TY - JOUR
T1 - Roche-lobe Overflow in Eccentric Planet-Star Systems
AU - Dosopoulou, Fani
AU - Naoz, Smadar
AU - Kalogera, Vassiliki
N1 - Publisher Copyright:
© 2017. The American Astronomical Society. All rights reserved.
Copyright:
Copyright 2017 Elsevier B.V., All rights reserved.
PY - 2017/7/20
Y1 - 2017/7/20
N2 - Many giant exoplanets are found near their Roche limit and in mildly eccentric orbits. In this study, we examine the fate of such planets through Roche-lobe overflow as a function of the physical properties of the binary components, including the eccentricity and the asynchronicity of the rotating planet. We use a direct three-body integrator to compute the trajectories of the lost mass in the ballistic limit and investigate the possible outcomes. We find three different outcomes for the mass transferred through the Lagrangian point L 1: (1) self-accretion by the planet, (2) direct impact on the stellar surface, and (3) disk formation around the star. We explore the parameter space of the three different regimes and find that at low eccentricities, , mass overflow leads to disk formation for most systems, while, for higher eccentricities or retrograde orbits, self-accretion is the only possible outcome. We conclude that the assumption often made in previous work that when a planet overflows its Roche lobe it is quickly disrupted and accreted by the star is not always valid.
AB - Many giant exoplanets are found near their Roche limit and in mildly eccentric orbits. In this study, we examine the fate of such planets through Roche-lobe overflow as a function of the physical properties of the binary components, including the eccentricity and the asynchronicity of the rotating planet. We use a direct three-body integrator to compute the trajectories of the lost mass in the ballistic limit and investigate the possible outcomes. We find three different outcomes for the mass transferred through the Lagrangian point L 1: (1) self-accretion by the planet, (2) direct impact on the stellar surface, and (3) disk formation around the star. We explore the parameter space of the three different regimes and find that at low eccentricities, , mass overflow leads to disk formation for most systems, while, for higher eccentricities or retrograde orbits, self-accretion is the only possible outcome. We conclude that the assumption often made in previous work that when a planet overflows its Roche lobe it is quickly disrupted and accreted by the star is not always valid.
KW - binaries: close
KW - binaries: general
KW - planet-star interactions
KW - planetary systems
KW - planets and satellites: gaseous planets
KW - stars: kinematics and dynamics
UR - http://www.scopus.com/inward/record.url?scp=85026430076&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85026430076&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/aa7a05
DO - 10.3847/1538-4357/aa7a05
M3 - Article
AN - SCOPUS:85026430076
VL - 844
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
M1 - 12
ER -