2010A&A...520A..52S


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.21CET11:38:38

2010A&A...520A..52S - Astronomy and Astrophysics, volume 520, A52-52 (2010/9-2)

Rotation and magnetic activity of the Hertzsprung-gap giant 31 Comae.

STRASSMEIER K.G., GRANZER T., KOPF M., WEBER M., KUEKER M., REEGEN P., RICE J.B., MATTHEWS J.M., KUSCHNIG R., ROWE J.F., GUENTHER D.B., MOFFAT A.F.J., RUCINSKI S.M., SASSELOV D. and WEISS W.W.

Abstract (from CDS):

The single rapidly-rotating G0 giant 31 Comae has been a puzzle because of the absence of photometric variability despite its strong chromospheric and coronal emissions. As a Hertzsprung-gap giant, it is expected to be at the stage of rearranging its moment of inertia, hence likely also its dynamo action, which could possibly be linked with its missing photospheric activity. Our aim is to detect photospheric activity, obtain the rotation period, and use it for a first Doppler image of the star's surface. Its morphology could be related to the evolutionary status. We carried out high-precision, white-light photometry with the MOST satellite, ground-based Stroemgren photometry with automated telescopes, and high-resolution optical echelle spectroscopy with the new STELLA robotic facility. The MOST data reveal, for the first time, light variations with a full amplitude of 5mmag and an average photometric period of 6.80±0.06 days. Radial-velocity variations with a full amplitude of 270m/s and a period of 1±2 days were detected from our STELLA spectra, which we also interpret as due to stellar rotation. The two-year constancy of the average radial velocity of +0.10±0.33km/s confirms the star's single status, as well as the membership in the cluster Melotte 111. A spectrum synthesis gives Teff=5660±42K, logg=3.51±0.09, and [Fe/H]=-0.15±0.03, which together with the revised Hipparcos distance, suggests a mass of 2.6±0.1M and an age of ≃540Myr. The surface lithium abundance is measured to be nearly primordial. A detection of a strong Hei absorption line indicates nonradiative heating processes in the atmosphere. Our Doppler images show a large, asymmetric polar spot, cooler than Teff by ≃1600K, and several small low-to-mid latitude features that are warmer by ≃300-400K and are possibly of chromospheric origin. We computed the convective turnover time for 31 Com as a function of depth and found on average τC≃5 days. 31 Com appears to be just at the onset of rapid magnetic braking and Li dilution because its age almost exactly coincides with the predicted onset of envelope convection. That we recover a big polar starspot despite the Rossby number being larger than unity, and thus no efficient (envelope) dynamo is expected, leads us to conclude that 31 Com still harbors a fossil predominantly poloidal magnetic field. However, the increasing convective envelope may have just started an interface dynamo that now is the source of the warm surface features and the corresponding UV and X-ray emission.

Abstract Copyright:

Journal keyword(s): stars: activity - stars: atmospheres - stars: individual: 31 Comae - starspots - stars: late-type - stars: rotation

VizieR on-line data: <Available at CDS (J/A+A/520/A52): table2.dat table3.dat>

Simbad objects: 22

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Number of rows : 22

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 * psi03 Psc * 01 09 49.2009931670 +19 39 30.269371143   6.263 5.562     F9IIIa 123 0
2 V* EK Eri BY* 04 20 38.6418116586 -06 14 45.579829233   7.036 6.154     K0III 109 0
3 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2731 0
4 * alf Tau LP? 04 35 55.23907 +16 30 33.4885 4.32 2.40 0.86 -0.37 -1.31 K5+III 1191 1
5 HD 282630 Or* 04 55 36.9698052301 +30 17 55.100440086   12.17 11.12 10.55   K0Ve 153 0
6 * alf Aur SB* 05 16 41.35871 +45 59 52.7693 1.33 0.88 0.08 -0.52 -0.96 G3III: 1142 0
7 * del Aur SB* 05 59 31.6184193950 +54 17 05.056666306 5.580 4.730 3.720 2.95 2.45 K0IIIb 180 0
8 * bet Gem PM* 07 45 18.94987 +28 01 34.3160 3.00 2.14 1.14 0.39 -0.11 K0IIIb 1058 1
9 * G CMi PM* 08 02 15.9365899 +02 20 04.452198 6.91 5.63 4.38 3.39 2.72 K2IIIbFe-0.5: 171 1
10 * 35 Cnc * 08 35 19.4461574183 +19 35 24.230780199   7.248 6.558     G0III 121 0
11 * eps Leo V* 09 45 51.0733004 +23 46 27.320834 4.23 3.79 2.98 2.36 1.93 G1IIIa 323 0
12 * c Vir PM* 12 20 20.9813348 +03 18 45.260365 7.27 6.12 4.96 4.07 3.46 K0.5IIIbFe-0.5 339 0
13 Cl Melotte 111 OpC 12 25 06.00 +26 06 00.0           ~ 416 0
14 * 30 Com ** 12 49 17.4513577175 +27 33 08.567319788 5.87 5.81 5.78   5.70 A1Van 77 0
15 * 31 Com Ro* 12 51 41.9190038520 +27 32 26.568320838 5.81 5.61 4.94 4.39 4.04 G0IIIp 412 1
16 HD 112152 * 12 54 06.6615935774 +27 40 33.800188758   9.23 9.05     A3V 33 0
17 * 41 Com PM* 13 07 10.7300255 +27 37 29.058512 8.14 6.22 4.69 3.64 2.83 K5-III 144 0
18 V* FK Com Ro* 13 30 46.7993742986 +24 13 57.786184235   9.04 8.245   7.204 G4III 350 1
19 V* V889 Her BY* 18 34 20.1030244573 +18 41 24.234582456   8.00 7.449   6.720 G2V 121 0
20 * bet Aqr * 21 31 33.5317148 -05 34 16.232006 4.27 3.71 2.89 2.29 1.84 G0Ib 433 0
21 * alf Aqr * 22 05 47.0359315 -00 19 11.456766 4.65 3.90 2.94 2.27 1.76 G2Ib 423 0
22 V* OU And Ro* 23 49 40.9598068715 +36 25 31.008222497   6.69 5.90     G1IIICaIIem 128 0

    Equat.    Gal    SGal    Ecl

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2021.01.21-11:38:39

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