The 21st Cambridge workshop on Cool Stars, Stellar Systems, and the Sun
Published November 22, 2022 | Version v1
Poster Open

Stellar Rotation of T Tauri stars in the Orion Star-Forming Complex

Authors/Creators

  • 1. Instituto de Astronomía, Universidad Autónoma de México, Ensenada, B.C., México
  • 2. Department of Physics and Astronomy, Vanderbilt University, VU Station 1807, Nashville, TN 37235, USA
  • 3. Departamento de Astronomía, Universidad de La Serena, 1700000 La Serena, Chile
  • 4. Observatorio Astronómico Nacional, Facultad de Ciencias, Universidad Nacional de Colombia, Bogotá, Colombia
  • 5. Department of Astronomy, University of Michigan, 1085 South University Avenue, Ann Arbor, MI 48109, USA
  • 6. Cerro Tololo Inter-American Observatory, Casilla 603, La Serena 1700000, Chile
  • 7. Department of Physics and Astronomy, The University of Western Ontario, 1151 Richmond Street, London, ON N6A 3K7, Canada
  • 8. Centro de Astronomía (CITEVA), Universidad de Antofagasta, Av. Angamos 601, Antofagasta, Chile
  • 9. Department of Physics and Astronomy, Western Washington University, 516 High Street, Bellingham, WA 98225, USA
  • 10. Centre for Astrophysics Research, School of Physics, Astronomy and Mathematics, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK
  • 11. Instituto de Astronomía, Universidad Católica del Norte, Av. Angamos 0610, Antofagasta, Chile

Contributors

Description

We present a large-scale study of stellar rotation for T Tauri stars in the Orion star-forming complex. We use the projected rotational velocity (v sin(i)) estimations reported by the APOGEE-2 collaboration as well as individual masses and ages derived from the position of the stars in the HR diagram, considering Gaia-EDR3 parallaxes and photometry plus diverse evolutionary models. We find an empirical trend for vsin(i) decreasing with age for low-mass stars (0.4Msun < M* < 1.2Msun). Our results support the existence of a mechanism linking vsin(i) to the presence of accreting protoplanetary disks, responsible for regulating stellar rotation on timescales of about 6 Myr, which is the timescale in which most of the T Tauri stars lose their inner disk. Our results provide significant constraints to models of rotation in the early phases of the evolution of young stars and their disks.

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Additional details

References

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