Magnetic Fields at Uranus

  title={Magnetic Fields at Uranus},
  author={Norman F. Ness and Mario H. Acu�a and Kenneth W. Behannon and Leonard F. Burlaga and John E. P. Connerney and Ronald P. Lepping and Fritz M. Neubauer},
  pages={85 - 89}
The magnetic field experiment on the Voyager 2 spacecraft revealed a strong planetary magnetic field of Uranus and an associated magnetosphere and fully developed bipolar masnetic tail. The detached bow shock wave in the solar wind supersonic flow was observed upstream at 23.7 Uranus radii (1 RU = 25,600 km) and the magnetopause boundary at 18.0 RU, near the planet-sun line. A miaximum magnetic field of 413 nanotesla was observed at 4.19 RU , just before closest approach. Initial analyses… 
Magnetic Fields at Neptune
The National Aeronautics and Space Administration Goddard Space Flight Center-University of Delaware Bartol Research Institute magnetic field experiment on the Voyager 2 spacecraft discovered a
Plasma waves in the magnetotail of Uranus
As the Voyager 2 spacecraft left Uranus during its encounter with the planet on January 24, 1986, it passed through the magnetotail over the distance range of about 11 RU to 79 RU. During this
Magnetic field and current structures in the magnetosphere of Uranus
We compare Voyager 2 magnetic field and plasma data with theoretical model calculations for the magnetosphere of Uranus in order to derive a global picture from the quite limited set of measurements.
Solar‐wind‐driven convection in the Uranian magnetosphere
We present an analytic, self-consistent model of time-dependent solar-wind-driven convection in the magnetosphere of Uranus. Because of the unusual orientation of the planetary rotation and magnetic
Electrostatic waves in the magnetosphere of Uranus
During its encounter with Uranus the plasma wave receiver on Voyager 2 observed electrostatic waves similar in many respects to those observed in other planetary magnetospheres. The most prominent
A physical model for the magnetosphere of Uranus at solstice time
Uranus is the only planet in the Solar System whose rotation axis and orbital plane are nearly parallel to each other. Uranus is also the planet with the largest angle between the rotation axis and
Voyager 2 Radio Observations of Uranus
Dynamically evolving radio events of various kinds embedded in these emissions suggest a Uranian magnetosphere rich in magnetohydrodynamic phenomena.
Uranus' magnetic field and particle drifts in its inner magnetosphere
Both the Q3 model (dipole and quadrupole) and OCT model (Q3 plus octupole) of Uranus' magnetic field within 5 R U are expressed in α and β (Euler potentials) coordinate systems. By using the α and β
The magnetic field of Uranus
A spherical harmonic model of the planetary magnetic field of Uranus is obtained from the Voyager 2 encounter observations using generalized inverse techniques which allow partial solutions to
The magnetotail of Uranus
Voyager 2 observations have shown that Uranus possesses a well-developed bipolar magnetotail similar in certain characteristics to that of Earth, in spite of an anomalously large tilt of the


Saturn's magnetosphere and its interaction with the solar wind
Pioneer 11 vector helium magnetometer observations of Saturn's planetary magnetic field, magnetosphere, magnetopause, and bow shock are presented. Models based on spherical harmonic analyses of
The magnetosphere of Uranus - Plasma sources, convection, and field configuration
At the time of the Voyager 2 flyby of Uranus, the planetary rotational axis will be roughly antiparallel to the solar wind flow. If Uranus has a magnetic dipole moment that is approximately aligned
Magnetic Field Studies at Jupiter by Voyager 2: Preliminary Results
Results and the magnetic field geometry confirm the earlier conclusion from Voyager I studies that Jupiter has an enormous magnetic tail, approximately 300 to 400 RJ in diameter, trailing behind the planet with respect to the supersonic flow of the solar wind.
Magnetic Field Studies by Voyager 2: Preliminary Results at Saturn
V Voyager 2 crossed the magnetopause of a relatively compressed Saturnian magnetosphere at 18.5 RS while inbound near the noon meridian and throughout the outbound magnetosphere passage, the field was relatively steady and smooth showing no evidence for any azimuthal asymmetry or magnetic anomaly in the planetary field.
Voyager 2 Radio Observations of Uranus
Dynamically evolving radio events of various kinds embedded in these emissions suggest a Uranian magnetosphere rich in magnetohydrodynamic phenomena.
The main magnetic field of Jupiter
The main magnetic field of Jupiter has been measured by the Goddard Space Flight Center flux gate magnetometer on Pioneer 11, and analysis of the data yields a more detailed model than that obtained
The induced magnetosphere of Titan
The Voyager 1 spacecraft had a close encounter (miss distance = 6970 km) with Titan (diameter = 5140 km) on November 12, 1980, while this large satellite was located within the Saturnian
Plasma Observations Near Uranus: Initial Results from Voyager 2
Extensive measurements of low-energy positive ions and electrons in the vicinity of Uranus have revealed a fully developed magnetosphere, with the boundary of the hot plasma component at L = 5 associated either with Miranda or with the inner limit of a deeply penetrating, solar wind-driven magnetospheric convection system.
Energetic Charged Particles in the Uranian Magnetosphere
From the locations of the absorption signatures observed in the electron flux, a centered dipole model for the magnetic field of Uranus with a tilt of 60.1 degrees has been derived, and a rotation period of the planet of 17.4 hours has been calculated, providing independent confirmaton of more precise determinations made by other Voyager experiments.