Faraday Rotation and Depolarization in AGN Jets

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Burn's (1966) model for internal Faraday rotation Here, u is a scaled wavelength (u = λ/λ 1/2 ), and µ is the ratio of the random and uniform components of rotation measure. For µ > 0 and u > 1, χ is not ~ constant, but in fact executes a random walk.
Corollary: If the observed EVPA rotates through much more than 45 o , without a decrease in the fractional polarization, then the Faraday rotation MUST be external to the emitting region.
Page 1 and 2: Faraday Rotation and Depolarization
Page 3 and 4: OUTLINE 1. Preliminaries - Faraday
Page 5 and 6: Preliminaries (1) χ(λ) = χ ο +
Page 7 and 8: Faraday Depolarization: This is due
Page 9 and 10: So how CAN you distinguish between
Page 11: ack back front front observed obser
Page 15 and 16: "Core" rotation measures pre-VLBA V
Page 17 and 18: Radial distribution of rotation mea
Page 19 and 20: QUASARS: 3C 273 3C 279 3C 345 3C380
Page 21 and 22: CLUES ABOUT THE ENVIRONMENT Connect
Page 23 and 24: Core Depolarization 43 and 86 GHz (
Page 25 and 26: Newspaper reporter: “Why do you r
Page 27 and 28: ∆χ = 60 o : minimum RMs are ± 2
Page 29 and 30: Transverse gradient of rotation mea
Page 31 and 32: Asada et al 2002 RM gradient = 70 r
Page 33 and 34: Zavala & Taylor 2005 • RM gradien
Page 35 and 36: ∆χ = 60 o 43 GHz Rotation measur
Page 37 and 38: 3C 273, epoch 1999.26, from 8, 15 a
Page 39 and 40: Is there a systematic component of
Page 41 and 42: There is a significant transverse g
Page 43 and 44: There is a significant transverse g
Page 45 and 46: 3C 273, epoch 1999.37 Total intensi
Page 47 and 48: The upper limit on the interior cur
Page 51: KONIEC

Faraday Rotation and Depolarization in AGN Jets

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