Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..97...73p&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 97, no. 1, Nov. 1983, p. 73-78. In French.
Astronomy and Astrophysics
Astrophysics
2
Astronomical Models, Interstellar Magnetic Fields, Paleomagnetism, Planetary Nebulae, Cylindrical Plasmas, Field Strength, Stellar Magnetic Fields, Structural Stability, Thermal Diffusion
Scientific paper
A theoretical model of the evolution of the magnetic fields (suggested by observations of stable filaments and globules) of planetary nebulae (PN) is proposed. An analytical examination of the thermal diffusion of a cylindrical plasma is used to calculate an approximate lower bound of 0.0001 G for the magnetic-field strength of a typical PN with temperature 10,000 K and hydrogen number density 100/cu cm. It is pointed out that this field cannot simply be attributed to the central star (CS) of the PN because the field strength in the CS vicinity would be too large (about 940 GG). It is determined, however, that a star with a relatively compact 1-G field can produce an enlarged 'fossil' field of 0.0001 G because the field lines are transported with the ejected material of the PN shell at the time of explosion. A reasonable value of the postejection CS-vicinity field (4.8 G) is computed. PN fields of 0.0001 G should be detectable but have not yet been observed.
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