The optical and ultraviolet spectra of the high excitation planetary nebula, CD -23 deg 12238 = ME 2-1

1981 ◽  
Vol 250 ◽  
pp. 596 ◽  
Author(s):  
L. H. Aller ◽  
C. D. Keyes ◽  
S. J. Czyzak
Keyword(s):  
Planetary Nebula ◽  
High Excitation ◽  
Ultraviolet Spectra

scholarly journals IUE and Optical Observations of HE 2-104

1988 ◽  
Vol 103 ◽  
pp. 305-306
Author(s):  
Julie H. Lutz
Keyword(s):  
Planetary Nebula ◽  
Optical Observations ◽  
Symbiotic Star ◽  
High Excitation ◽  
Ultraviolet Spectra ◽  
Evolutionary State ◽  
Very High

AbstractHe 2-104 has been classified as both a planetary nebula and as a symbiotic star. Optical and ultraviolet spectra and CCD images have been obtained in order to learn more about the evolutionary state of this object. The spectra of the object indicate that it could be either a symbiotic star or a very high excitation planetary nebula. The CCD images show a nebulosity with a radius of about 4 seconds of arc and faint bipolar outer structures extending out approximately 25 seconds of arc from the center of the nebula.

The High‐Excitation Planetary Nebula NGC 7662

1997 ◽  
Vol 491 (1) ◽  
pp. 242-253 ◽  
Author(s):  
Siek Hyung ◽  
Lawrence H. Aller
Keyword(s):  
Planetary Nebula ◽  
High Excitation ◽  
Ngc 7662

scholarly journals Models of Planetary Nebulae: Generalisation of the Multiple Winds Model

1989 ◽  
Vol 131 ◽  
pp. 411-424 ◽  
Author(s):  
F. D. Kahn
Keyword(s):  
Planetary Nebula ◽  
High Speed ◽  
Planetary Nebulae ◽  
Central Star ◽  
Theoretical Description ◽  
Basic Theory ◽  
Spectral Lines ◽  
High Excitation ◽  
General Shape ◽  
Fast Wind

According to the multiple winds model a planetary nebula forms as the result of the interaction of a fast wind from the central star with the superwind that had previously been emitted by the progenitor star. The basic theory which deals with the spherically symmetrical case is briefly summarised. Various improvements are then considered in turn. A better history is clearly needed of the way that the central star becomes hotter, it is unrealistic to make the assumption that the superwind is spherically symmetrical, and finally there are likely to be important instabilities at some of the interfaces in the PN, notably that between the shocked superwind and the HII layer. These changes in the theoretical description produce a better understanding of the conditions in the outer parts of a PN and of the nature of its general shape, and they should lead to an explanation for the occurrence of high speed motions, and of highly ionized species and high excitation spectral lines.

Spectrum of the high-excitation planetary Nebula NGC 6741 (33-2 deg 1)

1985 ◽  
Vol 296 ◽  
pp. 492 ◽  
Author(s):  
L. H. Aller ◽  
C. D. Keyes ◽  
S. J. Czyzak
Keyword(s):  
Planetary Nebula ◽  
High Excitation

scholarly journals N 66: A High Excitation N Rich Planetary Nebula in the LMC

1989 ◽  
Vol 131 ◽  
pp. 353-353
Author(s):  
M. Peña ◽  
M. T. Ruiz
Keyword(s):  
Spectral Range ◽  
Planetary Nebula ◽  
High Excitation

Spectrophotometry data of the planetary nebula N 66 (WS 35) has been obtained with the CTIO 4-m telescope equipped with an R-C spectrograph and a 2D-Frutti detector. The spectral range between 3700 A and 6800 A was covered at 4 A resolution.

scholarly journals Spectroscopy of Extragalactic Planetary Nebulae in the Ultraviolet

1983 ◽  
Vol 103 ◽  
pp. 545-545
Author(s):  
T.R. Gull ◽  
S.P. Maran ◽  
T.P. Stecher ◽  
L. H. Aller
Keyword(s):  
Planetary Nebula ◽  
Planetary Nebulae ◽  
Magellanic Clouds ◽  
Emission Lines ◽  
High Excitation ◽  
Long Wavelength ◽  
International Ultraviolet Explorer ◽  
Interstellar Media ◽  
Progenitor Stars ◽  
Stellar Envelopes

Three high-excitation planetary nebulae in the Magellanic Clouds were successfully observed with the International Ultraviolet Explorer. Emission lines as well as nebular and stellar continua were detected. Fluxes in the lines 1550 C IV, 1640 He II, 1663 O III, and 1909 C III were measured in spectra of LMC P40, SMC N2, and SMC N5 obtained with the IUE short wavelength spectrograph; 2422 Ne IV was measured in P40 with the long wavelength spectrograph. The data were analyzed together with groundbased observations by Aller in order to derive ionization models and the nebular abundances of He, C, N, O, S, Ar. The C abundances are as large as those typically found in galactic planetaries, although the interstellar media of the Clouds are notably deficient in C. Thus, the C was synthesized in the progenitor stars and presumably was lifted to the stellar envelopes by convection prior to the ejection of the nebulae. Other planetary nebulae in the Clouds, as well as the planetary nebula in the Fornax galaxy, may be observable with IUE.

scholarly journals The Hubble-Type Outflows from the High-Excitation, Polypolar Planetary Nebula NGC 6302

2005 ◽  
Vol 130 (5) ◽  
pp. 2303-2311 ◽  
Author(s):  
J. Meaburn ◽  
J. A. López ◽  
W. Steffen ◽  
M. F. Graham ◽  
A. J. Holloway
Keyword(s):  
Planetary Nebula ◽  
High Excitation
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