urn:nasa:pds:context:instrument:pvo.omag 1.0 1.7.0.0 Product_Context 2020-08-26 1.0 extracted metadata from PDS3 catalog and modified to comply with PDS4 Information Model urn:nasa:pds:context:instrument_host:spacecraft.pvo::1.0 instrument_to_instrument_host Busse, F., 'Generation of planetary field by convection', Phys. Earth Planet. Int., vol. 12, p. 350, 1976. reference.BUSSE1976 Dolginov, S.S., Y.G. Yeroshenko and L. Davis, 'On the nature of the magnetic field near Venus', Kosmich. Issled., vol. 7, p. 747, 1969. reference.DOLGINOVETAL1969 [see ELPHICETAL1980A] reference.ELPHICETAL1979 Gordon, D.I., and R.E. Brown, Recent Advances in Fluxgate Magnetometry, IEEE Trans. on Magnetics, Vol. MAG-8, 76, 1972. reference.GORDONETAL1972 Russell, C.T., 'The magnetic moment of Venus: Venera-4 measurements reinterpreted,' Geophys. Res. Lett., vol. 3, p. 125, 1976. reference.RUSSELL1976 Russell, C.T., The ISEE 1 and 2 fluxgate magnetometers, IEEE Trans. Geosci. Electro., GE-16, P. 239, 1978. reference.RUSSELL1978 Russell, C.T., R.C. Elphic, and J.A. Slavin, 'On the strength of the Venus bow shock', Nature, 1979. reference.RUSSELLETAL1979A Russell, C.T., R.C. Elphic, and J.A. Slavin, 'Initial Pioneer Venus magnetic field results: Dayside observations', Science, vol. 203, p. 745, 1979. reference.RUSSELLETAL1979B Russell, C.T., and R.C. Elphic, 'Observation of magnetic flux ropes in Venus ionosphere', Nature, vol. 279, p. 616, 1979. reference.RUSSELLETAL1979C Russell, C.T., R.C. Elphic, and J.A. Slavin, 'Initial Pioneer Venus magnetic field results: Nightside observations', Science, vol 205, p. 114, 1979. reference.RUSSELLETAL1979D Russell, C.T., R.C. Snare, J.D. Means, and R.C. Elphic, 'Pioneer Venus Orbiter Fluxgate Magnetometer', Ieee Trans. Geo. Elec., Vol. GE 18, No. 1 p. 32, 1980. reference.RUSSELLETAL1980 Slavin, J.A., R.C. Elphic, and C.T. Russell, 'A comparison of Pioneer Venus and Venera bow shock observations: Evidence for a solar cycle variation', Geophys. Res. Lett., 1979. reference.SLAVINETAL1979A Slavin, J.A., R.C. Elphic, C.T. Russell, J.H. Wolfe, and D.S. Intriligator, 'Position and shape of the Venus bow shock: Pioneer Venus orbiter magnetometer observations', Geophys. Res. Lett., 1979. reference.SLAVINETAL1979B Smith, E.J., L. Davis, Jr., P.J. Coleman, Jr., and C.P. Sonett, Science, vol. 139, p. 909, 1963. reference.SMITHETAL1963 Snare, R.C. and J.D. Means, A Magnetometer for the Pioneer Venus Orbiter, IEEE Trans. Magnetics, vol. MAG-13(5), 1107, (REPLACED BY SNARE&MEANS1977), 1977. reference.SNAREETAL1977 FLUXGATE MAGNETOMETER Magnetometer not applicable not applicable PI PDS User Id : CTRUSSELL Build Date : 1976 Instrument Mass : 1.98 Instrument Height : .15 Instrument Length : .22 Instrument Width : .15 Instrument Manufacturer Name : Westinghouse Electric Instrument Serial Number : 59-6803 (5968a03, 5968b03) ---------------------------------------------------------- Pioneer Venus Orbiter Fluxgate Magnetometer C.T. Russell, R.C. Snare, J.D. Means, and R.C. Elphic IEEE Transactions on Geoscience and Remote Sensing, January 1980. ---------------------------------------------------------- Abstract ======== The Earth's atmosphere is shielded from the solar wind, the rapidly expanding ionized gas of the sun's outer corona, by a moderately strong magnetic field generated by a dynamo inside the liquid core of the earth. That Venus is not thus shielded was evident from the measurements of the earliest probes to Venus [1], [2]. It was not certain that these measurements indicated that Venus had no intrinsic field. Rather, the existence of a small intrinsic field was still possible [3], and in fact expected from dynamo models [4]. A measure of the size of any Venus moment would be a check on our understanding of planetary dynamos. Furthermore, the solar wind was thought to interact directly with the upper atmosphere of Venus, a situation quite unlike that probed on other planetary missions. (Mars may have a similar interaction with the solar wind, but Martian studies have concentrated on the surface and lower atmosphere rather than the upper atmosphere.) Such an interaction is only poorly understood. It is possible that the weak magnetic field of the solar wind could act to shield the upper atmosphere by inhibiting the solar wind penetration into the atmosphere. Thus it was important for both aeronomical and planetological reasons to measure the magnetic field in the near vicinity of Venus. Only from an orbiter with a controllable periapsis altitude could the requisite series of low-altitude measurements be made. The intent of the Pioneer Venus mission was to be both comprehensive and low cost. The former requirement led to the inclusion of a large number of instruments and the need for a moderately high data rate and hence a despun antenna. The latter requirement led to a spinning spacecraft, a minimum magnetic cleanliness program and no allowance for redundancy. Even with a despun antenna the Pioneer Venus spacecraft would sometimes have to transmit data at rates as low as 8 bits/s when Venus was on the far side of the sun and the deep space net telemetry stations were being used for outer planet missions. These constraints made for some exacting design challenges both for the spacecraft design team and the magnetometer team. References [1] E.J. Smith, L. Davis, Jr., P.J. Coleman, Jr., and C.P. Sonett, Science, vol. 139, p. 909, 1963. [2] Sh. Sh. Dolginov, Ye. G. Yeroshenko and L. Davis, 'On the nature of the magnetic field near Venus,' Kosmich. Issle vol. 7, p. 747, 1969. [3] C.T. Russell, 'The magnetic moment of Venus: Venera-4 measurements reinterpreted,' Geophys. Res. Lett., vol. 3 125, 1976.