2019A&A...632A...6G


C.D.S. - SIMBAD4 rel 1.7 - 2021.06.20CEST21:06:16

2019A&A...632A...6G - Astronomy and Astrophysics, volume 632A, 6-6 (2019/12-0)

Rotational evolution of solar-type protostars during the star-disk interaction phase.

GALLET F., ZANNI C. and AMARD L.

Abstract (from CDS):


Context. The early pre-main sequence phase during which solar-mass stars are still likely surrounded by an accretion disk represents a puzzling stage of their rotational evolution. While solar-mass stars are accreting and contracting, they do not seem to spin up substantially.
Aims. It is usually assumed that the magnetospheric star-disk interaction tends to maintain the stellar rotation period constant ("disk-locking"), but this hypothesis has never been thoroughly verified. Our aim is to investigate the impact of the star-disk interaction mechanism on the stellar spin evolution during the accreting pre-main sequence phases.
Methods. We devised a model for the torques acting on the stellar envelope based on studies of stellar winds, and we developed a new prescription for the star-disk coupling founded on numerical simulations of star-disk interaction and magnetospheric ejections. We then used this torque model to follow the long-term evolution of the stellar rotation.
Results. Strong dipolar magnetic field components up to a few kG are required to extract enough angular momentum so as to keep the surface rotation rate of solar-type stars approximately constant for a few Myr. Furthermore an efficient enough spin-down torque can be provided by either one of the following: a stellar wind with a mass outflow rate corresponding to ~=10% of the accretion rate, or a lighter stellar wind combined with a disk that is truncated around the corotation radius entering a propeller regime.
Conclusions. Magnetospheric ejections and accretion powered stellar winds play an important role in the spin evolution of solar-type stars. However, kG dipolar magnetic fields are neither uncommon or ubiquitous. Besides, it is unclear how massive stellar winds can be powered while numerical models of the propeller regime display a strong variability that has no observational confirmation. Better observational statistics and more realistic models could contribute to help lessen our calculations' requirements.

Abstract Copyright: © F. Gallet et al. 2019

Journal keyword(s): stars: solar-type - stars: magnetic field - stars: evolution - stars: rotation - stars: winds - outflows

Simbad objects: 16

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Number of rows : 16

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NGC 869 OpC 02 19 00 +57 07.7           ~ 441 0
2 V* BP Tau Or* 04 19 15.8342975037 +29 06 26.929456808   13.13 12.12 11.89   K5/7Ve 619 0
3 V* AA Tau Or* 04 34 55.4222683130 +24 28 53.038273587 13.14 13.34 12.20     K5Ve 654 0
4 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2061 1
5 V* FU Ori Or* 05 45 22.3650208559 +09 04 12.296285806   10.72 9.60     F0Iab 739 1
6 NGC 2326 rG 07 08 11.0010077403 +50 40 54.842878046   14.3   11.88   ~ 26 0
7 NGC 2362 OpC 07 18 41 -24 57.3           ~ 366 0
8 Hen 3-545 Or* 10 59 06.9712894449 -77 01 40.309036535   12.91 11.136   9.596 K4Ve 193 0
9 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1634 1
10 V* CV Cha Or* 11 12 27.7052551478 -76 44 22.298597430   12.02 10.98 10.51 9.76 G9Ve 177 1
11 CD-35 10525 Or* 15 49 12.1055573607 -35 39 05.053991067 12.19 12.76 11.66 11.15   K7Ve 257 0
12 EM* SR 12 Or* 16 27 19.5054789229 -24 41 40.414828505     13.28 12.15 10.855 M0IVe 168 1
13 EM* SR 9 Or* 16 27 40.2858402419 -24 22 04.132012501   12.91 11.533 11.11 10.00 K5e 260 0
14 NGC 6530 OpC 18 04 31 -24 21.5           ~ 364 0
15 EM* AS 353 Or* 19 20 30.9919486938 +11 01 54.604157558   13.22 12.21     K5 184 1
16 NAME Ass Cep OB 3b As* 23 04.2 +63 24           ~ 22 0

    Equat.    Gal    SGal    Ecl

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2021.06.20-21:06:16

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