple average of E(B − V ) = 0.41 ± 0.15, which is consistent with our value.…”

Section: General Course Of Ubv Color-color Evolutionmentioning

confidence: 99%

“…Then it rapidly and smoothly declined with t 2 = 5 days (e.g., Cohen 1985) and t 3 = 16 days (e.g., Duerbeck 1981). We plot the color-color evolution of V446 Her in Figure 29(c), where the UBV data are taken mainly from Ross (1960) and Bronkalla & Notni (1961). These observations started after the nova had already decayed to m V = 5.5, so we missed the early evolution of this nova.…”

Section: V446 Her 1960mentioning

confidence: 99%

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

Hachisu

Kato

2014

ApJ

View full text Add to dashboard Cite

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.

show abstract

The Tables

Mermilliod

1994

Catalogue of Mean UBV Data on Stars

View full text Add to dashboard Cite

Lichtkurve und Farbe der Nova Herculis 1960 = V 446 Her

Cited by 7 publications

References 4 publications

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

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

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

The Tables

Contact Info

Product

Resources

About