1999ApJ...522.1053C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST07:17:23

1999ApJ...522.1053C - Astrophys. J., 522, 1053-1068 (1999/September-2)

Two-component theoretical chromosphere models for K dwarfs of different magnetic activity: exploring the Ca II emission-stellar rotation relationship.

CUNTZ M., RAMMACHER W., ULMSCHNEIDER P., MUSIELAK Z.E. and SAAR S.H.

Abstract (from CDS):

We compute two-component theoretical chromosphere models for K2 V stars with different levels of magnetic activity. The two components are a nonmagnetic component heated by acoustic waves and a magnetic component heated by longitudinal tube waves. The filling factor for the magnetic component is determined from an observational relationship between the measured magnetic area coverage and the stellar rotation period. We consider stellar rotation periods between 10 and 40 days. We investigate two different geometrical distributions of magnetic flux tubes: uniformly distributed tubes, and tubes arranged as a chromospheric network embedded in the nonmagnetic region. The chromosphere models are constructed by performing state-of-the-art calculations for the generation of acoustic and magnetic energy in stellar convection zones, the propagation and dissipation of this energy at the different atmospheric heights, and the formation of specific chromospheric emission lines that are then compared to the observational data. In all these steps, the two-component structure of stellar photospheres and chromospheres is fully taken into account. We find that heating and chromospheric emission is significantly increased in the magnetic component and is strongest in flux tubes that spread the least with height, expected to occur on rapidly rotating stars with high magnetic filling factors. For stars with very slow rotation, we are able to reproduce the basal flux limit of chromospheric emission previously identified with nonmagnetic regions. Most importantly, however, we find that the relationship between the Ca II H+K emission and the stellar rotation rate deduced from our models is consistent with the relationship given by observations.

Abstract Copyright:

Journal keyword(s): Line: Formation - Magnetohydrodynamics: MHD - Stars: Activity - Stars: Chromospheres - Stars: Late-Type - Stars: Rotation

Simbad objects: 14

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Number of rows : 14

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 * 54 Psc PM* 00 39 21.8055114029 +21 15 01.716052732 7.29 6.71 5.88 5.21 4.82 K0.5V 524 1
2 HD 4628 PM* 00 48 22.9763438736 +05 16 50.209562003 7.22 6.64 5.74 4.99 4.52 K2.5V 445 0
3 * 107 Psc PM* 01 42 29.7634932653 +20 16 06.660242064 6.57 6.08 5.24 4.55 4.12 K1V 505 0
4 HD 16160 PM* 02 36 04.9023844802 +06 53 12.431588708   6.81   5.2   K3V 484 1
5 HD 17925 RS* 02 52 32.1281853696 -12 46 10.970649463 7.48 6.91 6.05 5.34 4.89 K1V 470 0
6 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1697 1
7 HD 115404 PM* 13 16 51.0517063595 +17 01 01.840304856   7.69 6.66     K2V 254 0
8 * 12 Oph BY* 16 36 21.4492997704 -02 19 28.512485729 7.00 6.55 5.77 5.13 4.74 K1V 448 0
9 * 36 Oph A PM* 17 15 20.7837627960 -26 36 06.120125290   5.93 5.08     K2V 247 0
10 * 36 Oph B PM* 17 15 20.9846233161 -26 36 10.159381821   5.88 5.03     K1V 227 0
11 HD 160346 SB* 17 39 16.9163262 +03 33 18.875718   7.48   5.9   K3-V 269 0
12 * 70 Oph Ro* 18 05 27.28518 +02 30 00.3558 5.40 4.89 4.03 3.38 2.92 K0-V 607 0
13 HD 166620 PM* 18 09 37.4162810870 +38 27 27.995921559 7.86 7.27 6.40 5.63 5.14 K2V 391 0
14 * 94 Aqr B PM* 23 19 06.5608518922 -13 27 18.903718042         8.37 K2 68 1

    Equat.    Gal    SGal    Ecl

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2020.07.08-07:17:23

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