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3 edition of The ionization structure of planetary nebulae. found in the catalog.

The ionization structure of planetary nebulae.

# The ionization structure of planetary nebulae.

Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, D.C, Springfield, Va .
Written in English

Edition Notes

The Physical Object ID Numbers Statement Timothy Barker Series NASA contractor report -- NASA CR-180142 Contributions United States. National Aeronautics and Space Administration Format Microform Pagination 1 v Open Library OL14982527M

ABSTRACT Observations of the CO I 52 and 88vm lines and the CN 57pm line have been made at 6 positions and the [Ne I 36pm line at 4 positions in the Orion Nebula to probe its ionization structure. The measurements, made with a " diameter beam, were spaced every 45" in a line south from and including the Trapezium. Size: 1MB.   Abstract. Though the low-ionization small-scale structures (LISs) such as knots, filaments and jets of planetary nebulae (PNe) are known for ∼30 yr, some of thCited by:

@article{osti_, title = {PHOTOMETRY OF THE STINGRAY NEBULA (V ARA) FROM TO ACROSS THE IONIZATION OF ITS PLANETARY NEBULA}, author = {Schaefer, Bradley E. and Edwards, Zachary I.}, abstractNote = {Up until around , the Stingray was an ordinary B1 post-AGB star, but then it suddenly sprouted bright emission lines like in a planetary nebula (PN), and soon . The main aim of this work is to investigate the effect of charge transfer reaction upon gaseous nebula structure, temperature and recombination coefficients of nitrogen and oxygen. We have been used CLOUDY 90 to determine the ionization structure of nitrogen and oxygen. We have used the abundance of heavy elements relative to hydrogen He = , C = , N = , O = and Ne = Author: Belay Sitotaw Goshu.

New technology has captured a number of phenomenal images of planetary nebulae in extreme depth. In doing so, it has revealed the complexities that could occur at the end of the life of the sun. Planetary nebulae are formed after medium or low mass stars, such as the Sun, exhaust their hydrogen fuel in the stellar core. At this point the structure of the star changes so it can achieve a new equilibrium condition in which it can continue to burn; the outer layers of .

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Cite this paper as: Barker T. () The Ionization Structure of Planetary Nebulae. In: Weinberger R., Acker A.

(eds) Planetary Nebulae. International Astronomical Union / Cited by: 2. Get this from a library. The ionization structure of planetary nebulae: VI. NGC [Timothy Barker; Wheaton College (Norton, Mass.). Department of Physics and Astronomy.; United States.

National Aeronautics and Space Administration.]. Belay Sitotaw Goshu, Ionization Structure of Heavy Metals for Planetary Nebulae, American Journal of Astronomy and 6, No. 2,pp. Author: Belay Sitotaw Goshu. The starting point for the study of the ionization structure of planetary nebulae, and gaseous nebulae in general, is the ionization formula.

The atoms can be ionized in two ways: under direct radiation of the central star, and by collisions with free electrons. In the first case one has The ionization structure of planetary nebulae. book, in the second, collisional : Grigor A.

Gurzadyan. The Ionization Structure of Planetary Nebulae X. NGC TIMOTHY BARKER 1,2 Department of Physics and Astronomy Wheaton College Received October 3; 1Visiting Astronomer, Kitt Peak National Observatory, National Optical Astronomy Observatories, operated by the Association of Universities for Research in Astronomy, Inc., under contract with the.

Forms and structure. Compared with diffuse nebulae (see H II region), planetary nebulae are small objects, having a radius typically of 1 light-year and containing a mass of gas of about solar mass. One of the largest-known planetary nebulae, the Helix Nebula (NGC ) in the constellation Aquarius, subtends an angle of about 20 minutes of arc—two-thirds the angular size of the Moon.

This authoritative volume presents a thoroughly modern understanding of planetary nebulae, integrating new developments in stellar physics with the dynamics of nebular evolution.

It covers all the stages in the evolution of planetary nebulae, carefully synthesizes observations from across the spectrum and clearly explains all the key physical processes at work. Abstract: We report the detection of near-IR H$_2$ emission from the low-ionization structures (knots) in two planetary nebulae.

