The structure of the remnant of HR Del

Slavin, Arthur J.; O'Brien, T. J.; Dunlop, James

doi:10.1093/mnras/266.1.l55

Cited by 13 publications

(12 citation statements)

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“…The [O III] image shows a bi-polar structure, with an average surface brightness of 1.59 × 10 −13 ergs cm −2 s −1 arcsec −2 . The enhancements seen by Slavin, O'Brien and Dunlop (1994) in the Hα/[N II] image are not present in our image, and the emission in the 2 lines appear to be growing at slightly different rates (i.e. the major axis in [O III] is 9.…”

Section: Hr Del (1967)mentioning

confidence: 53%

Optical Imaging of Nova Shells and the Maximum Magnitude–Rate of Decline Relationship

Downes

Duerbeck

2000

The Astronomical Journal

223

374

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An optical imaging study of recent 30 novae has been undertaken using both ground-based and space-based observations. Resolved shells have been detected around 9 objects in the ground-based data, while another four objects have shells detected by Hubble Space Telescope observations; for RW UMi, we fail to detect a shell which was observed five years earlier. Images in Hα, and when appropriate [O III] λ5007, are shown, and finding charts for novae without shells are given if no published chart is available. Expansion parallaxes for all systems with shells are derived, and absolute magnitudes for a total of 28 objects are presented, along with a discussion of the maximum magnitude-rate of decline relation. We find that separate linear fits for fast and slow novae may be a better representation of the data than a single, global fit. At minimum, most novae have similar magnitudes as those of dwarf novae at maximum and novalike stars.

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Section: Hr Del (1967)mentioning

confidence: 53%

Optical Imaging of Nova Shells and the Maximum Magnitude–Rate of Decline Relationship

Downes

Duerbeck

2000

The Astronomical Journal

223

374

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“…Since the outburst day is not known, we adopted UT 1967 June 8.5 as the outburst day, i.e., t OB =JD 2439653.0, from the figure of Robinson & Ashbrook (1968). Verbunt (1987) 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: 99%

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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“…Recent observations (Slavin et al 1994; Slavin et al 1995) have revealed a structure with two polar caps and an equatorial ring but there are some discrepancies in the exact shell size (see also Downes & Duerbeck 2000). Very recently, O'Brien et al (2002) have reported v = −290 km s −1 and v = −580 km s −1 for the expansion speed in the equatorial ring and in the polar caps respectively and derived a distance d∼1100 ± 100 pc.…”

Section: Introductionmentioning

confidence: 99%

The active quiescence of HR Del (Nova Del 1967)

Selvelli

Friedjung²

2003

A&A

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Abstract. This new UV study of the ex-nova HR Del is based on all of the data obtained with the International Ultraviolet Explorer (IUE) satellite, and includes the important series of spectra taken in 1988 and 1992 that have not been analyzed so far. This has allowed us to make a detailed study of both the long-timescale and the short-timescale UV variations, after the return of the nova, around [1981][1982], to the pre-outburst optical magnitude. After the correction for the reddening (E B−V = 0.16), adopting a distance d = 850 pc we have derived a mean UV luminosity close to L UV ∼ 56 L , the highest value among classical novae in "quiescence". Also the "average" optical absolute magnitude (M v = +2.30) is indicative of a bright object. The UV continuum luminosity, the HeII 1640 Å emission line luminosity, and the optical absolute magnitude all give a mass accretion rateṀ very close to 1.4 × 10 −7 M yr −1 , if one assumes that the luminosity of the old nova is due to a non-irradiated accretion disk. The UV continuum has declined by a factor less than 1.2 over the 13 years of the IUE observations, while the UV emission lines have faded by larger factors. The continuum distribution is well fitted with either a black body of 33 900 K, or a power-law F λ ∼ λ −2.20 . A comparison with the grid of models of Wade & Hubeny (1998) indicates a low M 1 value and a relatively highṀ but the best fittings to the continuum and the line spectrum come from different models. We show that the "quiescent" optical magnitude at m v ∼ 12 comes from the hot component and not from the companion star. Since most IUE observations correspond to the "quiescent" magnitude at m v ∼ 12, the same as in the pre-eruption stage, we infer that the pre-nova, for at least 70 years prior to eruption, was also very bright at near the same L UV , M v ,Ṁ, and T values as derived in the present study for the ex-nova. The wind components in the P Cyg profiles of the CIV 1550 Å and NV 1240 Å resonance lines are strong and variable on short timescales, with v edge up to −5000 km s −1 , a remarkably high value. The phenomenology of the short-time variations of the wind indicates the presence of an inhomogeneous outflow. We discuss the nature of the strong UV continuum and wind features and the implications of the presence of a "bright" state a long time before and after outburst on our present knowledge of the pre-nova and post-nova behavior.

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The structure of the remnant of HR Del

Cited by 13 publications

References 0 publications

Optical Imaging of Nova Shells and the Maximum Magnitude–Rate of Decline Relationship

Optical Imaging of Nova Shells and the Maximum Magnitude–Rate of Decline Relationship

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

The active quiescence of HR Del (Nova Del 1967)

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