The Effect of Stellar Evolution on Migrating Warm Jupiters

@article{Frewen2015TheEO,
  title={The Effect of Stellar Evolution on Migrating Warm Jupiters},
  author={S. F. N. Frewen and Brad Hansen},
  journal={arXiv: Solar and Stellar Astrophysics},
  year={2015}
}
  • S. Frewen, B. Hansen
  • Published 21 October 2015
  • Geology, Physics
  • arXiv: Solar and Stellar Astrophysics
Warm jupiters are an unexpected population of extrasolar planets that are too near to their host to have formed in situ, but distant enough to retain a significant eccentricity in the face of tidal damping. These planets are curiously absent around stars larger than two solar radii. We hypothesize that the warm jupiters are migrating due to Kozai-Lidov oscillations, which leads to transient episodes of high eccentricity and a consequent tidal decay. As their host evolves, such planets would be… 

WARM JUPITERS FROM SECULAR PLANET–PLANET INTERACTIONS

Most warm Jupiters (gas-giant planets with 0.1 au ≲ a ≲ 1 au) have pericenter distances that are too large for significant orbital migration by tidal friction. We study the possibility that the warm

Dynamical constraints on the origin of hot and warm Jupiters with close friends

Gas giants orbiting their host star within the ice line are thought to have migrated to their current locations from farther out. Here we consider the origin and dynamical evolution of observed

Close-in planets around giant stars. Lack of hot-Jupiters and prevalence of multi-planetary systems

Extrasolar planets abound in almost any possible configuration. However, until five years ago, there was a lack of planets orbiting closer than 0.5 au to giant or subgiant stars. Since then, recent

A-type Stars, the Destroyers of Worlds: The Lives and Deaths of Jupiters in Evolving Stellar Binaries

Hot Jupiters (HJs), gas giant planets orbiting their host stars with periods on the order of days, commonly occur in the Galaxy, including relatively massive (1.6–2.4 M⊙, i.e., A-type main-sequence

THE ASTEROSEISMIC POTENTIAL of TESS: EXOPLANET-HOST STARS

New insights on stellar evolution and stellar interior physics are being made possible by asteroseismology. Throughout the course of the Kepler mission, asteroseismology has also played an important

The Eccentric Kozai-Lidov Effect and Its Applications

The hierarchical triple-body approximation has useful applications to a variety of systems from planetary and stellar scales to supermassive black holes. In this approximation, the energy of each

The Pan-Pacific Planet Search. VII. The Most Eccentric Planet Orbiting a Giant Star

Radial velocity observations from three instruments reveal the presence of a 4 MJup planet candidate orbiting the K giant HD 76920. HD 76920b has an orbital eccentricity of 0.856 ± 0.009, making it

Lithium Enrichment Signatures of Planetary Engulfment Events in Evolved Stars

Planetary engulfment events have long been proposed as a lithium (Li) enrichment mechanism contributing to the population of Li-rich giants (A(Li) ≥ 1.5 dex). Using MESA stellar models and A(Li)

Tracking Advanced Planetary Systems (TAPAS) with HARPS-N

Context. We present the current status of and new results from our search for exoplanets in a sample of solar-mass evolved stars observed with the HARPS-N and the 3.6 m Telescopio Nazionale Galileo

Quasi-secular evolution of mildly hierarchical triple systems: analytics and applications for GW sources and hot Jupiters

In hierarchical triple systems, the inner binary is perturbed by a distant companion. For large mutual inclinations, the Lidov-Kozai mechanism secularly excites large eccentricity and inclination

References

SHOWING 1-10 OF 58 REFERENCES

HOT JUPITERS AND COOL STARS

Close-in planets are in jeopardy, as their host stars evolve off the main sequence (MS) to the subgiant and red giant phases. In this paper, we explore the influences of the stellar mass (in the

Shrinking Binary and Planetary Orbits by Kozai Cycles with Tidal Friction

At least two arguments suggest that the orbits of a large fraction of binary stars and extrasolar planets shrank by 1-2 orders of magnitude after formation: (1) the physical radius of a star shrinks

EVIDENCE FOR THE TIDAL DESTRUCTION OF HOT JUPITERS BY SUBGIANT STARS

Tidal transfer of angular momentum is expected to cause hot Jupiters to spiral into their host stars. Although the timescale for orbital decay is very uncertain, it should be faster for systems with

THE PHOTOECCENTRIC EFFECT AND PROTO-HOT JUPITERS. III. A PAUCITY OF PROTO-HOT JUPITERS ON SUPER-ECCENTRIC ORBITS

Gas giant planets orbiting within 0.1 AU of their host stars are unlikely to have formed in situ and are evidence for planetary migration. It is debated whether the typical hot Jupiter smoothly

STEADY-STATE PLANET MIGRATION BY THE KOZAI–LIDOV MECHANISM IN STELLAR BINARIES

We study the steady-state orbital distributions of giant planets migrating through the combination of the Kozai–Lidov (KL) mechanism due to a stellar companion and friction due to tides raised on the

ON THE FORMATION OF HOT JUPITERS IN STELLAR BINARIES

We study the production of hot Jupiters (HJs) in stellar binaries. We show that the “eccentric Kozai–Lidov” (EKL) mechanism can play a key role in the dynamical evolution of a star–planet–star triple

Orbital migration of the planetary companion of 51 Pegasi to its present location

THE recent discovery1 and confirmation2 of a possible planetary companion orbiting the solar-type star 51 Pegasi represent a breakthrough in the search for extrasolar planetary systems. Analysis of

Gravitational scattering as a possible origin for giant planets at small stellar distances

TLDR
An alternative model for planetary migration that can account for two large orbital eccentricities of giant planets that are difficult to reconcile with a tidal-linkage model is described.

Tidal decay of close planetary orbits

The 4.2-day orbit of the newly discovered planet around 51~Pegasi is formally unstable to tidal dissipation. However, the orbital decay time in this system is longer than the main-sequence lifetime

HOT STARS WITH HOT JUPITERS HAVE HIGH OBLIQUITIES

We show that stars with transiting planets for which the stellar obliquity is large are preferentially hot (Teff > 6250 K). This could explain why small obliquities were observed in the earliest
...