Direct photography of the nebular remnant of nova Delphini 1967

Kohoutek, L.

doi:10.1093/mnras/196.1.87p

Cited by 10 publications

(14 citation statements)

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“…As to HR Del the nebulosity in [OIII] 5007Å was already reported (see e.g. Kohoutek 1981). For the year 1995 the nebulosity was expected to be larger than that we observed, so that we think that our small values are either due to the low brightness of the nebula relative to the very bright star in the centre, or that we see only the brightest part of the nebula.…”

Section: Possible Nebulaesupporting

confidence: 60%

Search for envelopes of some stellar planetary nebulae, symbiotic stars and further emission-line objects

Kohoutek

1997

Astron. Astrophys. Suppl. Ser.

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Abstract. At 17 emission-line objects, mainly PN, the seeing disc has been compared with that of some surrounding stars (CCD frames taken through B, V , R, [OIII] 5007Å and Hα filters). Nebulosities were found at: CPD − 53• 8315 (0. 5 in x-direction, 0. 4 in y-direction), H 2 − 2 (0. 3, 1. 4) and CPD − 56• 8032 (1. 3, 1. 3). Further small nebulosities are possible at MWC 560, MWC 574, LS IV − 12• 111 and HR Del, but they should be considered as rather uncertain. Besides, the known outer nebula at CPD − 53• 8315 (2 condensations, 11. 6 separation, PA = 146• ) was observed, and the author discovered a circular halo of 50 around Hb 6 -both outer nebulosities visible in the light of Hα.

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Section: Possible Nebulaesupporting

confidence: 60%

Search for envelopes of some stellar planetary nebulae, symbiotic stars and further emission-line objects

Kohoutek

1997

Astron. Astrophys. Suppl. Ser.

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“…More recently, Harman & O'Brien (2003) obtained a new value of the distance, d = 0.97 ± 0.07 kpc, also from the expansion parallax method using HST imaging. Other, older, estimates are all between the above two estimates, i.e., d = 0.940 ± 0.155 kpc from various expansion par- allax methods (Malakpur 1975;Kohoutek 1981;Duerbeck 1981;Solf 1983;Cohen & Rosenthal 1983;Slavin et al 1994Slavin et al , 1995 or d = 0.835 ± 0.092 kpc from other techniques (Drechsel et al 1977). If we adopted the new distance estimate of d = 0.97 kpc (Harman & O'Brien 2003) and the extinction of E(B −V ) = 0.15 (Verbunt 1987), the distance modulus is (m − M) V = 5 log 970/10 + 3.1 × 0.15 = 10.4, which is perfectly consistent with the value in Equation (11).…”

Section: Hr Del 1967mentioning

confidence: 95%

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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“…Spatially unresolved optical spectra display six-peaked profiles which were interpreted as evidence for the ejection of an oblate shell with two equatorial bands and polar blobs (Hutchings 1972). The first resolved photographs of the shell (Kohoutek 1981) taken in the light of [O III] revealed an oval brightness distribution of size 3.7 × 2.5 arcsec 2 . Solf (1983) obtained high-resolution spatially resolved spectra and proposed that the shell was in fact prolate.…”

Section: Introductionmentioning

confidence: 99%

Hubble Space Telescope imaging and ground-based spectroscopy of old nova shells - II. The bipolar shell of the slow nova HR Del

Harman¹,

O’Brien²

2003

Monthly Notices RAS

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We present Hubble Space Telescope (HST) WFPC2 imaging of HR Del in filters centred on the lines of Hα, [N ii] and [O iii], with corresponding William Herschel Telescope (WHT) ISIS slit spectroscopy for the lines of Hα, Hβ, [N ii] and [O iii]. The data show that the ejected shell of HR Del is composed of many small bright knots. These are distributed in a bipolar structure with an equatorial ring, and polar rings or caps. The [O iii] emission is significantly more bipolar than that seen in Hα/[N ii]. Diffuse material which extends radially outward from these knots may be further evidence for a fast wind from the central binary system. There are also [N ii] and [O iii] knots at both higher and lower velocity than that of the main shell which follow the general bipolar symmetry and may be associated with secondary mass ejections at outburst or interactions with the fast wind. Three‐dimensional models of the shell that reproduce the observed emission‐line images and longslit spectra in both the [O iii] and Hα morphologies are presented. We use these models to estimate an inclination for the shell of 35°± 3°, a polar expansion velocity of 560 ± 50 km s−1, an axial ratio of 1.75 ± 0.15 and a distance of 970 ± 70 pc. We discuss how these parameters can be used to improve the shell shape and maximum magnitude versus rate of decline (SSRD and MMRD, respectively) relationships for novae.

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Direct photography of the nebular remnant of nova Delphini 1967

Cited by 10 publications

References 0 publications

Search for envelopes of some stellar planetary nebulae, symbiotic stars and further emission-line objects

Search for envelopes of some stellar planetary nebulae, symbiotic stars and further emission-line objects

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

Hubble Space Telescope imaging and ground-based spectroscopy of old nova shells - II. The bipolar shell of the slow nova HR Del

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