Angular Expansion Measurement of the Young and Compact Planetary Nebula V[CLC]y[/CLC] 2-2

1998 ◽  
Vol 115 (6) ◽  
pp. 2466-2474 ◽  
Author(s):  
Haryadi Christianto ◽  
E. R. Seaquist
Keyword(s):  
Planetary Nebula ◽  
Angular Expansion

Detection of the Angular Expansion Rate and Determination of the Distance of the Planetary Nebula NGC 6302

1993 ◽  
Vol 416 ◽  
pp. 620 ◽  
Author(s):  
Yolanda Gomez ◽  
Luis F. Rodriguez ◽  
James M. Moran
Keyword(s):  
Planetary Nebula ◽  
Expansion Rate ◽  
Angular Expansion

scholarly journals A distance estimate based on angular expansion for the planetary nebula NGC 6881

2011 ◽  
Vol 414 (4) ◽  
pp. 3129-3133 ◽  
Author(s):  
Lizette Guzmán-Ramírez ◽  
Yolanda Gómez ◽  
Laurent Loinard ◽  
Daniel Tafoya
Keyword(s):  
Planetary Nebula ◽  
Distance Estimate ◽  
Angular Expansion

scholarly journals The Angular Expansion and Distance of the Planetary Nebula BD +30°3639

2002 ◽  
Vol 123 (5) ◽  
pp. 2676-2688 ◽  
Author(s):  
Jianyang Li ◽  
J. Patrick Harrington ◽  
Kazimierz J. Borkowski
Keyword(s):  
Planetary Nebula ◽  
Angular Expansion

scholarly journals HST Measurements of the Angular Expansion, Kinematics and Distance of the Planetary Nebula Bd+30°3639

2003 ◽  
Vol 209 ◽  
pp. 480-480
Author(s):  
J. Patrick Harrington ◽  
Jianyang Li ◽  
Kazimierz J. Borkowski
Keyword(s):  
Planetary Nebula ◽  
Three Dimensional ◽  
Axial Ratio ◽  
Position Angle ◽  
Model Atmosphere ◽  
Brightness Variation ◽  
Radio Continuum ◽  
Line Of Sight ◽  
Radial Expansion ◽  
Angular Expansion

The HST WFPC2 camera was used to obtain images of the planetary nebula BD+30°3639 at two epochs separated by 5.66 years. The expansion of the nebula in Hα and [N II] has been measured using several methods. Detailed expansion maps for both emission lines were constructed from nearly 200 almost independent features. There is good agreement between the (independent) Hα and [N II] proper motions. There are clear deviations from uniform radial expansion, with higher expansion rates in regions where the shell is faintest, such as the south-west quadrant.HST STIS echelle spectra obtained in the C II] λ2326 multiplet provide well-resolved expansion velocities at two position angles. We find that the central velocity split is ±36.3 km s-1 at a position angle of 99°.To determine the distance of BD+30°3639 by comparison of the angular expansion and the radial expansion, we must address the problem of the three dimensional shape of the nebula. We measured the angular expansion along the position of the 99° echelle slit, finding displacements of 4.25 mas yr-1 at the shell edge (2″.47 from the center). If the nebula were spherical, this would imply a distance of 1.80 kpc. But there is evidence that the nebula is elongated along the line of sight, which suggests that the actual distance is less. Radio continuum images from 5 and 15 GHz VLA observations provide information on the extent of the radial elongation. We fit the radio brightness variation and the echelle data by approximating the nebula as an ellipsoid. Our model has an axial ratio of 1.56, is inclined to the line of sight by 9°.7, and exhibits an expansion in the plane of the sky which is 2/3 that in the radial direction, leading to a distance of 1.2 kpc. Based on a recent model atmosphere (Crowther et al., these proceedings), this distance implies a stellar luminosity of 4250 L⊙.

High‐Resolution X‐Ray Image of the Hydrogen‐deficient Planetary Nebula Abell 30

1997 ◽  
Vol 482 (2) ◽  
pp. 891-896 ◽  
Author(s):  
You‐Hua Chu ◽  
Thomas H. Chang ◽  
Gail M. Conway
Keyword(s):  
High Resolution ◽  
Planetary Nebula ◽  
X Ray

The Kinematics and Excitation of Molecular Hydrogen Emission in the Planetary Nebula BD +30o3639

1998 ◽  
Vol 498 (1) ◽  
pp. 267-277 ◽  
Author(s):  
D. L. Shupe ◽  
J. E. Larkin ◽  
R. A. Knop ◽  
L. Armus ◽  
K. Matthews ◽  
...  
Keyword(s):  
Planetary Nebula ◽  
Molecular Hydrogen ◽  
Hydrogen Emission

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

The Structure and Dynamics of the Proto–Planetary Nebula M1‐92

1998 ◽  
Vol 504 (2) ◽  
pp. 915-920 ◽  
Author(s):  
V. Bujarrabal ◽  
J. Alcolea ◽  
R. Neri
Keyword(s):  
Planetary Nebula ◽  
Structure And Dynamics

scholarly journals Planetary Nebulae in M31: Abundances, and comparison with bright Planetary Nebulae in the LMC

1997 ◽  
Vol 180 ◽  
pp. 475-476
Author(s):  
M. G. Richer ◽  
G. Stasińska ◽  
M. L. McCall
Keyword(s):  
Planetary Nebula ◽  
Luminosity Function ◽  
Large Population ◽  
Wavelength Region ◽  
Planetary Nebulae ◽  
Surprising Result ◽  
Population Synthesis ◽  
Abundance Distribution ◽  
Wide Range ◽  
The Mean

We have obtained spectra of 28 planetary nebulae in the bulge of M31 using the MOS spectrograph at the Canada-France-Hawaii Telescope. Typically, we observed the [O II] λ3727 to He I λ5876 wavelength region at a resolution of approximately 1.6 å/pixel. For 19 of the 21 planetary nebulae whose [OIII]λ5007 luminosities are within 1 mag of the peak of the planetary nebula luminosity function, our oxygen abundances are based upon a measured [OIII]λ4363 intensity, so they are based upon a measured electron temperature. The oxygen abundances cover a wide range, 7.85 dex < 12 + log(O/H) < 9.09 dex, but the mean abundance is surprisingly low, 12 + log(O/H)–8.64 ± 0.32 dex, i.e., roughly half the solar value (Anders & Grevesse 1989). The distribution of oxygen abundances is shown in Figure 1, where the ordinate indicates the number of planetary nebulae with abundances within ±0.1 dex of any point on the x-axis. The dashed line indicates the mean abundance, and the dotted lines indicate the ±1 σ points. The shape of this abundance distribution seems to indicate that the bulge of M31 does not contain a large population of bright, oxygen-rich planetary nebulae. This is a surprising result, for various population synthesis studies (e.g., Bica et al. 1990) have found a mean stellar metallicity approximately 0.2 dex above solar. This 0.5 dex discrepancy leads one to question whether the mean stellar metallicity is as high as the population synthesis results indicate or if such metal-rich stars produce bright planetary nebulae at all. This could be a clue concerning the mechanism responsible for the variation in the number of bright planetary nebulae observed per unit luminosity in different galaxies (e.g., Hui et al. 1993).

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