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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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granulation<br />

have been broken at extremely high energies.<br />

Thus, many gauge particles would be very massive,<br />

explaining why we have not yet observed<br />

them. See spontaneous symmetry breaking.<br />

granulation Cellular structure of the photosphere<br />

visible at high spatial resolution. The<br />

characteristic scale of the granulation is ∼<br />

1000 km, ranging widely from∼ 300 km to over<br />

2000 km. Typical velocities present in the granules<br />

are horizontal outflows ∼ 1.4 km s −1 <strong>and</strong><br />

upflows in the center of the granules ∼ 1.8 km<br />

s −1 . Identifiable granules live for∼ 5to10min<br />

<strong>and</strong> at any one time ∼ 3 to 4× 10 6 granules<br />

cover the surface of the sun.<br />

grating spectrograph An instrument for the<br />

analysis of radiation at different wavelengths, in<br />

which light is dispersed by a diffraction grating.<br />

In a typical grating spectrograph design, light<br />

focused on the focal plane of the telescope is<br />

collimated (i.e., the rays of the beam are made<br />

parallel) on a blazed diffraction grating. Light<br />

of different wavelengths is thus diffracted along<br />

different directions, <strong>and</strong> it is then re-focused on<br />

a detector, for example a photographic plate or<br />

a CCD, by a lens or a mirror. Several designs<br />

exist, based on different choices of the focusing<br />

<strong>and</strong> collimating elements, or on the use of a<br />

reflection or a transmission grating. The spectral<br />

resolving power, i.e., the ability to separate<br />

two close spectral lines spaced by λ at wavelengthλ<br />

is usuallyλ/λ < ∼ 10 4 . See diffraction<br />

grating.<br />

gravitation The interaction between objects<br />

that in Newtonian theory depend only on their<br />

distances <strong>and</strong> masses:<br />

F=Gm1m2ˆrr −2 ,<br />

where F is the attractive force,m1 <strong>and</strong>m2 are the<br />

masses, r is their separation, ˆr is a unit vector<br />

between the masses, <strong>and</strong> G is Newton’s gravitational<br />

constant.<br />

In the more accurate description in general<br />

relativity, the gravitational field is a symmetric<br />

rank two tensor in four dimensions, which obeys<br />

Einstein’s equations, which have as a source<br />

the stress-energy tensor of the matter. General<br />

relativity reduces to the Newtonian description<br />

in weak-field, quasi stationary situations. See<br />

© 2001 by CRC Press LLC<br />

208<br />

Newtonian gravity, general relativity, Newtonian<br />

gravitational constant.<br />

gravitational collapse One of several possible<br />

final episodes of stellar evolution. Stars<br />

are supported against collapse under their own<br />

weight by gas pressure resulting from high temperature.<br />

The equilibrium of cold matter can<br />

be supported by the pressure of degenerate electron<br />

gas. The equilibrium of white dwarf stars is<br />

thoughttobeduetothis. Ch<strong>and</strong>rasekharshowed<br />

in 1939 that the maximal mass of a white dwarf<br />

is 1.4 solar mass <strong>and</strong> that stars more massive<br />

than this will collapse (to a neutron star or to a<br />

black hole).<br />

gravitational constant G In Newtonian<br />

physics, the acceleration of a particle towards<br />

the Earth isGm/r 2 wherem <strong>and</strong>r are the mass<br />

<strong>and</strong> radius of the Earth, respectively <strong>and</strong><br />

G= 6.670× 10 −8 cm 3 /g· sec 2<br />

is the gravitational constant.<br />

gravitational deflection of light The presence<br />

of a central mass (e.g., the sun) causes local<br />

curvature of spacetime, <strong>and</strong> trajectories of photons<br />

(the quanta of light) are deflected (attracted<br />

to the mass). In the case of a spherical central<br />

body, for small angle deflection, the angle deflected<br />

is<br />

θ= 4GM/dc 2 ,<br />

whereM is the central mass,G is Newton’s constant,c<br />

is the speed of light, <strong>and</strong>d is the impact<br />

parameter of the light past the mass. If the deflection<br />

were as if the photon were a particle<br />

in Newtonian gravity traveling at the speed of<br />

light, the deflection would be half the relativistic<br />

result. Deflection of light has been verified<br />

to parts in 1000 by observations of the direction<br />

to extragalactic radio sources, as the sun passes<br />

near their position in the sky. In the case of distant<br />

sources, deflection by intervening galaxies<br />

or clusters of galaxies causes lensing, leading to<br />

the appearance of multiple images, <strong>and</strong> of rings<br />

or arcs of distorted images. See gravitational<br />

lens, light deflection.<br />

gravitational equations The field equations<br />

of the gravitational interaction. The basic tenet

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