Context. TYC8241 2652 1 is a young star that showed a strong mid-infrared (mid-IR, 8-25 μm) excess in all observations before 2008, which is consistent with a dusty disk. Between 2008 and 2010 the mid-IR luminosity of this system dropped dramatically by at least a factor of 30 suggesting a loss of dust mass of an order of magnitude or more.
Aims: We aim to constrain possible models including the removal of disk material by stellar activity processes, the presence of a binary companion, or other explanations suggested in the literature.
Methods: We present new X-ray observations, optical spectroscopy, near-IR interferometry, and mid-IR photometry of this system to constrain its parameters and further explore the cause of the dust mass loss.
Results: In X-rays TYC8241 2652 1 has all the properties expected from a young star: Its luminosity is in the saturation regime and the abundance pattern shows enhancement of O/Fe. The photospheric Hα line is filled with a weak emission feature, indicating chromospheric activity that is consistent with the observed level of coronal emission. Interferometry does not detect a companion and sets upper limits on the companion mass of 0.2, 0.35, 0.1, and 0.05 M⊙ at projected physical separations of 0.1-4 AU, 4-5 AU, 5-10 AU, and 10-30 AU, respectively (assuming a distance of 120.9 pc). Our mid-IR measurements, the first of the system since 2012, are consistent with the depleted dust level seen after 2009.
Conclusions: The new data confirm that stellar activity is unlikely to destroy the dust in the disk and shows that scenarios, in which either TYC8241 2652 1 heats the disk of a binary companion or a potential companion heats the disk of TYC8241 2652 1, are unlikely.
Astronomy and Astrophysics
- Pub Date:
- February 2017
- stars: formation;
- stars: individual: TYC 8241 2652 1;
- stars: variables: general;
- Astrophysics - Solar and Stellar Astrophysics
- accepted by A&