Stellar Rotation of T Tauri stars in the Orion Star-Forming Complex
Creators
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Serna, Javier1
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Hernández, Jesús1
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Kounkel, Marina2
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Manzo-Martínez, Ezequiel1
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Roman-Lopes, Alexandre3
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Román-Zúñiga, Carlos G.1
- Batista, Maria Gracia4
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Pinzón, Giovanni4
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Calvet, Nuria5
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Briceño, Cesar6
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Tapia, Mauricio1
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Suárez, Genaro7
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Peña Ramírez, Karla8
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Stassun, Keivan G.2
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Covey, Kevin9
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Vargas-González, J.10
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Fernández-Trincado, José G.11
- 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
- Briceño, C. et al. (2019), AJ, 157, 85
- Hernández, J. et al. (2014), ApJ, 794, 36
- Gallet, F., & Bouvier, J. (2015), A&A, 577, A98
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