2005ApJ...632.1104L


Query : 2005ApJ...632.1104L

2005ApJ...632.1104L - Astrophys. J., 632, 1104-1112 (2005/October-3)

Predicting the length of magnetic cycles in late-type stars.

LORENTE R. and MONTESINOS B.

Abstract (from CDS):

In this paper we present a modification of a local approximation of the so-called interface dynamo in an attempt to reproduce the length of the magnetic cycles for a sample of late-type stars. The sample consists of 25 stars, observed during the Mount Wilson and Las Campanas long-term monitoring campaigns, for which well-defined cycles have been detected. We have focused our efforts on reproducing general trends observed, namely, the dependence of the cycle length, Pcyc, on the stellar rotation period, Prot, rather than attempting to infer from the dynamo model individual cycle lengths for each star. In spite of the simplicity of the model, the results are promising. The trend of increasing cycle length with increasing rotation period is reproduced with a minimum of assumptions.

Abstract Copyright:

Journal keyword(s): Stars: Activity - Stars: Late-Type - Stars: Magnetic Fields - Stars: Rotation

Simbad objects: 25

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Number of rows : 25
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 * 9 Cet BY* 00 22 51.7883318927 -12 12 33.972374893 7.29 7.05 6.39     G2.5V 459 0
2 * 54 Psc PM* 00 39 21.8055114029 +21 15 01.716052732 7.29 6.71 5.88 5.21 4.82 K0.5V 544 1
3 HD 4628 PM* 00 48 22.9763438736 +05 16 50.209562003 7.22 6.64 5.74 4.99 4.52 K2.5V 465 0
4 * 107 Psc PM* 01 42 29.7634932653 +20 16 06.660242064 6.57 6.08 5.24 4.55 4.12 K1V 519 0
5 HD 16160 PM* 02 36 04.9023844802 +06 53 12.431588708   6.81   5.2   K3V 500 1
6 * kap01 Cet BY* 03 19 21.6963205 +03 22 12.715139 5.71 5.52 4.85 4.27 3.91 G5V 836 0
7 * omi02 Eri Er* 04 15 16.3197260 -07 39 10.338087 5.69 5.25 4.43 3.74 3.29 K0V 761 0
8 HD 32147 PM* 05 00 48.9991346145 -05 45 13.220341956 8.27 7.27 6.21 5.36 4.87 K3+V 425 1
9 HD 76151 PM* 08 54 17.9469808897 -05 26 04.046487788 6.89 6.67 6.00     G2V 485 0
10 HD 78366 PM* 09 08 51.0705427688 +33 52 55.988119240   6.53   5.6   G0IV-V 224 0
11 HD 81809 SB* 09 27 46.77993 -06 04 16.2822   6.02 5.40     G1.5IV-V 281 0
12 * 88 Leo ** 11 31 44.9446108040 +14 21 52.213131158   6.77   5.9   F9.5V 178 0
13 HD 103095 PM* 11 52 58.7683801554 +37 43 07.240082865 7.38 7.20 6.45 5.80 5.35 K1V_Fe-1.5 757 1
14 * bet Com PM* 13 11 52.3937856 +27 52 41.453553 4.92 4.84 4.25 3.77 3.47 F9.5V 859 0
15 HD 115404 PM* 13 16 51.0517063595 +17 01 01.840304856   7.69 6.66     K2V 260 0
16 * 12 Oph BY* 16 36 21.4492997704 -02 19 28.512485729 7.00 6.55 5.77 5.13 4.74 K1V 457 0
17 HD 152391 PM* 16 52 58.8025427362 -00 01 35.116299669   7.40 6.64     G8.5Vk: 343 0
18 V* V2215 Oph RS* 17 16 13.3627374963 -26 32 46.133091527   7.50 6.34   4.8 K5V 284 0
19 HD 160346 SB* 17 39 16.9163262 +03 33 18.875718   7.496 6.525 5.9   K3-V 278 0
20 * 70 Oph A SB* 18 05 27.370543 +02 29 59.31669       3.6   K0V 211 0
21 HD 166620 PM* 18 09 37.4162810870 +38 27 27.995921559 7.86 7.27 6.40 5.63 5.14 K2V 401 0
22 * 15 Sge PM* 20 04 06.2209062328 +17 04 12.677429047   6.390 5.788 5.4   G0V 349 0
23 * 61 Cyg A BY* 21 06 53.9396100677 +38 44 57.897024357 7.50 6.39 5.21 4.19 3.54 K5V 972 0
24 * 61 Cyg B Er* 21 06 55.2640651855 +38 44 31.362140913 8.63 7.40 6.03 4.86 3.55 K7V 682 1
25 * 94 Aqr B PM* 23 19 06.5608518922 -13 27 18.903718042         8.37 K2 73 1

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2021.09.21-06:47:28

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