NGC 6543: The Rings Around the Cat’s Eye

Balick, Bruce; Wilson, J. C.; Hajian, Arsen R.

doi:10.1086/318052

Cited by 49 publications

(58 citation statements)

References 24 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Both methods have their limitations, and the result remains inconclusive. Balick et al (2001) derived density variations from Hα emission variations, and found them to be consistent with individual shells with negligible amounts of material between them.…”

Section: Reproduce the Ring Features Bymentioning

confidence: 83%

The post-AGB evolution of AGB mass loss variations

Meijerink¹,

Mellema²,

Simis

2003

A&A

View full text Add to dashboard Cite

Abstract. We present new numerical hydrodynamical modelling of the evolution of Asymptotic Giant Branch (AGB) mass loss fluctuations during the post-AGB/Planetary Nebula phase. These models show that after ionization, the observable effects of the mass loss fluctuations disappear in a few thousand years, consistent with the fact that only few PNe have been found to be surrounded by "rings". We derive the observational characteristics of these rings, and compare them to reported observations of the rings around NGC 6543, finding a good match of emission properties and line shapes. We predict small variations in the observable electron temperatures.

show abstract

Section: Reproduce the Ring Features Bymentioning

confidence: 83%

The post-AGB evolution of AGB mass loss variations

Meijerink¹,

Mellema²,

Simis

2003

A&A

View full text Add to dashboard Cite

show abstract

“…Some circularly symmetric brightness enhancements are evident, reminiscent of similar structure seen in the surface brightness distribution of several planetary nebulae (cf. Balick et al 2001, their Fig.1), usually interpreted as variations in the progenitor AGB mass loss rate. Their angular separation indicate a ∼1200 year recurrence time.…”

Section: The Light-echo and Distance To V838 Monmentioning

confidence: 99%

The mysterious eruption of V838 Mon

Munari

Henden

Kiyota³

et al. 2002

A&A

179

316

View full text Add to dashboard Cite

Abstract. V838 Mon is marking one of the most mysterious stellar outbursts on record. The spectral energy distribution of the progenitor resembles an under-luminous F main sequence star (at V =15.6 mag), that erupted into a cool supergiant following a complex and multi-maxima lightcurve (peaking at V =6.7 mag). The outburst spectrum show BaII, LiI and lines of several s−elements, with wide P-Cyg profiles and a moderate and retracing emission in the Balmer lines. A light-echo discovered expanding around the object helped to constrain the distance (d=790±30 pc), providing MV = +4.45 in quiescence and MV = −4.35 at optical maximum (somewhat dependent on the still uncertain EB−V =0.5 reddening). The general outburst trend is toward lower temperatures and larger luminosities, and continuing so at the time of writing. The object properties conflict with a classification within already existing categories: the progenitor was not on a post-AGB track and thus the similarities with the bornagain AGB stars FG Sge, V605 Aql and Sakurai's object are limited to the cool giant spectrum at maximum; the cool spectrum, the moderate wind velocity (500 km sec −1 and progressively reducing) and the monotonic decreasing of the low ionization condition argues against a classical nova scenario. The closest similarity is with a star that erupted into an M-type supergiant discovered in M31 by Rich et al. (1989), that became however much brighter by peaking at MV = −9.95, and with V4332 Sgr that too erupted into an M-type giant (Martini et al. 1999) and that attained a lower luminosity, closer to that of V838 Mon. M31-RedVar, V4332 Sgr and V838 Mon could be all manifestations of a new class of astronomical objects.

show abstract

“…Unlike what is advocated for NGC 6720, the rings and the core in NGC 6543 seem to have same chemical composition (Balick et al 2001). It must be noted however, that the abundances may not be reliable, since a photoionization model for the core of NGC 6543 predicts a far too high [O iii] λ4363/5007 (Hyung et al 2000).…”

Section: Abundance Inhomogeneitiesmentioning

confidence: 80%