2018MNRAS.476.3245J


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.16CET07:10:39

2018MNRAS.476.3245J - Mon. Not. R. Astron. Soc., 476, 3245-3262 (2018/May-3)

The inflated radii of M dwarfs in the Pleiades.

JACKSON R.J., DELIYANNIS C.P. and JEFFRIES R.D.

Abstract (from CDS):

Rotation periods obtained with the Kepler satellite have been combined with precise measurements of projected rotation velocity from the WIYN 3.5-m telescope to determine the distribution of projected radii for several hundred low-mass (0.1 <= M/M <= 0.8), fast-rotating members of the Pleiades cluster. A maximum likelihood modelling technique, that takes account of observational uncertainties, selection effects and censored data, and considers the effects of differential rotation and unresolved binarity, has been used to find that the average radius of these stars is 14 ± 2 per cent larger at a given luminosity than predicted by current evolutionary models of Dotter et al. and Baraffe et al. The same models are a reasonable match to the interferometric radii of older, magnetically inactive field M dwarfs, suggesting that the over-radius may be associated with the young, magnetically active nature of the Pleiades objects. No evidence is found for any change in this over-radius above and below the boundary marking the transition to full convection. Published evolutionary models that incorporate either the effects of magnetic inhibition of convection or the blocking of flux by dark star-spots do not individually explain the radius inflation, but a combination of the two effects might. The distribution of projected radii is consistent with the adopted hypothesis of a random spatial orientation of spin axes; strong alignments of the spin vectors into cones with an opening semi-angle <30° can be ruled out. Any plausible but weaker alignment would increase the inferred over-radius.

Abstract Copyright: © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): stars: activity - stars: evolution - stars: low-mass - stars: pre-main-sequence - open clusters and associations: general

Status in Simbad:  waiting for electronic table

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 - 2020
#notes
1 * p Eri B PM* 01 39 47.5649272123 -56 11 47.211206475   6.692 5.797     K2V 114 0
2 G 245-71 PM* 03 21 21.7794053122 +79 58 02.154836577       10.2   M2.0Ve 49 0
3 Cl Melotte 22 173 SB* 03 43 48.4129134344 +25 11 24.248383174   12.2 10.7     K0V 43 0
4 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 2917 0
5 2MASS J03474464+2342033 PM* 03 47 44.6492928857 +23 42 03.260193534     18.20   15.14 ~ 15 0
6 V* V338 Tau Fl* 03 47 59.7361155222 +24 43 52.745169615   14.71 13.51   12.00 K6e 57 0
7 Cl Melotte 22 2027 SB* 03 48 48.9543063501 +24 16 02.582849161   11.77 10.91   10.01 G2V 53 0
8 V* V548 Tau Fl* 03 49 01.0063753518 +22 58 49.499092944   16.94 15.39   13.23 ~ 23 0
9 V* V1283 Tau RS* 03 49 42.2767465069 +24 27 46.825343005   13.39 12.29 11.39 11.17 K3 49 0
10 BD+52 911 PM* 05 03 23.9014100324 +53 07 42.487841299   11.789 10.059 9.08 8.11 M0.5Ve 78 0
11 HD 34055 V* 05 14 36.9535345397 -00 33 46.218589070   8.321       M4III 25 0
12 HD 36395 PM* 05 31 27.3958475290 -03 40 38.021551815 10.626 9.443 7.968 6.996 5.913 M1.5Ve 420 0
13 V* YZ CMi BY* 07 44 40.1726285952 +03 33 08.877830321 13.761 12.831 11.225 9.958 8.263 M4.0Ve 771 0
14 NGC 2516 OpC 07 58 04 -60 45.2           ~ 576 0
15 Ass Vel OB 2 As* 08 09 22.478 -47 21 03.46           ~ 200 0
16 NGC 2547 OpC 08 09 52.360 -49 10 35.01           ~ 303 0
17 NGC 2632 OpC 08 40 24 +19 40.0           ~ 1184 0
18 V* V768 Cen LP* 14 48 38.0448178746 -36 38 04.901243442   7.37 6.01     M5III 31 0
19 * 41 Ara ** 17 19 03.83574 -46 38 10.4467 6.66 6.28 5.48 4.76 4.30 G8/K0V 165 0

    Equat.    Gal    SGal    Ecl

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2019.12.16-07:10:39

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