2016A&A...595A..12S


Query : 2016A&A...595A..12S

2016A&A...595A..12S - Astronomy and Astrophysics, volume 595A, 12-12 (2016/11-1)

Magnetic cycles and rotation periods of late-type stars from photometric time series.

SUAREZ MASCARENO A., REBOLO R. and GONZALEZ HERNANDEZ J.I.

Abstract (from CDS):

Aims. We investigate the photometric modulation induced by magnetic activity cycles and study the relationship between rotation period and activity cycle(s) in late-type (FGKM) stars.
Methods. We analysed light curves, spanning up to nine years, of 125 nearby stars provided by the All Sky Automated Survey (ASAS). The sample is mainly composed of low-activity, main-sequence late-A to mid-M-type stars. We performed a search for short (days) and long-term (years) periodic variations in the photometry. We modelled the light curves with combinations of sinusoids to measure the properties of these periodic signals. To provide a better statistical interpretation of our results, we complement our new results with results from previous similar works.
Results. We have been able to measure long-term photometric cycles of 47 stars, out of which 39 have been derived with false alarm probabilities (FAP) of less than 0.1 per cent. Rotational modulation was also detected and rotational periods were measured in 36 stars. For 28 stars we have simultaneous measurements of activity cycles and rotational periods, 17 of which are M-type stars. We measured both photometric amplitudes and periods from sinusoidal fits. The measured cycle periods range from 2 to 14yr with photometric amplitudes in the range of 5-20 mmag. We found that the distribution of cycle lengths for the different spectral types is similar, as the mean cycle is 9.5yr for F-type stars, 6.7yr for G-type stars, 8.5yr for K-type stars, 6.0yr for early M-type stars, and 7.1yr for mid-M-type stars. On the other hand, the distribution of rotation periods is completely different, trending to longer periods for later type stars, from a mean rotation of 8.6 days for F-type stars to 85.4 days in mid-M-type stars. The amplitudes induced by magnetic cycles and rotation show a clear correlation. A trend of photometric amplitudes with rotation period is also outlined in the data. The amplitudes of the photometric variability induced by activity cycles of main-sequence GK stars are lower than those of early- and mid-M dwarfs for a given activity index. Using spectroscopic data, we also provide an update in the empirical relationship between the level of chromospheric activity as given by log10R 'HK and the rotation periods.

Abstract Copyright: © ESO, 2016

Journal keyword(s): stars: low-mass - stars: late-type - stars: rotation - stars: activity - techniques: photometric

