Kuiperian Objects and Wandering Cosmic Objects. (arXiv:1908.06191v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Couture_G/0/1/0/all/0/1">Gilles Couture</a>
We study the effects of an encounter between a wandering cosmic object (WCO)
of 0.1 solar mass and some Kuiperian Objects (KO). First, we let the WCO cross
the out-skirt of ou Kuiper belt. Such encounters can produce two types of solar
objects: Eccentric Kuiper Objects of type I (EKO-I) whose perihelion is
comparable to, but always smaller than the aphelion of the initial KO and
Eccentric Kuiper Objects of type II (EKO-II) whose perihelion can be as small
as a few AU. EKO-I tend to have a fairly large range of eccentricities, but
EKO-II tend to have very large eccentricities. Both tend to be produced in
clusters similar to those observed in Extreme TransNeptunian Objects (ETNO).
When a WCO crosses the path of an EKO-I, it will produce two main classes of
objects: Far Kuiper Objects (FKO) of types I and II. The Sednitos discovered in
the past years fit the FKO-I class with their large major axis and fairly large
eccentricity, while the FKO-II class is different with its large major axis but
smaller eccentricity and opposite spinning direction. When a WCO encounters an
EKO-II, the latter can remain in the same class, spinning in either direction,
it can also en up in the EKO-I class also spinning in either direction, but it
can also be sent onto orbits with extremely long semi-major axis, relatively
small eccentricity where both spins are allowed. This FKO-III class could be
likened to the Lower Oort Cloud Objects as their major axis is a fair fraction
of a light-year. These results lead us to consider the possibility that the
Kuiper Belt was once substantially larger than it is now, perhaps 90 AU. We
find some evidence of this scenario in current astronomical data.
We study the effects of an encounter between a wandering cosmic object (WCO)
of 0.1 solar mass and some Kuiperian Objects (KO). First, we let the WCO cross
the out-skirt of ou Kuiper belt. Such encounters can produce two types of solar
objects: Eccentric Kuiper Objects of type I (EKO-I) whose perihelion is
comparable to, but always smaller than the aphelion of the initial KO and
Eccentric Kuiper Objects of type II (EKO-II) whose perihelion can be as small
as a few AU. EKO-I tend to have a fairly large range of eccentricities, but
EKO-II tend to have very large eccentricities. Both tend to be produced in
clusters similar to those observed in Extreme TransNeptunian Objects (ETNO).
When a WCO crosses the path of an EKO-I, it will produce two main classes of
objects: Far Kuiper Objects (FKO) of types I and II. The Sednitos discovered in
the past years fit the FKO-I class with their large major axis and fairly large
eccentricity, while the FKO-II class is different with its large major axis but
smaller eccentricity and opposite spinning direction. When a WCO encounters an
EKO-II, the latter can remain in the same class, spinning in either direction,
it can also en up in the EKO-I class also spinning in either direction, but it
can also be sent onto orbits with extremely long semi-major axis, relatively
small eccentricity where both spins are allowed. This FKO-III class could be
likened to the Lower Oort Cloud Objects as their major axis is a fair fraction
of a light-year. These results lead us to consider the possibility that the
Kuiper Belt was once substantially larger than it is now, perhaps 90 AU. We
find some evidence of this scenario in current astronomical data.
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