magnetorotation instability - This has to do with the instability that can occur in a rotating magnetic field. In the context used by Wood, it refers to the stability of the magnetic field transferred to the nebula from the protosun. It depends in part on the amount of gas that is ionized and the rate at which the nebular gas revolves around the sun relative to the rate at which the magnetic field is rotating. Ionization will occur in the inner edge of the protoplanetary disk via irradiation from the protosun, as well as in the outer edges of the disk via irradiation from other stars.
Figure 2 - Note that in this plot, distance from the sun increases to the right (increasing "AU" or astronomical units).
Keplerian velocity - This is the velocity of a orbiting body determined by gravity. Kepler showed that for planets, there is a relationship between orbital period (the time to make one orbit) and the semi-major axis of an orbit. This means that the Keplerian orbital velocity depends only on the distance between the sun and the orbiting object, with objects closer to the sun moving faster. The same relationship holds for moons in orbit around a planet (faster movement closer to the planet). For the nebula, this means that bodies too large to be affected by non-gravitational effects (e.g., by gas drag, radiation pressure, or by the Poynting-Robertson Effect or Yarkovsky Effect) would move at Keplerian velocity as they orbit the sun.
density waves and spiral density waves - These
are wave-like fluctuations in particle density caused by gravitational
effects. They are observed in spiral galaxies and the rings of Saturn
and could have been important in the solar nebula, with waves in the protoplanetary
disk generated by the sun or by protoplanets in the disk. The density wave
pattern moves at a velocity that is not the same as the Keplerian velocity.
This means that for most locations (depending on orbital location), there
will be a difference in velocity between the wave pattern and the speed
at which particles are moving, and this difference can result in shock
heating as the waves pass through the particles in the disk. According
to Wood, the relative velocity and thus the strength of the shocks increases
as one moves closer to the sun (if the pattern is centered on the sun)
or away from Jupiter (if the pattern is centered on Jupiter). An
analogy to an astrophysical density wave is what I call a traffic accordion.
Imagine that cars are driving at normal speed (analogous to Keplerian velocity)
until they encounter traffic congestion (analogous to the density wave)
and are forced to slow down. Once the congestion eases up, the cars
can resume normal speed. Depending on the number of cars and their
speeds inside and outside the congestion pulse, it is possible for the
location of the pulse itself to move, at a speed that is different than
the speed that the cars are moving. One can extend the analogy further
by imagining that the cars will experience frictional heating as they enter
the traffic pulse (by application of brakes, analogous to shock heating).
Whether or not any significant heating occurs depends on the properties
of the medium and the strength of the shock. Shock wave heating is
a leading candidate to explain the melting process recorded by chondrules.
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Credit: NASA. |
Snow line - The distance from the protosun in the
protoplanetary disk corresponding to the position that water ice becomes
stable (unstable closer to the protosun as it is warmer; stable further
away).