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Motions and Structure of the Filamentary Envelope of the Crab Nebula

Trimble, Virginia (1968) Motions and Structure of the Filamentary Envelope of the Crab Nebula. Astronomical Journal, 73 (7). 535-547, 657. ISSN 0004-6256. https://resolver.caltech.edu/CaltechAUTHORS:20190918-133846829

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Abstract

Proper motions have been measured for 132 line-emitting filaments in the Crab Nebula on direct plates taken with the 100- and 200-in. telescopes. These motions, if assumed constant and extrapolated backward in time, converge toward a point about 12" southeast of the double star near the center of the nebula. The filaments approach, on the average, most closely to that point or expansion center in about the year 1140, indicating that the expansion has been somewhat accelerated. Proper motions and radial velocities were measured for an additional 126 features on the same direct plates and Mt. Wilson and Palomar spectra. These, along with other, nondynamical data, indicate a most probable distance to the object of 2.02 kpc. Two projections of the nebula perpendicular to the one seen in the plane of the sky are constructed and do not differ significantly from that presented to us. The proper motion and radial velocity of the nebula as a whole are found and converted into galactic coordinates. This requires several assumptions of questionable validity. The nebula seems to be moving about 114 km/sec faster than the galactic rotation at its position. The proper motion of the so-called central star translates into an equally unlikely space motion, but this is also extremely uncertain. The likelihood of a physical connection between the star and the nebula is discussed. The line-emitting filaments are shown to be distributed throughout the nebula rather than being confined to a thin outer envelope. The motions are largely radial, each filament having a velocity approximately proportional to its distance from the expansion center. The deviations from this proportionality are as large as 0.032"/yr or 300 km/sec and have mean values near 0.010"/yr or 70 km/sec. These deviations are correlated with the scatter of the filaments around the expansion center in 1140.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1086/110658DOIArticle
Additional Information:© 1968 American Astronomical Society • Provided by the NASA Astrophysics Data System. (Received 1 May 1968) The author is greatly indebted to Dr. Guido Münch, who originally suggested the project, has guided it throughout, and has taken plates especially for it. Thanks are also due to Dr. Jesse L. Greenstein, Dr. Richard P. Feynman, and Dr. Jan H. Oort, who read the manuscript and made many helpful suggestions, and to Dr. Rudolph Minkowski for the loan of observing charts and several illuminating conversations. Conversations with Dr. P. A. G. Scheuer, Dr. James E. Gunn, and Dr. Jeffrey D. Scargle were also most helpful. National Science Foundation Fellow 1966-68.
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Funding AgencyGrant Number
NSF Graduate Research FellowshipUNSPECIFIED
Issue or Number:7
Record Number:CaltechAUTHORS:20190918-133846829
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190918-133846829
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:98732
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:19 Sep 2019 14:09
Last Modified:03 Oct 2019 21:43

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