The Formation of Habitable Planets in the Four-Planet System HD 141399. (arXiv:1904.13120v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dvorak_R/0/1/0/all/0/1">R. Dvorak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loibnegger_B/0/1/0/all/0/1">B. Loibnegger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_L/0/1/0/all/0/1">L.Y. Zhou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_L/0/1/0/all/0/1">L. Zhou</a>
The presented work investigates the possible formation of terrestrial planets
in the habitable zone (HZ) of the exoplanetary system HD 141399. In this system
the HZ is located approximately between the planets c (a = 0.7 au) and d (a =
2.1 au). Extensive numerical integrations of the equations of motion in the
pure Newtonian framework of small bodies with different initial conditions in
the HZ are performed. Our investigations included several steps starting with
500 massless bodies distributed between planets c and d in order to model the
development of the disk of small bodies. It turns out that after some 10^6
years a belt-like structure analogue to the main belt inside Jupiter in our
Solar System appears. We then proceed with giving the small bodies masses
(Moon-mass) and take into account the gravitational interaction between these
planetesimal-like objects. The growing of the objects – with certain percentage
of water – due to collisions is computed in order to look for the formation of
terrestrial planets. We observe that planets form in regions connected to mean
motion resonances (MMR). So far there is no observational evidence of
terrestrial planets in the system of HD 141399 but from our results we can
conclude that the formation of terrestrial planets – even with an appropriate
amount of water necessary for being habitable – in the HZ would have been
possible.
The presented work investigates the possible formation of terrestrial planets
in the habitable zone (HZ) of the exoplanetary system HD 141399. In this system
the HZ is located approximately between the planets c (a = 0.7 au) and d (a =
2.1 au). Extensive numerical integrations of the equations of motion in the
pure Newtonian framework of small bodies with different initial conditions in
the HZ are performed. Our investigations included several steps starting with
500 massless bodies distributed between planets c and d in order to model the
development of the disk of small bodies. It turns out that after some 10^6
years a belt-like structure analogue to the main belt inside Jupiter in our
Solar System appears. We then proceed with giving the small bodies masses
(Moon-mass) and take into account the gravitational interaction between these
planetesimal-like objects. The growing of the objects – with certain percentage
of water – due to collisions is computed in order to look for the formation of
terrestrial planets. We observe that planets form in regions connected to mean
motion resonances (MMR). So far there is no observational evidence of
terrestrial planets in the system of HD 141399 but from our results we can
conclude that the formation of terrestrial planets – even with an appropriate
amount of water necessary for being habitable – in the HZ would have been
possible.
http://arxiv.org/icons/sfx.gif
