scholarly journals HIP 3678: a hierarchical triple stellar system in the centre of the planetary nebula NGC 246★

2014 ◽  
Vol 444 (4) ◽  
pp. 3459-3465 ◽  
Author(s):  
C. Adam ◽  
M. Mugrauer
Keyword(s):  
Planetary Nebula ◽  
Stellar System

scholarly journals ALMA imaging of the nascent planetary nebula IRAS 15103–5754

2018 ◽  
Vol 480 (4) ◽  
pp. 4991-5009 ◽  
Author(s):  
José F Gómez ◽  
Gilles Niccolini ◽  
Olga Suárez ◽  
Luis F Miranda ◽  
J Ricardo Rizzo ◽  
...  
Keyword(s):  
Mass Loss ◽  
High Velocity ◽  
Planetary Nebula ◽  
Symmetry Axis ◽  
Stellar System ◽  
Line Emission ◽  
Ionized Gas ◽  
Molecular Line ◽  
Common Envelope ◽  
Loss Event

ABSTRACT We present continuum and molecular-line (CO, C18O, HCO+) observations carried out with the Atacama Large Millimeter/submillimeter Array toward the ‘water fountain’ star IRAS 15103–5754, an object that could be the youngest planetary nebula (PN) known. We detect two continuum sources, separated by 0.39 ± 0.03 arcsec. The emission from the brighter source seems to arise mainly from ionized gas, thus confirming the PN nature of the object. The molecular-line emission is dominated by a circumstellar torus with a diameter of ≃0.6 arcsec (2000 au) and expanding at ≃23 km s−1. We see at least two gas outflows. The highest-velocity outflow (deprojected velocities up to 250 km s−1), traced by the CO lines, shows a biconical morphology, whose axis is misaligned ≃14° with respect to the symmetry axis of the torus, and with a different central velocity (by ≃8 km s−1). An additional high-density outflow (traced by HCO+) is oriented nearly perpendicular to the torus. We speculate that IRAS 15103–5754 was a triple stellar system that went through a common envelope phase, and one of the components was ejected in this process. A subsequent low-collimation wind from the remaining binary stripped out gas from the torus, creating the conical outflow. The high velocity of the outflow suggests that the momentum transfer from the wind is extremely efficient, or that we are witnessing a very energetic mass-loss event.

Density waves in disk galaxies

1967 ◽  
Vol 31 ◽  
pp. 313-317 ◽  
Author(s):  
C. C. Lin ◽  
F. H. Shu
Keyword(s):  
Mathematical Analysis ◽  
Spiral Structure ◽  
Stellar System ◽  
Collective Modes ◽  
Disk Galaxies ◽  
Spiral Pattern ◽  
Density Waves ◽  
The Galaxy ◽  
Detailed Mathematical Analysis

Density waves in the nature of those proposed by B. Lindblad are described by detailed mathematical analysis of collective modes in a disk-like stellar system. The treatment is centered around a hypothesis of quasi-stationary spiral structure. We examine (a) the mechanism for the maintenance of this spiral pattern, and (b) its consequences on the observable features of the galaxy.

A Statistical Approach to Two-Parameter Families of Triple Close Approaches in Stellar System (I)

2012 ◽  
Vol 3 (7) ◽  
pp. 306-320
Author(s):  
Ranjeet Kumar ◽  
◽  
Navin Chandra ◽  
Surekha Tomar
Keyword(s):  
Statistical Approach ◽  
Stellar System ◽  
Two Parameter

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

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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