Simbad objects: 55

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Number of rows : 55
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 HD 224789 PM* 00 00 40.3202289480 -69 40 33.474806652   9.12 8.24     K1V 68 0
2 HD 1320 PM* 00 17 16.5269419376 -43 51 09.835811318   8.63 7.98     G2V 79 0
3 HD 1388 PM* 00 17 58.8685975874 -13 27 20.307118533   7.09 6.50     G0V 110 0
4 HD 2071 PM* 00 24 42.5482773168 -53 59 02.393720124   7.95 7.27     G2V 82 0
5 V* YZ Cet Er* 01 12 30.6368826382 -16 59 56.358011559 15.315 13.885 12.074 10.696 8.938 M4.0Ve 236 0
6 HD 10180 * 01 37 53.5772394024 -60 30 41.482108548   7.95 7.32     G1V 176 2
7 HD 21019 PM* 03 23 17.7011620632 -07 47 38.755366656   6.92 6.23     G5/6V 131 0
8 V* V660 Tau Er* 03 48 28.0289494257 +23 18 02.731712608   13.66 12.60   11.43 K2V 87 0
9 V* V410 Tau Or* 04 18 31.1081296680 +28 27 16.155955728   12.13 10.75 8.45 9.408 K3Ve 444 0
10 HD 285968 PM* 04 42 55.7750207949 +18 57 29.395947044 12.668 11.49 9.951 8.931 7.702 M2.5V 297 2
11 HD 32147 PM* 05 00 48.9993452248 -05 45 13.224327192 8.27 7.27 6.21 5.36 4.87 K3+V 432 1
12 HD 36395 PM* 05 31 27.3957852161 -03 40 38.024004501 10.626 9.443 7.968 6.996 5.913 M1.5Ve 476 0
13 HD 42581 Er* 06 10 34.6149358167 -21 51 52.656352926 10.801 9.607 8.125 7.164 6.121 M1V 434 0
14 HD 45088 BY* 06 26 10.2546417144 +18 45 24.761018520 8.402 7.74   6.2   K2Ve 234 0
15 Ross 614 Er* 06 29 23.3915175239 -02 48 48.803911021 13.942 12.764 11.071 9.77 8.05 M4.5V 340 0
16 HD 260655 PM* 06 37 10.7988015297 +17 33 53.333221083 12.303 11.104 9.593 8.661 7.718 M0.0V 155 0
17 BD+05 1668 PM* 07 27 24.4989685603 +05 13 32.841491057 12.558 11.443 9.872 8.699 7.161 M3.5V 377 0
18 V* YZ CMi Er* 07 44 40.1723046464 +03 33 08.875227574 13.761 12.831 11.225 9.958 8.263 M4.0Ve 831 0
19 HD 63765 PM* 07 47 49.7198598818 -54 15 50.920919607   8.85 8.10     G9V 79 1
20 L 675-81 PM* 08 40 59.2057867166 -23 27 22.592748045   13.2 11.975 11.637 9.37 M3.5V 126 1
21 V* LQ Hya BY* 09 32 25.5683895648 -11 11 04.692242760 9.316 8.761 7.891 7.288 6.815 K1Vp 431 0
22 CD-40 5404 ** 09 39 46.3687964591 -41 04 03.204421513 13.395 12.215 10.694 9.617 8.231 M3V 104 0
23 V* AN Sex RS* 10 12 17.6682499584 -03 44 44.392042932 11.941 10.757 9.264 8.258 7.066 M2V 213 0
24 Wolf 359 Er* 10 56 28.9208702274 +07 00 53.003285286 16.706 15.541 13.507 11.684 9.507 dM6 678 0
25 Ross 104 PM* 11 00 04.2570074282 +22 49 58.645009946 12.826 11.584 10.020 8.952 7.646 M4V 162 0
26 Ross 128 Er* 11 47 44.3972681420 +00 48 16.400337591 14.223 12.905 11.153 9.859 8.184 dM4 381 0
27 HD 104067 PM* 11 59 10.0088449029 -20 21 13.612067116 9.683 8.897 7.921 7.369 6.913 K2V 111 1
28 CD-51 6859 PM* 12 37 52.2160953269 -52 00 05.322430607 13.397 12.198 10.663 9.586 8.233 M3V(e) 103 0
29 HD 113538 PM* 13 04 57.4765361506 -52 26 34.525896996 11.733 10.433 9.057 8.202 7.418 K9Vk: 72 1
30 BD+11 2576 PM* 13 29 59.7858994351 +10 22 37.784532575 11.728 10.524 9.029 8.07 7.013 M1.0V 225 0
31 HD 118100 Er* 13 34 43.2063495866 -08 20 31.338030204 11.578 10.552 9.372 8.602 7.930 K5Ve 335 0
32 HD 119850 Er* 13 45 43.7755597223 +14 53 29.471707437 10.989 9.894 8.50 7.465 6.363 M2V 323 0
33 HD 122303 PM* 14 01 03.1882316643 -02 39 17.519814662 12.343 11.177 9.707 8.745 7.66 M0V 144 0
34 HD 125595 PM* 14 21 23.1859553470 -40 23 38.220151339   10.13 9.03     K4Vk: 85 1
35 CD-45 9206 PM* 14 29 18.5643592920 -46 27 49.737783060 13.059 11.798 10.376 9.492 8.637 K7Vk 51 1
36 NAME Proxima Centauri Er* 14 29 42.9461331854 -62 40 46.164680672 14.21 12.95 11.13 9.45 7.41 M5.5Ve 1144 0
37 HD 131977 BY* 14 57 28.0007918772 -21 24 55.727265310 7.89 6.83 5.72 4.74 4.19 K4V 466 0
38 BD-07 4003 BY* 15 19 26.8269387505 -07 43 20.189497466 13.403 11.76 10.560 9.461 8.911 M3V 593 2
39 CD-40 9712 PM* 15 32 12.9323109019 -41 16 32.130433884 11.918 10.815 9.311 8.265 6.947 M2.5V 127 0
40 BD-12 4523 BY* 16 30 18.0583947383 -12 39 45.321217732 12.829 11.638 10.072 8.917 7.421 M3V 287 0
41 * 36 Oph B PM* 17 15 20.9838262152 -26 36 10.173444860   5.88 5.03     K1V 236 0
42 CD-46 11540 LM* 17 28 39.9455781571 -46 53 42.688095874 12.177 10.973 9.407 8.337 7.006 M3V 231 1
43 CD-51 10924 PM* 17 30 11.2044753442 -51 38 13.130309109 12.317 11.028 9.585 8.675 8.60 M0V 94 1
44 CD-48 11837 PM* 17 35 13.6172141343 -48 40 51.121402968 12.875 11.673 10.127 9.101 7.871 M1.5V 62 0
45 Ross 154 Er* 18 49 49.3637762005 -23 50 10.447375350 13.528 12.19 10.43 10.23 7.703 M3.5Ve 354 0
46 HD 176986 PM* 19 03 05.8729653768 -11 02 38.130757620   9.39 8.45     K2.5V 55 0
47 HD 180617 PM* 19 16 55.2565688720 +05 10 08.040554168 11.768 10.63 9.115 8.076 6.782 M3-V 387 0
48 V* AU Mic LM* 20 45 09.5324974119 -31 20 27.237889841   10.05 8.627 9.078 6.593 M1VeBa1 1012 0
49 LP 816-60 PM* 20 52 33.0166041464 -16 58 29.003281943 14.094 13.029 11.458 10.251 8.658 M4V 87 0
50 HD 204961 PM* 21 33 33.9751191976 -49 00 32.399427028 11.359 10.176 8.672 7.665 6.479 M2/3V 246 1
51 HD 209290 PM* 22 02 10.2750978279 +01 24 00.832158070 11.838 10.616 9.146 8.213 7.245 M0.5V 216 0
52 BD-05 5715 PM* 22 09 40.3443137051 -04 38 26.650757960 13.006 11.868 10.366 9.279 7.877 M3.5V 253 1
53 HD 215152 PM* 22 43 21.3028100652 -06 24 02.953048623   9.12 8.13 7.83 8.46 K3V 103 1
54 L 49-19 PM* 22 55 45.5127596213 -75 27 31.203633959 13.004 11.873 10.377 9.312 7.958 M3V 66 0
55 BD+19 5116A Er* 23 31 52.1738511880 +19 56 14.130398245   12.27 10.173 9.946   M3.5Ve 87 0

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2022.08.11-20:17:50

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