The spectroscopic signature of hot Jupiters in FU Orionis objects

Abstract

We show that if FU Orionis objects harbour hot Jupiters embedded in their discs, the resulting non-axisymmetric dissipation profile in the disc would be manifest as time-dependent distortions in the absorption line profiles of these objects. In order to affect the infrared line profiles, planets must lie within approximately 0.5 au of the central star, whereas only planets within 0.1 au would influence the optical line profiles. The timescale for modulation of the line profiles is relatively short (months) in each case, so that the effect could not have been discovered from published spectra (which combine data taken in different observing seasons). The detection of hot Jupiters in FU Orionis objects would be in line with the expectations of tidal migration theories (which predict a high incidence of close planets around young stars) and would also lend support to models which link the triggering of rapid rise FU Orionis events to the existence of a close massive planet.

MNRAS, in press

References in corpus (3)

• Three-dimensional Calculations of High and Low-mass Planets Embedded in Protoplanetary Discs
• Saturation of the corotation resonance in a gaseous disk
• Orbital migration and the frequency of giant planet formation

Cited by in corpus (8)

• Massive planets in FU Orionis discs: implications for thermal instability models
• The photometric evolution of FU Orionis objects: disc instability and wind-envelope interaction
• High-Resolution Near Infrared Spectroscopy of HD 100546: II. Analysis of variable rovibrational CO emission lines
• The Periodic Spectroscopic Variability of FU Orionis
• Detectability of giant planets in protoplanetary disks by CO emission lines
• Light curves of the latest FUor: Indication of a close binary
• Accretion discs, low-mass protostars and planets: probing the impact of magnetic fields on stellar formation
• The youngest of hot jupiters in action: episodic accretion outbursts in Gaia20eae