Orbital eccentricity growth through disc-companion tidal interaction

By J. Papaloizou, R. Nelson, F. Masset. 2001

206 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/f107f6d271f64bce5abde93c26132f9382fb6064

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In Astronomy and Astrophysics

1. C. Mordasini
2. A. Morbidelli
3. Y. Alibert
4. M. Perryman
5. Th. Henning
6. F. Rasio
7. S. Raymond
8. J. Winn

In Spectroscopy

1. C. Mordasini
2. Y. Alibert
3. Th. Henning
4. W. Kley
5. H. Klahr
6. M. Mayor
7. Eric B. Ford
8. F. Rasio

Citations in the corpus

• HD 80606 b, a planet on an extremely elongated orbit (2001, background): “However, a recent study (Papaloizou et al. 2001) suggests that for a standard disk model this can happen only for massive companions, at least in the range of brown dwarf masses.”
• Massive Black Hole Binary Evolution (2004, background): “These low-frequency components activate resonances located at larger radii than in the circular case, and might lead to mutual excitation and reinforcement of the binary and the disk eccentricities [162, 70].”
• Gas Flow across Gaps in Protoplanetary Disks (2005, background): “But accretion may still occur at higher planet masses, if the disk becomes eccentric as a consequence of a tidal instability (Papaloizou et al. 2001; Kley & Dirksen 2006; D’Angelo et al. 2005).”
• The primordial excitation and clearing of the asteroid belt—Revisited (2006, background): “…1996; Lubow et al., 1999) tend to form planets on circular orbits, and it is not clear that planet–disk interactions are capable of exciting the eccentricities and inclinations of Jupiter-and Saturn-mass planets (e.g., Papaloizou et al., 2001; D'Angelo et al., 2006; Kley and Dirksen, 2006).”
• HOW EMPTY ARE DISK GAPS OPENED BY GIANT PLANETS (2013, background): “For formal powerlaw fits, see the main text. outward transport of angular momentum by waves launched at the 1:3 outer eccentric Lindblad resonance pumps the eccentricity of the outer disk (Lubow 1991; Papaloizou et al. 2001).”
• THREE-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS OF CIRCUMBINARY ACCRETION DISKS: DISK STRUCTURES AND ANGULAR MOMENTUM TRANSPORT (2011, background): “Conversely, disk eccentricity might also excite eccentricity in the binary (e.g., Papaloizou et al. 2001).”
• Disk eccentricity and embedded planets (2005, background): “The good agreement of our results with theoretical expectations supports our conclusion that the mechanism for eccentri - ity growth is that described by Lubow (1991a) and Papaloizou et al. (2001).”
• Eccentricity Evolution for Planets in Gaseous Disks (2002, background): “In apparent contradiction with our conclusions, Papaloizou et al. (2001) did not obtain eccentricity growth for Jovian mass planets.”
• Origins of Eccentric Extrasolar Planets: Testing the Planet-Planet Scattering Model (2007, background): “…(Murrary et al. 1998), g) interactions with a gaseous proto-planetary disk (Goldreich & Tremaine 1980; Artymowicz 1992; Papaloizou & Larwood 2000; Papaloizou et al. 2001; Goldreich & Sari 2003; Ogilvie & Lubow 2003; Cresswell et al. 2007; Moorhead & Adams 2008), h) asymmetric stellar jets…”
• Characterization of exoplanets from their formation - II. The planetary mass-radius relationship (2012, background): “Such a situation arises if the eccentric instability (Papaloizou et al. 2001; Kley & Dirksen 2006) allows the planets to efficiently access disk material even after a gap has formed.”
• Spin-Orbit Evolution of Short-Period Planets (2004, background): “…resonant interactions would naturally damp the eccentricities of planets with masses Mp < 10MJ (where MJ is the mass of Jupiter; Goldreich & Tremaine 1980; Artymowicz 1992; Papaloizou et al. 2001), although in some circumstances, it may also excite planets’ eccentricities (Goldreich & Sari 2003).”
• Building the terrestrial planets: Constrained accretion in the inner Solar System (2009, background): “However, other studies have shown that eccentricity growth via planet-disk interactions can only occur for very massive, > 10MJup planets (Papaloizou et al., 2001; Kley and Dirksen, 2006).”
• Dynamics and Origin of the 2:1 Orbital Resonances of the GJ 876 Planets (2001, background): “In addition to its effect on the semi-major axis, planet-nebula interaction can also affect the orbital eccentricity of a planet (e.g., Goldreich & Tremaine 1980; Artymowicz 1992, 1993; Pa- paloizou et al. 2001).”
• Tidal Dissipation in Rotating Giant Planets (2003, background): “…with their natal disks (Lin et al. 1996), such a process may be able to damp the eccentricities of planets with masses MpP 10MJ (where MJ is the mass of Jupiter; Goldreich & Tremaine 1980; Artymowicz 1992), although this hypothesis remains uncertain (Papaloizou et al. 2001; Goldreich & Sari 2003).”