On the Luminosity of Young Jupiters

Abstract

Traditional thermal evolution models of giant planets employ arbitrary initial conditions selected more for computational expediency than physical accuracy. Since the initial conditions are eventually forgotten by the evolving planet, this approach is valid for mature planets, if not young ones. To explore the evolution at young ages of jovian mass planets we have employed model planets created by one implementation of the core accretion mechanism as initial conditions for evolutionary calculations. We find that young jovian planets are smaller, cooler, and several to 100 times less luminous than predicted by earlier models. Furthermore the time interval during which the young jupiters are fainter than expected depends on the mass of planet. Jupiter mass planets (1 M_J) align with the conventional model luminosity in as little at 20 million years, but 10 M_J planets can take up to 1 billion years to match commonly cited luminosities, given our implementation of the core accretion mechanism. If our assumptions, especially including our treatment of the accretion shock, are correct, then young jovian planets are substantially fainter at young ages than currently believed. These results have important consequences both for detection strategies and for assigning masses to young jovian planets based on observed luminosities.

20 pages, 6 figures, Astrophys. J. in press

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• Direct detection and spectral characterization of outer exoplanets with the SPICA coronagraph instrument (SCI)
• Photophoresis in the circumjovian disk and its impact on the orbital configuration of the Galilean satellites
• Protoplanetary disk insights from the first ERIS/APP survey at 4 μm
• Detecting planetary mass companions near the water frost-line using JWST interferometry
• Planetary Accretion Shocks with a Realistic Equation of State
• The paradox of youth for ALMA planet candidates
• Orbital Modeling of HII 1348B: An Eccentric Young Substellar Companion in the Pleiades
• An unusual reservoir of water emission in the VV CrA A protoplanetary disk
• An L+T Spectral Binary with Possible AB Doradus Kinematics
• Search for transiting exoplanets and variable stars in the open cluster NGC 7243
• ISPY -- NaCo Imaging Survey for Planets around Young stars. CenteR: the impact of centering and frame selection
• YOUNG Star detrending for Transiting Exoplanet Recovery (YOUNGSTER) II: Using Self-Organising Maps to explore young star variability in Sectors 1-13 of TESS data
• SAFARI I: A SPHERE discovery of a super metal-rich M dwarf companion to the star HD 86006
• An Imaging Search for Post-Main-Sequence Planets of Sirius B
• New Mid-Infrared Imaging Constraints on Companions and Protoplanetary Disks around six Young Stars
• Adapting a gas accretion scenario for migrating planets in FARGO3D
• The Sonora Brown Dwarf Atmosphere and Evolution Models I. Model Description and Application to Cloudless Atmospheres in Rainout Chemical Equilibrium
• How Internal Structure Shapes the Metallicity of Giant Exoplanets
• Detecting Exoplanets Using Eclipsing Binaries as Natural Starshades
• Semianalytical Accretion-Tracer Emission: Forming Planets Are Intrinsically Faint
• Stellar halo subtraction alternative for accreting companions' characterization with integral field spectroscopy: Analytical and on-sky demonstration on the PDS70, HTLup, and YSES1 systems
• Direct Imaging Discovery of Giant Exoplanet $\beta$ Pictoris d: A Decade-Long Game of Hide-and-Seek
• Adapting a solid accretion scenario for migrating planets in FARGO3D
• High-contrast imaging of tight resolved binaries with two vector vortex coronagraphs in cascade with the Palomar SDC instrument
• Hi-5: a potential high-contrast thermal near-infrared imager for the VLTI
• The Directly-Imaged Exoplanet Host Star 51 Eridani is a Gamma Doradus Pulsator
• Exoplanets through extreme optics: from PLATO to SHARK-NIR
• L-band Integral Field Spectroscopy of the HR 8799 Planetary System
• GPI 2.0: Exploring The Impact of Different Readout Modes on the Wavefront Sensor's EMCCD
• Rapid and Predictive Planet Population Synthesis Model (RAPPS) I. Upgraded model and resulting synthetic populations
• Stellar flare study of nearby young moving group members with TESS Data
• Searching for Embedded Protoplanets with the Keck/NIRC2 Vortex Coronagraph: Confirmation of a Core-accretion Planet in the Narrow Gap of the Elias 2-24 Disk
• TOI-3757 b: A low density gas giant orbiting a solar-metallicity M dwarf