Symbiotic star AS 201: A planetary nebula

1987 ◽  
Vol 131 (1-2) ◽  
pp. 781-784 ◽  
Author(s):  
L. Kohoutek
Keyword(s):  
Planetary Nebula ◽  
Symbiotic Star

scholarly journals The IUE Ultraviolet Spectrum of PC 11

1993 ◽  
Vol 155 ◽  
pp. 398-398 ◽  
Author(s):  
M. Parthasarathy ◽  
S.R. Pottasch ◽  
J. Clavel
Keyword(s):  
Short Wavelength ◽  
Planetary Nebula ◽  
Significant Variation ◽  
Central Star ◽  
Ultraviolet Spectrum ◽  
Emission Lines ◽  
Symbiotic Star ◽  
Iras Source ◽  
Long Wavelength ◽  
Cold Dust

PC 11 (HD 149427, PK 331-5 1) is classified as a young planetary nebula with strong OIII 4363Å and a Zanstra temperature of TZ = 27000K. It is also classified as (D′ — type) yellow symbiotic star with A — F type companion. It is an IRAS source with detached cold dust with far intrared (IRAS) colours similar to planetary nebulae. The IUE short wavelength (SWP) spectra show emission lines due to OIII] (1661/1666Å). NIII] (1746/1754Å) CIII] (1907/1909Å). The OIII] and NIII] emission lines show significant variation. Variation in the strength of CIII] is not very significant. The strength of OIII] has decreased and NIII] has increased. The long wavelength (LWP) spectrum shows stellar continuum (A-F) and absorption lines due Mg II 2800Å feature. It also show emission lines at 2772Å (?) 3133Å −3140Å (very strong) (OIII, [FeV], 3209Å (He II?) ([FEII]). The variation in the strength of emission line due OIII] and NIII] and the presence of stellar continuum (A-F) suggests that the central star of PC 11 is a binary.

scholarly journals Discovery of a planetary nebula surrounding the symbiotic star DT Serpentis

2013 ◽  
Vol 558 ◽  
pp. A2 ◽  
Author(s):  
U. Munari ◽  
R. L. M. Corradi ◽  
A. Siviero ◽  
L. Baldinelli ◽  
A. Maitan
Keyword(s):  
Planetary Nebula ◽  
Symbiotic Star

scholarly journals Symbiotic Star as 201: a Planetary Nebula

1987 ◽  
Vol 93 ◽  
pp. 781-784
Author(s):  
L. Kohoutek
Keyword(s):  
Absorption Spectrum ◽  
Mass Loss ◽  
Planetary Nebula ◽  
Optical Spectrum ◽  
Interstellar Extinction ◽  
Emission Lines ◽  
Symbiotic Star ◽  
Cool Stars ◽  
Central Stars

AbstractOptical spectrum of AS 201 is presented: this object shows emission lines of moderate excitation (exc.class 5) and absorption spectrum of a G2III star. For the interstellar extinction and distance the values c=0.45 and d=1.5 kpc were estimated. The hot components of AS 2Ol, Cn 1–1 and M 1–2 are located on the Harman-Seaton sequence in the region of evolved central stars of PN. It is suggested that the hot components of some SS are evolved nuclei of PN; high el.density of their nebulae may be explained due to mass loss from the respective cool stars of the binaries.

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 Symbiotic Star H1-36

1983 ◽  
Vol 5 (2) ◽  
pp. 211-213 ◽  
Author(s):  
David A. Allen
Keyword(s):  
Emission Line ◽  
Planetary Nebula ◽  
Line Spectrum ◽  
Symbiotic Star ◽  
Symbiotic Stars ◽  
High Excitation ◽  
Infrared Excess ◽  
Emission Line Spectrum ◽  
Definition Of ◽  
Meaningful Definition

Since its discovery by Haro (1952) the star H1-36 has been catalogued as a planetary nebula despite its extremely high-excitation emission-line spectrum (e.g. [Fe VII], [Ne V]) and its imposing, variable infrared excess. Because its optical spectrum resembled those of many symbiotic stars, I have persistently classified H1-36 as such. A meaningful definition of a symbiotic star would necessarily include both the high-excitation emission-line spectrum and the presence of a cool (usually M-type or Mira) giant.

scholarly journals DT Serpentis: neither a symbiotic star nor a planetary nebula associate

2014 ◽  
Vol 445 (2) ◽  
pp. 1605-1613 ◽  
Author(s):  
David J. Frew ◽  
Joao Bento ◽  
Ivan S. Bojičić ◽  
Quentin A. Parker
Keyword(s):  
Planetary Nebula ◽  
Symbiotic Star

The Proto–Planetary Nebula M1‐92 and the Symbiotic Star MWC 560: Two Evolutionary Phases of the Same Type of Object?

2005 ◽  
Vol 623 (1) ◽  
pp. 252-268 ◽  
Author(s):  
A. Arrieta ◽  
S. Torres‐Peimbert ◽  
L. Georgiev
Keyword(s):  
Planetary Nebula ◽  
Symbiotic Star
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