The deepest ever, high-angular resolution H$_2$ S(1) at $\mu$, H$_2$ S(1) at $\mu$ and Br$\gamma$ images of K and NGCobtained using the Near InfraRed Imager and Spectrometer (NIRI) at Gemini-North, are analyzed by:   Preface; 1. History and overview; 2. Ionization structure of planetary nebulae; 3.

Nebular line radiation; 4. Nebular continuum radiation; 5. The neutral gas component; 6. The dust component; 7. Observations of the central star of planetary nebulae; 8. Morphologies of planetary nebulae; 9.

Problems and questions; Asymptotic giant branch stars - progenitors of planetary nebulae; 11 Cited by: The 3-D ionization structure of the planetary nebula NGC Article in Astronomy and Astrophysics (3) March with 14 Reads How we measure 'reads'. We study the physical structure of H II regions, including Planetary Nebulae (PNe), through detailed analysis of the ionization structure and spectra of iron in relevant ionization stages.

40 Belay Sitotaw Goshu: Ionization Structure of Heavy Metals for Planetary Nebulae The organization of this paper is as follows. The first section describe the properties of the planetary nebulae database from Infrared Astronomical Satellite (IRAS) as given in the literature, focusing on the mainAuthor: Belay Sitotaw Goshu.

Low-ionization structures in planetary nebulae 3 Figure 1. Observed spectra of the NW jet in Wray (upper panel), covering the wavelength range of { A, obtained with [email protected], and SE outer NEB in NGC (lower panel) with a wavelength range of { A, and observed with the IDS attached to the Isaac Newton telescope Cited by: Coverage also describes exciting possibilities such as the use of planetary nebulae in determining the cosmic distance scale, the distribution of dark matter and the chemical evolution of galaxies.

This book provides graduate students with an accessible introduction to planetary nebulae, and researchers with an authoritative reference. This book presents a thoroughly modern understanding of planetary nebulae, integrating developments in stellar physics with the dynamics of nebular evolution.

It also describes exciting possibilities such as the use of planetary nebulae in determining the cosmic distance scale, the distribution of dark matter and the chemical evolution of galaxies.5/5(1).

Timothy Barker has written: 'The ionization structure of planetary nebulae' -- subject(s): Planetary nebulae. Book 1 online resource (xiii, pages History and overview Ionization structure of planetary nebulae Nebular line radiation Nebular continuum radiation The neutral gas component The dust component Observation of the cental star of planetary nebulae Morphologies of planetary nebulae Problems and questions Asymptotic giant.

Planetary Nebulae- completely unrelated to planets. planetary nebulae is when gas and plasma are formed after certain types of stars die. it sometimes looks like gas planets, like neptune and.

This written account of the Symposium on Planetary Nebulae was prepared from manuscripts submitted by the participants. Nearly every paper that was presented at the meeting is reproduced here, in either complete or abbreviated form. The dis­ cussions have been somewhat shortened and rearranged, but.

A planetary nebula, abbreviated as PN or plural PNe, is a type of emission nebula consisting of an expanding, glowing shell of ionized gas ejected from red giant stars late in their lives.

The term "planetary nebula" is a misnomer because they are unrelated to planets or term originates from the planet-like round shape of these nebulae observed by astronomers through early.

Planetary nebulae as a phase of stellar evolution 2 Discovery and identiﬁcation 3 Confusion with other galactic objects 4 Plantary nebulae as a physics laboratory 7 2 Ionization structure of planetary nebulae 9 Photoionization 9 Recombination 13 Ionization structure of a static nebula 16 Ionization of complex File Size: KB.Planetary nebulae present a fascinating range of shapes and morphologies.

They are ideal laboratories for the study of different astrophysical processes: atomic physics, radiative transfer, stellar winds, shocks, wind-wind interaction, and the interaction between stellar winds and the.The book is slim and stylish, characteristic of the Cambridge Astrophysics Series.'Dr X.-W.

Lou, Contemporary Physics, "The reader who is inspired by the images of planetary nebulae to go beyond aesthetic appreciation, to delve into the physics and astrophysics of these fascinating structures in space, cannot do better than to start with this.