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DICTIONARY OF GEOPHYSICS, ASTROPHYSICS, and ASTRONOMY

DICTIONARY OF GEOPHYSICS, ASTROPHYSICS, and ASTRONOMY

DICTIONARY OF GEOPHYSICS, ASTROPHYSICS, and ASTRONOMY

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eccentricity<br />

Magnitude<br />

distance (km) Felt Intensity Damage<br />

2 0 I Not felt<br />

II Felt by a few people<br />

3 15 III Hanging objects sway<br />

IV Windows <strong>and</strong> doors rattle<br />

4 80 V Sleepers awaken<br />

5 150 VI Windows <strong>and</strong> glassware broken<br />

VII Difficult to st<strong>and</strong><br />

6 220 VIII Branches broken from trees<br />

7 400 IX Cracks in ground – general panic<br />

X Large l<strong>and</strong>slides – most masonry structures destroyed<br />

8 600 XI Nearly total destruction<br />

east-west effect An east-west anisotropy in<br />

the arrival of cosmic ray particles. At equal inclinations<br />

to the vertical, a higher flux of particles<br />

is observed from the west than from the<br />

east because of an asymmetry in the distribution<br />

of trapped orbits (see cutoff energy). The direction<br />

of the asymmetry (more from west than<br />

from east) shows that primary cosmic ray particles<br />

have a positive electric charge.<br />

easy access region Prior to the observations<br />

of the spacecraft Ulysses, the topology of the<br />

heliosphere was assumed to be similar to the<br />

one of the magnetosphere. In particular, above<br />

the solar poles cusp-like regions were expected<br />

where the cosmic radiation should have an easy<br />

access to the inner heliosphere, leading to higher<br />

fluxes over the poles compared to the ones at the<br />

same radial distance in the equatorial plane. Although<br />

Ulysses’ findings show an increase in the<br />

intensity of the galactic cosmic radiation over<br />

the sun’s poles, this increase is much smaller<br />

than the one expected in the picture of an easy<br />

access.<br />

Two physical mechanisms seem to contribute<br />

to this lack of easy access: (a) an unexpected<br />

high level of magnetic field turbulence, leading<br />

to an enhanced scattering <strong>and</strong> thus preventing<br />

a relatively large number of particles from<br />

penetrating deep into the heliosphere, <strong>and</strong> (b) a<br />

more peanut-like shape of the heliosphere with<br />

a wider extent over the poles owing to the fast<br />

solarwindflowingoutofthepolarcoronalholes.<br />

ebb current The tidal current that results<br />

when the water in bays <strong>and</strong> estuaries is higher<br />

© 2001 by CRC Press LLC<br />

than that in the adjoining sea. The opposite is<br />

referred to as a flood current.<br />

ebb delta A deposit of sediments immediately<br />

offshore a tidal inlet.<br />

ebb shoal See ebb delta.<br />

ebb tide Used essentially interchangeably<br />

with ebb current.<br />

eccentric Not centered, or not circular.<br />

Refers to elliptical orbits, where eccentricity is<br />

defined as the distance between the foci divided<br />

by the major axis, or equivalently<br />

ɛ 2 2 b<br />

= 1 − ,<br />

a<br />

where ɛ is the eccentricity, a is the semimajor<br />

axis, <strong>and</strong>b is the semiminor axis. The eccentricity<br />

of a circle is zero. For parabolas eccentricity<br />

= 1; for hyperbolic orbits, eccentricity exceeds<br />

1. See eccentricity.<br />

eccentric dipole An approximation to the<br />

internal magnetic field of the Earth. It replaces<br />

that field with the field of a magnetic dipole,<br />

suitably oriented, but achieves additional accuracy<br />

by displacing that dipole from the center<br />

of the Earth in such a way that the quadrupole<br />

harmonic terms (terms which diminish as 1/r 4 )<br />

are reduced as much as possible.<br />

eccentricity A characterization of conic sections,<br />

which are also solutions to the Newtonian<br />

equations of motion for a mass in the field of<br />

141

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