Probing Extrasolar Planetary Systems with Interstellar Meteors. (arXiv:1906.03270v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Siraj_A/0/1/0/all/0/1">Amir Siraj</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loeb_A/0/1/0/all/0/1">Abraham Loeb</a>
The first interstellar object, `Oumuamua, was discovered in the Solar System
by Pan-STARRS in 2017, allowing for a calibration of the impact rate of
interstellar meteors of its size $sim 100;$m. The discovery of CNEOS
2014-01-08 allowed for a calibration of the impact rate of interstellar meteors
of its size $sim 1;$m. Analysis of interstellar dust grains have allowed for
calibrations of the impact rate of smaller interstellar meteors down to the
size $sim 10^{-8};$m. We analyze the size distribution of interstellar
meteors, finding that for smooth power-law fits of the form $N(r)propto
r^{-q}$, the possible values of $q$ are in the range $3.41 pm 0.17$. We then
consider the possibility of analyzing interstellar meteors to learn about their
parent planetary systems. We propose a strategy for determining the orbits and
chemical compositions of interstellar meteors, using a network of $sim 600$
all-sky camera systems to track and conduct remote spectroscopy on meteors
larger than $sim 5$cm once every few years. It should also be possible to
retrieve meteorites from the impact sites, providing the first samples of
materials from other planetary systems.
The first interstellar object, `Oumuamua, was discovered in the Solar System
by Pan-STARRS in 2017, allowing for a calibration of the impact rate of
interstellar meteors of its size $sim 100;$m. The discovery of CNEOS
2014-01-08 allowed for a calibration of the impact rate of interstellar meteors
of its size $sim 1;$m. Analysis of interstellar dust grains have allowed for
calibrations of the impact rate of smaller interstellar meteors down to the
size $sim 10^{-8};$m. We analyze the size distribution of interstellar
meteors, finding that for smooth power-law fits of the form $N(r)propto
r^{-q}$, the possible values of $q$ are in the range $3.41 pm 0.17$. We then
consider the possibility of analyzing interstellar meteors to learn about their
parent planetary systems. We propose a strategy for determining the orbits and
chemical compositions of interstellar meteors, using a network of $sim 600$
all-sky camera systems to track and conduct remote spectroscopy on meteors
larger than $sim 5$cm once every few years. It should also be possible to
retrieve meteorites from the impact sites, providing the first samples of
materials from other planetary systems.
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