# XMM-Newton X-ray Observations of LkCa 15: A T Tauri Star With a Formative Planetary System

## TL;DR

This study uses deep XMM-Newton X-ray observations to analyze the young T Tauri star LkCa 15, revealing variable hot plasma components and assessing X-ray heating effects on its forming planetary system.

## Contribution

It provides new, detailed X-ray spectral data of LkCa 15, showing variability in plasma temperatures and evaluating the impact of X-ray irradiation on its protoplanets within the disk.

## Key findings

- X-ray emission shows two temperature components at ~0.4 keV and ~2.2 keV.
- The hot component temperature varies over time.
- X-ray heating of the inner disk and protoplanets is minimal at 15-20 AU.

## Abstract

High-resolution ground-based images of the T Tauri star LkCa 15 have revealed multiple companions that are thought to comprise a formative planetary system. The candidate protoplanets orbit at distances ~15 - 20 AU within the dust-depleted inner region of the circumstellar disk. Because of its young age (1 - 4 Myr), LkCa 15 provides a benchmark system for testing planet-formation models. We detected LkCa 15 as a bright X-ray source in a short 10 ks Chandra observation in 2009. We report here new results obtained from a deeper 37 ks XMM-Newton observation in 2014. The new data provide better sampling in the time domain and improved sensitivity at low energies below 1 keV. Spectral fits with thermal emission models require at least two temperature components at kT_cool ~ 0.4 keV and kT_hot ~ 2.2 keV. The value of kT_hot is about a factor of two less than inferred from Chandra, suggesting that the hot-component temperature is variable. The best-fit absorption column density is in good agreement with that expected from optical extinction estimates A_v = 1.3 - 1.7 mag. The intrinsic X-ray luminosity is L_x(0.2 - 10 keV) = 3e30 ergs/s. Estimates of the X-ray heating rate of the inner disk and protoplanets are sensitive to the assumed disk gas surface density for which recent ALMA observations give estimates Sigma_0(gas) ~ 100 g/cm^2 at 1 AU from the star. At such densities, X-ray heating is confined mainly to the upper disk layers and X-ray penetration through the disk midplane to the protoplanets at r ~ 15 - 20 AU is negligible.