The post-disk (or primordial) spin distribution of M dwarf stars

Autor(en)

L. Gehrig, E. Gaidos, M. Güdel

Abstrakt

Context. The rotation periods of young low-mass stars after disks have dissipated (≲-pagination10 Myr) but before magnetized winds have removed significant angular momentum is an important launch point for gyrochronology and models of stellar rotational evolution; the rotation of these stars also regulates the magnetic activity and the intensity of high-energy emission that affects any close-in planets. A recent analysis of young M dwarf stars suggests a distribution of specific angular momentum (SAM) that is mass-independent, but the physical basis of this observation is unclear. Aims. We investigate the influence of an accretion disk on the angular momentum (AM) evolution of young M dwarfs, whose parameters govern the AM distribution after the disk phase, and whether this leads to a mass-independent distribution of SAM. Methods. We used a combination of protostellar spin and implicit hydrodynamic disk evolution models to model the innermost disk (∼0.01 AU), including a self-consistent calculation of the accretion rate onto the star, non-Keplerian disk rotation, and the influence of stellar magnetic torques over the entire disk lifetime. We executed and analyzed over 500 long-term simulations of the combined stellar and disk evolution. Results. We find that above an initial rate of crit ∼ 10-8 M_⊙ yr-1, accretion "erases" the initial SAM of M dwarfs during the disk lifetime, and stellar rotation converges to values of SAM that are largely independent of initial conditions. For stellar masses > 0.3 M_⊙, we find that observed initial accretion rates init are comparable to or exceed crit. Furthermore, stellar SAM after the disk phase scales with the stellar magnetic field strength as a power law with an exponent of -1.1. For lower stellar masses, init is predicted to be smaller than crit and the initial conditions are imprinted in the stellar SAM after the disk phase. Conclusions. To explain the observed mass-independent distribution of SAM, the stellar magnetic field strength has to range between 20 G and 500 G (700 G and 1500 G) for a 0.1 M_⊙ (0.6 M_⊙) star. These values match observed large-scale magnetic field measurements of young M dwarfs and the positive relation between stellar mass and magnetic field strength agrees with a theoretically motivated scaling relation. The scaling law between stellar SAM, mass, and the magnetic field strength is consistent for young stars, where these parameters are constrained by observations. Due to the very limited number of available data, we advocate for efforts to obtain more such measurements. Our results provide new constraints on the relation between stellar mass and magnetic field strength and they can be used as initial conditions for future stellar spin models, starting after the disk phase.

Organisation(en)

Institut für Astrophysik

Externe Organisation(en)

University of Hawaii at Manoa, Max-Planck-Institut für Astronomie

Journal

Astronomy and Astrophysics

Band

675

Anzahl der Seiten

16

ISSN

0004-6361

DOI

https://doi.org/10.1051/0004-6361/202243521

Publikationsdatum

07-2023

Peer-reviewed

Ja

ÖFOS 2012

103003 Astronomie, 103004 Astrophysik

Schlagwörter

ASJC Scopus Sachgebiete

Astronomy and Astrophysics, Space and Planetary Science

Link zum Portal

https://ucrisportal.univie.ac.at/de/publications/2184a8ea-9e2a-46fc-8226-cbeff66eb0e1