Engineering topics
Publications and source records attributed to Smith, E..
Evidence of a north-south asymmetry in the global heliosphere, first inferred from Ulysses cosmic ray observations, is investigated using simultaneous Ulysses and WIND magnetic field observations.
Direct measurements of the solar wind and the interplanetary magnetic field acquired over more than three solar cycles both near Earth and in interplanetary space are used to search for signatures of a persistent dependence of solar wind properties on solar longitude.
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This seminar is the first of two on the sun and heliosphere. It adresses the sun, solar wind and magnetic field with emphasis on recent observations by the Ulysses mission.
The concept of the heliosphere as a quasi-spherical cavity in the surrounding interstellar medium (ISM) has a history at least as long as that of an extended solar corona and solar wind.
Ulysses recently completed a second slow latitude scan of the northern heliosphere, a descent from 80.2 degrees North in July 1995 to the solar equator in December 1997.
In early 1992, at 13 degrees south latitude, in transit to the southern solar pole, Ulysses began to sample a recurrent high-speed solar wind stream which emanated from a coronal hole at the south pole of the Sun.
Atmospheric latent heating field is fundamental to all modes of atmospheric circulation and upper mixed layer circulations of the ocean.
Measurements of the specific entropy argument of solar wind protons, T/n superscript y-1, reveal that nearly every occurrence of a high-speed stream seen at Ulysses in 1992-3 is characterized by an abrupt interface at its trailing edge.
This paper describes the magnetometer instrument (MAG) to be flown on the Cassini spacecraft. The instrument consists of two magnetometers and an on-board data processing unit.
We summarize recent Ulysses observations of the variances over large temporal scales in the interplanetary magnetic field components and their increase as Ulysses approached the South Solar Pole. A model of these fluctuations is shown to provide a very good fit to the observed amplitude and temporal variation of the fluctuations. In addition, the model predicts that the transport of cosmic rays in the heliosphere will be significantly altered by this level of fluctuations. In addition to altering the inward diffusion and drift access of cosmic rays over the solar poles, we find that the magnetic fluctuations also imply a large latitudinal diffusion, caused primarily by the associated field-line random walk.
ICE and IMP-8 magnetic field data from 1984 1988 were analyzed in a magnetic coordinate system defined by the orientation of the solar magnetic dipole. The heliomagnetic latitude dependence of the radial component of the magnetic field (Br) was then investigated in the range of magnetic latitudes from 60 above and below the heliospheric current sheet. Investigators found that Br reverses sign abruptly across the current sheet, consistent with solar magnetic field models, but inconsistent with the source surface models.
ICE and IMP-8 data were analyzed in a heliomagnetic coordinate system defined by the orientation of the solar magnetic dipole. Observations were compared with several solar magnetic field models. The radial component of the magnetic field was found to reverse sign abruptly at the sector boundary; this is consistent with the sheet model, but inconsistent with source surface models .
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