490 research outputs found
I Care Not What Your Past May Be : I Love You Just The Same
https://digitalcommons.library.umaine.edu/mmb-vp/3564/thumbnail.jp
We Met, We Loved, We Parted
https://digitalcommons.library.umaine.edu/mmb-vp/2629/thumbnail.jp
While The Whole Damm Family Stuck Around
https://digitalcommons.library.umaine.edu/mmb-vp/5015/thumbnail.jp
I Am Always Building Castles In The Air
https://digitalcommons.library.umaine.edu/mmb-vp/1633/thumbnail.jp
Good Bye, Little Girl Of My Dreams
https://digitalcommons.library.umaine.edu/mmb-vp/1544/thumbnail.jp
I Am Always Building Castles In The Air
https://digitalcommons.library.umaine.edu/mmb-vp/1632/thumbnail.jp
Egyptian Moonlight : An Oriental Love Song
https://digitalcommons.library.umaine.edu/mmb-vp/1374/thumbnail.jp
Effects of Collisions with Rocky Planets on the Properties of Hot Jupiters
Observed Hot Jupiters exhibit a wide range of physical properties. For a
given mass, many planets have inflated radii, while others are surprisingly
compact and may harbor large central cores. Motivated by the observational
sample, this paper considers possible effects from collisions of smaller rocky
planets with gas giant planets. In this scenario, the Jovian planets migrate
first and enter into (approximately) 4 day orbits, whereas rocky planets (mass
= 0.1-20 that of Earth) migrate later and then encounter the gaseous giants.
Previous work indicates that the collision rates are high for such systems.
This paper calculates the trajectories of incoming rocky planets as they orbit
within the gaseous planets and are subjected to gravitational, frictional, and
tidal forces. These collisions always increase the metallicity of the Jovian
planets. If the incoming rocky bodies survive tidal destruction and reach the
central regions, they provide a means of producing large planetary cores. Both
the added metallicity and larger cores act to decrease the radii of the gas
giants at fixed mass. The energy released during these collisions provides the
Jovian planet with an additional heat source; here we determine the radial
layers where kinetic energy of the colliding body is dissipated, including the
energy remaining upon impact with the existing core. This process could have
long-term effects if the colliding body deposits significant energy deep in the
interior, in regions of high opacity. Both Hot Jupiters and newly formed gas
giants have inflated radii, large enough to allow incoming rocky planets to
survive tidal disruption, enhance the central core mass, and deposit
significant energy (in contrast, denser giant planets with the mass and radius
of Jupiter are expected to tidally destroy incoming rocky bodies).Comment: 35 pages, 11 figures, accepted to PAS
On The Sunset Trail
https://digitalcommons.library.umaine.edu/mmb-vp/5912/thumbnail.jp
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