Hot Jupiters accreting onto their parent stars: effects on the stellar activity
arXiv:2111.11110 · doi:10.1002/asna.20210096
Abstract
Hot Jupiters (HJs) are massive gaseous planets orbiting close to their host stars. Due to their physical characteristics and proximity to the central star, HJs are the natural laboratories to study the process of star-planet interaction (SPI). Phenomena related to SPI may include the inflation and the evaporation of planetary atmospheres, the formation of cometary tails and bow shocks and magnetospheric interaction between the magnetic field of the planet and that of the star. Several works suggest that some systems show enhanced stellar activity in phase with the planetary rotation period. In this work, we use a 3D magneto-hydrodynamic model that describes a system composed of a star and an HJ and that includes the corresponding planetary and stellar winds. The aim is to investigate whether the material evaporating from the planet interacts with the stellar extended corona, and generates observable features. Our simulation shows that, in some conditions, the planetary wind expands and propagates mainly along the planetary orbit. Moreover, part of the planetary wind collides with the stellar wind and a fraction of the planet's outflow is funnelled by the stellar magnetic field and hits the stellar surface. In both events, the material is heated up to temperatures of a few MK by a shock. These phenomena could manifest in the form of enhanced stellar activity at some orbital phases of the planet.
Accepted for publication in Astronomische Nachrichten - Astronomical Notes
References in corpus (10)
- Atmospheric Escape from Hot Jupiters
- Lyman- Transit Spectroscopy and the Neutral Hydrogen Tail of the Hot Neptune GJ436b
- Early UV Ingress in WASP-12b: Measuring Planetary Magnetic Fields
- Atmospheric escape from HD 189733b observed in HI Lyman-alpha: detailed analysis of HST/STIS September 2011 observations
- New observations of the extended hydrogen exosphere of the extrasolar planet HD209458b
- The Rotation Period of the Planet-Hosting Star HD 189733
- The shocking transit of WASP-12b: Modelling the observed early ingress in the near ultraviolet
- The corona of HD 189733 and its X-ray activity
- FUV variability of HD 189733. Is the star accreting material from its hot Jupiter?
- ROME (Radio Observations of Magnetized Exoplanets). II. HD 189733 Does Not Accrete Significant Material from its Exoplanet like a T Tauri Star from A Disk