Stellar X-Ray Variability and Planetary Evolution in the DS Tucanae System

doi:10.3847/1538-4357/ada948

Stellar X-Ray Variability and Planetary Evolution in the DS Tucanae System

2025-02-03

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Leonardo A. Dos Santos

DOI：10.3847/1538-4357/ada948

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We present an analysis of four Chandra observations of the 45 Myr old DS Tuc binary system. We observed X-ray variability of both stars on timescales from hours to months, including two strong X-ray flares from star A. The implied flaring rates are in agreement with past observations made with XMM-Newton, though these rates remain imprecise due to the relatively short total observation time. We find a clear, monotonic decline in the quiescent level of the star by a factor of 1.8 across 8 months, suggesting stellar variability that might be due to an activity cycle. If proven through future observations, DS Tuc A would be the youngest star for which a coronal activity cycle has been confirmed. The variation in our flux measurements across the four visits is also consistent with the scatter in empirical stellar X-ray relationships with Rossby number. In simulations of the possible evolution of the currently super-Neptune-sized planet DS Tuc A b, we find a range of scenarios for the planet once it reaches a typical field age of 5 Gyr, from Neptune size down to a completely stripped super-Earth. Improved constraints on the planet's mass in the future would significantly narrow these possibilities. We advocate for further Chandra observations to better constrain the variability of this important system.

Keywords:

POWERED MASS-LOSS

ACTIVITY-ROTATION RELATIONSHIP

RADIUS DISTRIBUTION

XMM-NEWTON

TESS HUNT

CONVECTIVE BOUNDARIES

ATMOSPHERIC LOSS

ACTIVITY CYCLE

SUPER-EARTHS

HOT JUPITER

Stellar X-Ray Variability and Planetary Evolution in the DS Tucanae System

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