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WFPC2 studies of the Crab Nebula. II. Ionization structure of the Crab filaments

Sankrit, Ravi and Hester, J. Jeff and Scowen, P. A. and Ballester, Gilda E. and Burrows, Christopher J. and Clarke, John T. and Crisp, David and Evans, R. W. and Gallagher, John S., III and Griffiths, Richard E. and Hoessel, John G. and Holtzman, Jon A. and Krist, John and Mould, Jeremy R. and Stapelfeldt, Karl R. and Trauger, John T. and Watson, Alan and Westphal, James A. (1998) WFPC2 studies of the Crab Nebula. II. Ionization structure of the Crab filaments. Astrophysical Journal, 504 (1). pp. 344-358. ISSN 0004-637X. doi:10.1086/306078.

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Narrowband images of the Crab Nebula taken with the Hubble Space Telescope (HST) WFPC2 show the morphology and ionization structure of the filaments in great detail. At HST resolution, low- and high-ionization emission from filaments in the Crab differ in two complementary respects. First, low-ionization emission is found to be concentrated in very sharp structures, while high-ionization emission is predominantly found in a much more diffuse component. For example, approximately 80% of emission from [O I]λ6300 arises in features with scales of less than 0".5, while only 10% of [O III]λ5007 emission arises in such compact structures. Second, individual filaments are found to lie along a sequence of ionization structures, ranging from features in which all lines are concentrated in the same compact volume through features with low-ionization cores surrounded by high-ionization envelopes. Hester and coworkers proposed in 1996 that this sequence can be understood as the result of the nonlinear development of magnetic Rayleigh-Taylor (R-T) instabilities along the interface between the Crab synchrotron nebula and swept-up ejecta. We present photoionization models of cylindrically symmetrical filaments consisting of a quadratic core surrounded by an extended envelope. A good deal of the observed variation in filament structure in the Crab can be matched by varying the assumed density profiles in these models. This implies that variations in the development of R-T instabilities in the Crab account for much of the spectral variation within the remnant. We also present a photoionization model of a uniform, low-density medium, which reasonably matches the extended diffuse component that dominates the high-ionization emission. This envelope model produces strong [O III] but virtually no [O I]. While the He I/Hβ ratio remains fairly constant throughout a range of filament models, this ratio is a factor of 5 lower in the envelope model. We find that the apertures used in ground-based spectroscopy of the Crab generally include emission from several discrete filaments as well as a component of diffuse emission. This places a fundamental limit on what can be inferred reliably from comparison of spectra with one-dimensional photoionization models. Many filament cores coincide with dust extinction features seen in a continuum image of the Crab. We consider one such feature in detail and find that the extinction of about 1.2 mag suggests that the dust-to-gas mass ratio may be an order of magnitude higher than is typical in the interstellar medium.

Item Type:Article
Related URLs:
URLURL TypeDescription
Crisp, David0000-0002-4573-9998
Gallagher, John S., III0000-0001-8608-0408
Mould, Jeremy R.0000-0003-3820-1740
Stapelfeldt, Karl R.0000-0002-2805-7338
Additional Information:© 1998 American Astronomical Society. Received 1998 January 21; accepted 1998 April 3. We thank the referee for a number of useful suggestions that improved the presentation of the ideas in this paper. This work was supported by NASA contract NAS 7-1260 to the WFPC2 IDT. This work was supported at ASU by NASA/JPL contracts 959289 and 959329.
Funding AgencyGrant Number
NASANAS 7-1260
Subject Keywords:ISM : individual (Crab Nebula); ISM : structure; supernova remnants
Issue or Number:1
Record Number:CaltechAUTHORS:20150121-095628407
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Official Citation:WFPC2 Studies of the Crab Nebula. II. Ionization Structure of the Crab Filaments Ravi Sankrit et al. 1998 ApJ 504 344
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:53937
Deposited By: Ruth Sustaita
Deposited On:21 Jan 2015 20:42
Last Modified:10 Nov 2021 20:25

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