Emission-line profiles for selected planetary nebulae and symbiotic stars, V1016 Cygni, and HM Sagittae

1983 ◽  
Vol 95 ◽  
pp. 217 ◽  
Author(s):  
D. E. Welty
Keyword(s):  
Emission Line ◽  
Planetary Nebulae ◽  
Symbiotic Stars ◽  
Line Profiles

scholarly journals Emission-Line Profiles in Planetary Nebulae

1968 ◽  
Vol 34 ◽  
pp. 267-269
Author(s):  
Donald E. Osterbrock
Keyword(s):  
Velocity Distribution ◽  
Emission Line ◽  
Observational Data ◽  
Planetary Nebulae ◽  
Line Profiles ◽  
Measured Velocity ◽  
Hydrodynamical Models ◽  
Internal Velocity ◽  
First Time

This research was undertaken with the idea of measuring as accurately as possible the internal-velocity distribution in planetary nebulae, in order to compare the observational measurements with hydrodynamical models of expanding nebulae. Much of the work was done in collaboration with J. S. Miller and D.W. Weedman. All the observational data were obtained photographically with the Coudé spectrograph of the 100-inch telescope at Mt. Wilson, using an image rotator, a 900 line/mm grating, and an F/5-2 camera, giving a dispersion of about 4 Å/mm in the blue and about 6 Å/mm in the red. The measured velocity resolution is approximately 5–6 km/sec. The data for five nebulae have been published (Osterbrock et al., 1966) while data for three more, NGC 2392, NGC 3242, and IC 418 are discussed here for the first time.

Optical emission line profiles of symbiotic stars

1989 ◽  
pp. 85-86 ◽  
Author(s):  
K. Robinson ◽  
M. F. Bode ◽  
J. Meabum ◽  
M. J. Whitehead
Keyword(s):  
Emission Line ◽  
Optical Emission ◽  
Symbiotic Stars ◽  
Line Profiles

Emission-Line Profiles in Planetary Nebulae

1966 ◽  
Vol 145 ◽  
pp. 697 ◽  
Author(s):  
D. E. Osterbrock ◽  
J. S. Miller ◽  
D. W. Weedman
Keyword(s):  
Emission Line ◽  
Planetary Nebulae ◽  
Line Profiles

scholarly journals Broad Hα wings in Young Planetary Nebulae

2003 ◽  
Vol 209 ◽  
pp. 391-392
Author(s):  
Anabel Arrieta ◽  
Silvia Torres-Peimbert
Keyword(s):  
Emission Line ◽  
Planetary Nebulae ◽  
Symbiotic Stars ◽  
First Report

In a sample of 30 young planetary nebulae, proto-PNe and other emission line objects we have found 11 young PNe and 2 symbiotic stars that show very broad wings of the emission Hα line (from 800 km s-1 and up to 5100 km s-1). For 7 objects, their first report was in Arrieta & Torres-Peimbert (2002).

scholarly journals Is there Any Connection Between Planetary Nebulae and Symbiotic Stars ?

1993 ◽  
Vol 155 ◽  
pp. 401-401
Author(s):  
Michael Friedjung
Keyword(s):  
Emission Line ◽  
Planetary Nebulae ◽  
H Ii Regions ◽  
Symbiotic Stars ◽  
Cool Star

Symbiotic stars have sometimes been misidentified as planetary nebulae, because their line spectra are similar to those of planetary nebulae particularly in the ultraviolet L.(Houziaux 1982 in “The Nature of Symbiotic Stars”, M. Friedjung & R. Viotti eds., Reidel. p 229), while the infrared shows the presence of the spectrum of a cool star. The similarity is not complete; when H. E. Schwarz (1988 in “The Symbiotic Phenomenon”, J. Mikolajewska et al eds., Kluwer, p 123) plotted a graph of two ratios derived from emission line fluxes, symbiotic stars did not occupy the regions of the diagram occupied by planetary nebulae and H II regions.

scholarly journals Scattering by Dust in Planetary Nebulae: Polarization as a Diagnostic Tool

2003 ◽  
Vol 209 ◽  
pp. 321-322
Author(s):  
J. R. Walsh ◽  
L. Walsh
Keyword(s):  
Emission Line ◽  
Linear Polarization ◽  
Diagnostic Tool ◽  
Line Emission ◽  
Planetary Nebulae ◽  
Central Star ◽  
Line Profiles ◽  
Gaseous Emission ◽  
Atmospheric Scattering ◽  
Spatially Varying

There is a wealth of evidence for the presence of dust in PN from continuum and line emission in the IR, spatially varying extinction and ERE emission in the optical and strength of resonance lines in the UV. The dust emits strongly in the IR but in the UV-optical absorbs and scatters the radiation from the central star and the gaseous emission envelope. Linear polarization of PN light is thus an expected consequence of the presence of dust both within and outside the ionized region. Intrinsic scattering haloes of PN can be confused with local (telescope + atmospheric) scattering; polarimetry however allows the morphology of a dusty halo to be studied. Spectropolarimetry of emission line profiles allows the kinematics of the dust relative to the gaseous emission to be uniquely studied. Polarization contributes to understanding the scattering properties of the grains in PN and how they relate to those of the general ISM to which they will subsequently contribute.

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