The Solar Probe Plus Radio Frequency Spectrometer: Measurement requirements, analog design, and digital signal processing

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  • M. Pulupa
    Space Sciences Laboratory University of California Berkeley California USA
  • S. D. Bale
    Space Sciences Laboratory University of California Berkeley California USA
  • J. W. Bonnell
    Space Sciences Laboratory University of California Berkeley California USA
  • T. A. Bowen
    Space Sciences Laboratory University of California Berkeley California USA
  • N. Carruth
    Space Sciences Laboratory University of California Berkeley California USA
  • K. Goetz
    School of Physics and Astronomy University of Minnesota Minneapolis Minnesota USA
  • D. Gordon
    Space Sciences Laboratory University of California Berkeley California USA
  • P. R. Harvey
    Space Sciences Laboratory University of California Berkeley California USA
  • M. Maksimovic
    LESIA Observatoire de Paris Meudon France
  • J. C. Martínez‐Oliveros
    Space Sciences Laboratory University of California Berkeley California USA
  • M. Moncuquet
    LESIA Observatoire de Paris Meudon France
  • P. Saint‐Hilaire
    Space Sciences Laboratory University of California Berkeley California USA
  • D. Seitz
    Space Sciences Laboratory University of California Berkeley California USA
  • D. Sundkvist
    Space Sciences Laboratory University of California Berkeley California USA

説明

<jats:p>The Radio Frequency Spectrometer (RFS) is a two‐channel digital receiver and spectrometer, which will make remote sensing observations of radio waves and in situ measurements of electrostatic and electromagnetic fluctuations in the solar wind. A part of the FIELDS suite for Solar Probe Plus (SPP), the RFS is optimized for measurements in the inner heliosphere, where solar radio bursts are more intense and the plasma frequency is higher compared to previous measurements at distances of 1 AU or greater. The inputs to the RFS receiver are the four electric antennas mounted near the front of the SPP spacecraft and a single axis of the SPP search coil magnetometer (SCM). Each RFS channel selects a monopole or dipole antenna input, or the SCM input, via multiplexers. The primary data products from the RFS are autospectra and cross spectra from the selected inputs. The spectra are calculated using a polyphase filter bank, which enables the measurement of low amplitude signals of interest in the presence of high‐amplitude narrowband noise generated by spacecraft systems. We discuss the science signals of interest driving the RFS measurement objectives, describe the RFS analog design and digital signal processing, and show examples of current performance.</jats:p>

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