The influence of the environment on the spin evolution of low-mass stars - I. External photoevaporation of circumstellar discs

• Verfasst von: Roquette, Julia [VerfasserIn]
• Verfasst von: Matt, S P [VerfasserIn]
• Verfasst von: Winter, Andrew J. [VerfasserIn]
• Verfasst von: Amard, L [VerfasserIn]
• Verfasst von: Stasevic, S [VerfasserIn]
• Titel: The influence of the environment on the spin evolution of low-mass stars - I. External photoevaporation of circumstellar discs
• Verf.angabe: J. Roquette, S.P. Matt, A.J. Winter, L. Amard and S. Stasevic
• E-Jahr: 2021
• Jahr: 02 October 2021
• Umfang: 20 S.
• Fussnoten: Gesehen am 17.12.2021
• Titel Quelle: Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
• Ort Quelle: Oxford : Oxford Univ. Press, 1827
• Jahr Quelle: 2021
• Band/Heft Quelle: 508(2021), 3, Seite 3710-3729
• ISSN Quelle: 1365-2966
• DOI: doi:10.1093/mnras/stab2772
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1782435344

Abstract

Massive stars are strong sources of far-ultraviolet radiation that can be hostile to the evolution of protoplanetary discs, driving mass-loss by external photoevaporation and shortening disc-dissipation time-scales. Their effect may also reduce the time-scale of angular momentum exchanges between the disc and host star during the early pre-main-sequence phase. To improve our understanding of the environmental influence on the rotational history of stars, we developed a model that considers the influence of the local far-ultraviolet radiation on the spin evolution of low mass stars. Our model includes an assumption of disc locking, which fixes the rotation rate during the star-disc-interaction phase, with the duration of this phase parametrized as a function of the local far-ultraviolet radiation and stellar mass (in the range of 0.1-1.3 M⊙). In this way, we demonstrate how the feedback from massive stars can significantly influence the spin evolution of stars and explain the mass dependence observed in period-mass distributions of young regions like Upper Sco and NGC 2264. The high far-ultraviolet environments of high-mass stars can skew the period distribution of surrounding stars towards fast-rotation, explaining the excess of fast-rotating stars in the open cluster h Per. The proposed link between rotation and the pre-main-sequence environment opens new avenues for interpreting the rotational distributions of young stars. For example, we suggest that stellar rotation may be used as a tracer for the primordial ultraviolet irradiation for stars up to ∼1 Gyr, which offers a potential method to connect mature planetary systems to their birth environment.