lmd_Fairhead1991.bib

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@article{1991ApJ...378..687F,
  author = {{Foster}, R.~S. and {Fairhead}, L. and {Backer}, D.~C.},
  title = {{A spectral study of four millisecond pulsars}},
  journal = {\apj},
  keywords = {Pulsars, Radio Astronomy, Radio Sources (Astronomy), Stellar Spectra, Analytic Functions, Frequency Ranges, Radiant Flux Density, Stellar Luminosity},
  year = 1991,
  month = sep,
  volume = 378,
  pages = {687-695},
  abstract = {{Flux density measurements of four millisecond pulsars, PSR 1620-26,
1821-24, PSR 1855 + 09, and PSR 1937 + 21, have been made to determine
their spectral indices in the frequency range between 425 MHz and 3 GHz.
The four objects are shown to have indices that range from -1.3 to -2.6.
The luminosities of these four pulsars are spread over nearly three
orders of magnitude. An analytic pulse component model is developed for
each object. Individual components are allowed to have different
spectral indices and hence different component ratios as a function of
frequency. Component separations are evaluated as a function of
frequency. The analytic models are used to determine dispersion measures
with a precision better than 0.01 pc/cu cm for each object.
}},
  doi = {10.1086/170469},
  adsurl = {http://adsabs.harvard.edu/abs/1991ApJ...378..687F},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{1991A&A...241..289F,
  author = {{Fairhead}, L.},
  title = {{Astrometric analysis of timing observations of the fast pulsar PSR 1937 + 214}},
  journal = {\aap},
  keywords = {Astrometry, Ephemerides, Pulsars, Time Measurement, Astronomical Observatories, Atomic Clocks, Correlation Coefficients, astrometry, ephemerides, pulsars: PSR 1937+214, time scales},
  year = 1991,
  month = jan,
  volume = 241,
  pages = {289-296},
  abstract = {{A new analysis of the first two years of timing data acquired on the
fast pulsar PSR 1937+214 at Arecibo is presented. Parameters are
evaluated with various models based on two ephemerides, two atomic time
scales and two TT-TB time transformations and comparison is carried out
with previously published results. We provide evidence that systematic
errors induced by the model adopted are 5 to 10 times larger than the
formal uncertainties calculated by the fitting procedure. One must
therefore exercise great care in the reduction method when comparing
results from different timing programs for precise astrometric
applications.
}},
  adsurl = {http://adsabs.harvard.edu/abs/1991A%26A...241..289F},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}