About: Inclination instability

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An inclination instability is a dynamical instability that can occur in a disk of objects with eccentric orbits, causing it to form into a conical shape. The gravity of the objects causes an exponential growth of their inclinations while reducing their eccentricities. The inclination instability also results in a clustering of the arguments of perihelion of the objects orbits, similar to what has been observed among the extreme trans-Neptunian objects with semi-major axes greater than 150 AU, it does not produce an alignment of the longitudes of perihelion, however. For an inclination instability to be responsible for the observed clustering, a disk with a mass of 1-10 Earth masses must have existed for over a billion years. This is more than is estimated from current observations, and lon

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  • An inclination instability is a dynamical instability that can occur in a disk of objects with eccentric orbits, causing it to form into a conical shape. The gravity of the objects causes an exponential growth of their inclinations while reducing their eccentricities. The inclination instability also results in a clustering of the arguments of perihelion of the objects orbits, similar to what has been observed among the extreme trans-Neptunian objects with semi-major axes greater than 150 AU, it does not produce an alignment of the longitudes of perihelion, however. For an inclination instability to be responsible for the observed clustering, a disk with a mass of 1-10 Earth masses must have existed for over a billion years. This is more than is estimated from current observations, and longer than the timescale of the depletion of the planetesimal disk in models of the early Solar System. (en)
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  • An inclination instability is a dynamical instability that can occur in a disk of objects with eccentric orbits, causing it to form into a conical shape. The gravity of the objects causes an exponential growth of their inclinations while reducing their eccentricities. The inclination instability also results in a clustering of the arguments of perihelion of the objects orbits, similar to what has been observed among the extreme trans-Neptunian objects with semi-major axes greater than 150 AU, it does not produce an alignment of the longitudes of perihelion, however. For an inclination instability to be responsible for the observed clustering, a disk with a mass of 1-10 Earth masses must have existed for over a billion years. This is more than is estimated from current observations, and lon (en)
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  • Inclination instability (en)
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