Corpus ID: 10228256

A New Model for the Galactic Distribution of Free Electrons and its Fluctuations

@inproceedings{Cordes2001ANM,
  title={A New Model for the Galactic Distribution of Free Electrons and its Fluctuations},
  author={James M. Cordes and T. J. W. Lazio},
  year={2001}
}
We present a new model for the Galactic distribution of free electrons. It (a) describes the distribution of the free electrons responsible for pulsar dispersion measures and thus can be used for estimating the distances to pulsars; (b) describes large-scale variations in the strength of fluctuations in electron density that underly interstellar scattering; (c) can be used to interpret interstellar scattering and scintillation observations of Galactic objects and of extragalactic objects, such… Expand
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ApJS, 83, 111 Table 1 Data Summary Number of Measurements Work D
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specbroad(sm,nu,vperp): calculates the spectral broadening, ∆ν b (Hz), that is proportional to the reciprocal of the scintillation time
  • specbroad(sm,nu,vperp): calculates the spectral broadening, ∆ν b (Hz), that is proportional to the reciprocal of the scintillation time
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Radiative Processes
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): calculates the angular broadening, θ d (mas), appropriate for the scattering geometry for an extragalactic source
    ): calculates the angular broadening, θ d (mas), of a Galactic source
      5 indicates which spiral arm contributes to the density, with numbering as in the text and where a zero value denotes an interarm region
      • 5 indicates which spiral arm contributes to the density, with numbering as in the text and where a zero value denotes an interarm region
      5 indicates which spiral arm contributes to the density, with numbering as in the text and where a zero value denotes an interarm region
        Sample output for ℓ = 45 @BULLET , b = 5 @BULLET , and DM = 50 pc cm −3 is
        • Sample output for ℓ = 45 @BULLET , b = 5 @BULLET , and DM = 50 pc cm −3 is
        calculates the pulse broadening time, τ d (ms). See Eq. 9. 2. scintbw(d,sm,nu): calculates the scintillation bandwidth, ∆ν d (MHz). See Eq
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