2017ApJ...850..134S


Query : 2017ApJ...850..134S

2017ApJ...850..134S - Astrophys. J., 850, 134-134 (2017/December-1)

M dwarf rotation from the K2 young clusters to the field. I. A mass-rotation correlation at 10 Myr.

SOMERS G., STAUFFER J., REBULL L., CODY A.M. and PINSONNEAULT M.

Abstract (from CDS):

Recent observations of the low-mass (0.1-0.6 M) rotation distributions of the Pleiades and Praesepe clusters have revealed a ubiquitous correlation between mass and rotation, such that late M dwarfs rotate an order-of-magnitude faster than early M dwarfs. In this paper, we demonstrate that this mass-rotation correlation is present in the 10 Myr Upper Scorpius association, as revealed by new K2 rotation measurements. Using rotational evolution models, we show that the low-mass rotation distribution of the 125 Myr Pleiades cluster can only be produced if it hosted an equally strong mass-rotation correlation at 10 Myr. This suggests that physical processes important in the early pre-main sequence (PMS; star formation, accretion, disk-locking) are primarily responsible for the M dwarf rotation morphology, and not quirks of later angular momentum (AM) evolution. Such early mass trends must be taken into account when constructing initial conditions for future studies of stellar rotation. Finally, we show that the average M star loses ∼25%-40% of its AM between 10 and 125 Myr, a figure accurately and generically predicted by modern solar-calibrated wind models. Their success rules out a lossless PMS and validates the extrapolation of magnetic wind laws designed for solar-type stars to the low-mass regime at early times.

Abstract Copyright: © 2017. The American Astronomical Society. All rights reserved.

Journal keyword(s): stars: evolution - stars: formation - stars: low-mass - stars: pre-main sequence - stars: rotation - stars: rotation

Simbad objects: 19

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Number of rows : 19
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 NGC 869 OpC 02 18 57.8 +57 08 02           ~ 472 0
2 Cl Melotte 22 OpC 03 46 24.2 +24 06 50           ~ 3411 0
3 Cl Melotte 25 OpC 04 29 47.3 +16 56 53           ~ 3050 0
4 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1353 0
5 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2311 0
6 NAME sig Ori Cluster OpC 05 38 42 -02 36.0           ~ 566 0
7 M 37 OpC 05 52 17.8 +32 32 42   6.19 5.6     ~ 397 2
8 NGC 2168 OpC 06 09 05.3 +24 20 10           ~ 551 0
9 NGC 2264 OpC 06 40 52.1 +09 52 37           ~ 1780 0
10 NGC 2362 OpC 07 18 41.0 -24 57 14           ~ 407 0
11 NGC 2516 OpC 07 58 06.5 -60 48 00           ~ 709 0
12 NGC 2547 OpC 08 09 52.360 -49 10 35.01           ~ 394 0
13 NGC 2632 OpC 08 40 13.0 +19 37 16           ~ 1546 0
14 NAME Upper Sco Association As* 16 12 -23.4           ~ 1359 1
15 NAME rho Oph Cluster Cl* 16 26 22 -24 23.7           ~ 70 0
16 NGC 6360 ? 17 25 30 -29 58.5           ~ 4 0
17 NGC 6791 OpC 19 20 53.0 +37 46 41   10.52 9.5     ~ 1030 0
18 NGC 6811 OpC 19 37 21.6 +46 22 41   7.47 6.8     ~ 372 0
19 NGC 6819 OpC 19 41 18.5 +40 11 24   8.21 7.3     ~ 618 0

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