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Line of Sight Magnetic Fields

This study explores the Zeeman effect in magnetic fields across various astronomical sources, particularly focusing on diffuse clouds. We derive magnetic field strengths and turbulence characteristics from observed spectral lines of HI and maser emissions. Key results include measurements of B los in sources like W3OH and DR21OH, revealing critical insights into the interstellar medium's magnetic properties. Our findings contribute to a deeper understanding of the dynamics of star formation and the role of magnetic fields in these environments.

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Line of Sight Magnetic Fields

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  1. Line of Sight Magnetic Fields

  2. Zeeman Effect Z = B Z, Z  1 – 2 Hz/G, (ZH I = 1.4 Hz/G) V = LR  (dI/d)(Zcos)  line of sight B Q or U  (d2I/d2)(Zsin)2  plane of sky B (not really) (dI/d)Z  I (Z/ FWHM)

  3. Diffuse Cloud (H I Zeeman) Arecibo “Millennium” Survey I opacity profile CNM component (1 of 6) 3C 138 V opacity profile  dI/dv Blos = 5.6  1.0 G Blos = 11  3.1 G

  4. L1448 (OH Zeeman) Blos=28 6 µG Blos=25 5 µG

  5. DR21OH (CN Zeeman) Blos = 0.4, 0.7 mG

  6. W3OH (excited OH, maser Zeeman) 8-11 mG

  7. W3 IRS5 (H2O maser Zeeman)

  8. Blos in HI toward Trapezium

  9. Blos in the HV HI component

  10. W 3

  11. Zeeman Effect Results Species  (GHz) n(protons/cm-3 B H I 1.4 101-2 3-10 G OH (~thermal) 1.6 103-4 10-100 G CN 113.5 105-60.3-1 mG OH (masers) 1.6, 6.0, 13.4 107-8 1-10 mG H2O (masers) 22.2 109-10 10-100 mG

  12. Results for Field Strength

  13. Results for Mass/Flux

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