2015A&A...577A..98G


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST21:21:12

2015A&A...577A..98G - Astronomy and Astrophysics, volume 577A, 98-98 (2015/5-1)

Improved angular momentum evolution model for solar-like stars. II. Exploring the mass dependence.

GALLET F. and BOUVIER J.

Abstract (from CDS):

Understanding the physical processes that dictate the angular momentum evolution of solar-type stars from birth to maturity remains a challenge for stellar physics. We aim to account for the observed rotational evolution of low-mass stars over the age range from 1Myr to 10Gyr. We developed angular momentum evolution models for 0.5 and 0.8M stars. The parametric models include a new wind braking law based on recent numerical simulations of magnetised stellar winds, specific dynamo and mass-loss rate prescriptions, as well as core-envelope decoupling. We compare model predictions to the distributions of rotational periods measured for low-mass stars belonging to star-forming regions and young open clusters. Furthermore, we explore the mass dependence of model parameters by comparing these new models to the solar-mass models we developed earlier.Rotational evolution models are computed for slow, median, and fast rotators at each stellar mass. The models reproduce reasonably well the rotational behaviour of low-mass stars between 1Myr and 8-10Gyr, including pre-main sequence to zero-age main sequence spin up, prompt zero-age main sequence spin down, and early-main sequence convergence of the surface rotation rates. Fast rotators are found to have systematically shorter disk lifetimes than moderate and slow rotators, thus enabling dramatic pre-main sequence spin up. They also have shorter core-envelope coupling timescales, i.e., more uniform internal rotation. As for the mass dependence, lower mass stars require significantly longer core-envelope coupling timescales than solar-type stars, which results in strong differential rotation developing in the stellar interior on the early main sequence. Lower mass stars also require a weaker braking torque to account for their longer spin-down timescale on the early main sequence, while they ultimately converge towards lower rotational velocities than solar-type stars in the longer term because of their reduced moment of inertia. We also find evidence that the mass dependence of the wind braking efficiency may be related to a change in the magnetic topology in lower mass stars. We have included in parametric models the main physical processes that dictate the angular momentum evolution of low-mass stars. The models suggest that these processes are quite sensitive to both mass and instantaneous rotation rate. We have worked out and reported here the main trends of these mass and rotation dependencies, whose origin still have to be addressed through a detailed modelling of magnetised stellar winds, internal angular momentum transport processes, and protoplanetary disk dissipation mechanisms.

Abstract Copyright:

Journal keyword(s): stars: evolution - stars: solar-type - stars: low-mass - stars: rotation - stars: mass-loss - stars: magnetic field

CDS comments: Star #3245 not identified.

Simbad objects: 40

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Number of rows : 40

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 869 OpC 02 19 00 +57 07.7           ~ 426 0
2 [MAB2013] 494 * 02 20 03.176 +57 11 44.68     20.4603   17.9348 ~ 2 0
3 NGC 1039 OpC 02 42 05 +42 45.7           ~ 370 0
4 Cl Melotte 20 OpC 03 26 42 +48 48.0           ~ 750 0
5 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 2978 0
6 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2654 0
7 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 1977 1
8 2MASS J05361500-0531567 V* 05 36 15.0064408261 -05 31 56.845145266         19.383 ~ 5 0
9 M 37 OpC 05 52 18 +32 33.2   6.19 5.6     ~ 332 2
10 NGC 2168 OpC 06 08 54 +24 20.0           ~ 457 0
11 NGC 2264 OpC 06 40 58 +09 53.7     3.9     ~ 1587 1
12 [IAB2009] M50-3-464 * 07 01 39.03 -08 22 55.2     17.611     ~ 1 0
13 [IAB2009] M50-3-1468 * 07 01 49.26 -08 20 18.8     16.908     ~ 1 0
14 [IAB2009] M50-4-2077 * 07 01 55.89 -08 13 16.5     17.328     ~ 1 0
15 [IAB2009] M50-3-2531 * 07 02 01.02 -08 20 09.1     17.563     ~ 1 0
16 [IAB2009] M50-4-4939 * 07 02 21.55 -08 09 25.8     17.477     ~ 1 0
17 [IAB2009] M50-3-5840 * 07 02 33.30 -08 20 20.4     15.764     ~ 1 0
18 NGC 2323 OpC 07 02 47.5 -08 20 16           ~ 154 0
19 [IAB2009] M50-3-7334 * 07 02 47.58 -08 19 23.6     15.861     ~ 1 0
20 [IAB2009] M50-6-1574 * 07 03 02.54 -08 32 16.4     17.030     ~ 1 0
21 [IAB2009] M50-5-1624 * 07 03 03.59 -08 39 17.3     16.838     ~ 1 0
22 [IAB2009] M50-5-2673 * 07 03 11.71 -08 40 32.8     17.181     ~ 1 0
23 [IAB2009] M50-7-5624 * 07 03 31.44 -08 20 26.0     16.297     ~ 1 0
24 [IAB2009] M50-7-7623 * 07 03 55.94 -08 15 10.0     15.737     ~ 1 0
25 [BNM2013] 68.04 1456 * 07 18 15.5906379682 -25 00 46.435202961 21.678   20.01     ~ 2 0
26 NGC 2362 OpC 07 18 41 -24 57.3     4.1     ~ 361 0
27 [IHA2008b] N2362-5-4947 * 07 19 20.59 -25 10 55.4     20.62     ~ 1 0
28 NGC 2516 OpC 07 58 04 -60 45.2           ~ 587 0
29 NGC 2547 OpC 08 09 52.360 -49 10 35.01           ~ 310 0
30 Cl* NGC 2632 S 14 Ro* 08 37 22.2266583174 +20 10 37.238283429   12.077 11.378     G 29 0
31 Cl* NGC 2632 JC 187 Pu* 08 40 05.7147090719 +19 01 30.667177497   13.720 12.706 12.150   K1V 29 0
32 NGC 2632 OpC 08 40 24 +19 40.0           ~ 1224 0
33 IC 2391 OpC 08 40 32 -53 02.0           ~ 714 0
34 Cl* NGC 2632 JS 634 * 08 46 38.2189781268 +19 52 44.843837994   18.85 16.37     M2.5 10 0
35 [BNM2013] 7.04 780 * 18 04 06.4987006924 -24 17 41.240439780 19.871 19.233 17.948   16.261 ~ 6 0
36 NGC 6530 OpC 18 04 31 -24 21.5   4.74 4.6     ~ 347 1
37 KIC 8366239 RG* 19 28 19.0902589679 +44 19 18.594810144   13.35 11.71     G6V 39 0
38 NGC 6811 OpC 19 37 17 +46 23.3   7.47 6.8     ~ 250 0
39 NGC 6819 OpC 19 41 18 +40 11.2   8.21 7.3     ~ 465 0
40 Ass Cep OB 3b As* 23 04.2 +63 24           ~ 19 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-21:21:12

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