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Polarization of background starlight and the structure of the interstellar magnetic field

Published online by Cambridge University Press:  03 August 2017

Alyssa A. Goodman ,
Philip C. Myers  and
Pierre Bastien
Alyssa A. Goodman
Affiliation:
Astronomy Department, University of California, Berkeley, CA 94720, USA E—mail AGOODMAN@UCBBKYAS.BITNET
Philip C. Myers
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 42, Cambridge, MA 02138, USA E—mail MYERS@CFARG1.BITNET
Pierre Bastien
Affiliation:
Department de Physique, Université de Montreal, BP 6128, Succursale A, Montreal, PQ H3C 3J7, CANADA E-mail BASTIEN@CC.UMontreal.CA.BITNET

Abstract

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We discuss the use of polarization maps of background starlight in studying the structure of the interstellar magnetic field. We make the assumption that the polarization observed is due to magnetically aligned dust grains associated with interstellar clouds along the line of sight, and that the position angle (ΘE) of polarization observed gives the direction (modulo 180°) of , the plane-of-the-sky projection of the (line-of-sight-averaged) magnetic field.

There are two basic points in this paper. (1.) Out of context, the projected orientation of an elongated dark cloud may appear special (e.g. roughly "parallel" or “perpendicular”) in relation to the local (plane-of-the-sky) field direction given by polarization observations, but, when the view is expanded to include an entire complex of dark clouds, the shape and orientation of clouds within a complex often appears unrelated to the field structure. (2.) the dispersion in the postion angle of polarization observed in a region of the sky contains information about the ratio of the strength of the uniform (straight) component of the local magnetic field as compared to the dispersion (nonuniform component) in the field. Furthermore, in a region where Zeeman measurements covering the same region as polarization observations have been made, the uniform-to-nonuniform ratio deduced for the field from polarization data, can be combined with information about the line-of-sight field and an estimate of the correlation length of the field, to describe the magnetic field in three dimensions. We discuss the results of such an analysis for the dark cloud Lynds 204 (L204).

Keywords

Magnetic fieldsdark cloudsL204
Type
Poster Sessions
Information
Symposium - International Astronomical Union , Volume 147: Fragmentation of Molecular Clouds and Star Formation , 1991 , pp. 417 - 423
Copyright
Copyright © Kluwer 1991 

References

Chandrasekhar, S. and Fermi, E.: 1953, “Problems of Gravitational Instability in the Presence of a Magnetic Field.” Ap. J., 118, 113.Google Scholar
Goodman, A.A., Bastien, P., Myers, P.C., and Ménard, F.: 1990, “Optical Polarization Maps of Star Forming Regions in Perseus, Taurus, and Ophiuchus.” Ap. J., 359, 363.Google Scholar
Heiles, C.: 1988, “L204: A Gravitationally Confined Dark Cloud in a Strong Magnetic Environment.” Ap. J., 324, 321.Google Scholar
Heyer, M.H., Vrba, F.J., Snell, R.L., Schloerb, F.P., Strom, S.E., Goldsmith, P.F. and Strom, K.M.: 1987, “The Magnetic Evolution of the Taurus Molecular Clouds I. Large Scale Properties.” Ap. J., 321, 855.Google Scholar
Jokipii, J.R., and Parker, E.N.: 1969, “Stochastic Aspects of Magnetic Lines of Force with Application to Cosmic-Ray Propagation.” Ap. J., 155, 799.Google Scholar
Loren, R.B.: 1989, “The Cobwebs of Ophiuchus. I. Strands of 13CO: The Mass Distribution.” Ap. J., 338, 902.Google Scholar
McCutcheon, W.H., Vrba, F.J., Dickman, R.L., and Clemens, D.P.: 1986, “The Lynds 204 Complex: Magnetic Field Controlled Evolution?” Ap. J., 309, 619.Google Scholar
Moneti, A., Pipher, J.L., Helfer, H.L., McMillan, R.S., and Perry, M.L.: 1984, “Magnetic Field Structure in the Taurus Dark Cloud.” Ap. J., 282, 508.CrossRefGoogle Scholar
Myers, P.C. and Goodman, A.A.: 1990, “On the Dispersion in Direction of Interstellar Polarization.” submitted to Ap. J. Google Scholar
Tamura, M., Nagata, T., Sato, S., and Tanaka, M.: 1987, “Infrared polarimetry of dark clouds–I. Magnetic field structure in Heiles Cloud 2.” M. N. R. A. S., 224, 413.Google Scholar
Vrba, F.J., Strom, S.E., and Strom, K.M.: 1976, “Magnetic Field Structure in the Vicinity of Five Dark Cloud Complexes.” A.J., 81, 958.CrossRefGoogle Scholar
Zweibel, E.: 1990, “Magnetic Fieldline Tangling and Polarization Measurements in Clumpy Molecular Gas.” submitted to Ap. J. Google Scholar