2021A&A...649A..96J


Query : 2021A&A...649A..96J

2021A&A...649A..96J - Astronomy and Astrophysics, volume 649A96-96 (2021/5-1)

The active lives of stars: A complete description of the rotation and XUV evolution of F, G, K, and M dwarfs.

JOHNSTONE C.P., BARTEL M. and GUDEL M.

Abstract (from CDS):


Aims. We study the evolution of the rotation and the high energy X-ray, extreme ultraviolet (EUV), and Ly-α emission for F, G, K, and M dwarfs, with masses between 0.1 and 1.2M☉, and provide a freely available set of evolutionary tracks for use in planetary atmosphere studies.
Methods. We develop a physical rotational evolution model constrained by observed rotation distributions in young stellar clusters. Using rotation, X-ray, EUV, and Ly-α measurements, we derive empirical relations for the dependences of high energy emission on stellar parameters. Our description of X-ray evolution is validated using measurements of X-ray distributions in young clusters.
Results. A star's X-ray, EUV, and Ly-α evolution is determined by its mass and initial rotation rate, with initial rotation being less important for lower mass stars. At all ages, solar mass stars are significantly more X-ray luminous than lower mass stars and stars that are born as rapid rotators remain highly active longer than those born as slow rotators. At all evolutionary stages, habitable zone planets receive higher X-ray and EUV fluxes when orbiting lower mass stars due to their longer evolutionary timescales. The rates of flares follow similar evolutionary trends with higher mass stars flaring more often than lower mass stars at all ages, though habitable zone planets are likely influenced by flares more when orbiting lower mass stars.
Conclusions. Our results show that single decay laws are insufficient to describe stellar activity evolution and highlight the need for a more comprehensive description based on the evolution of rotation that also includes the effects of short-term variability. Planets at similar orbital distances from their host stars receive significantly more X-ray and EUV energy over their lifetimes when orbiting higher mass stars. The common belief that M dwarfs are more X-ray and EUV active than G dwarfs is justified only when considering the fluxes received by planets with similar effective temperatures, such as those in the habitable zone.

Abstract Copyright: © ESO 2021

Journal keyword(s): stars: activity - stars: chromospheres - stars: coronae - stars: late-type - stars: magnetic field - stars: rotation

Simbad objects: 43

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Number of rows : 43
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 Cl Blanco 1 OpC 00 03 04.1 -29 48 55           ~ 380 0
2 G 272-61B PM* 01 39 01.6377185550 -17 57 01.001240728           M6V 892 0
3 NGC 752 OpC 01 56 53.7 +37 45 06           ~ 712 0
4 NGC 869 OpC 02 18 57.0 +57 08 02           ~ 504 0
5 HD 17925 RS* 02 52 32.1281856011 -12 46 10.968056223 7.48 6.91 6.05 5.34 4.89 K1V 557 0
6 * kap01 Cet BY* 03 19 21.6964175772 +03 22 12.714979884 5.71 5.52 4.85 4.27 3.91 G5V 948 0
7 * alf Per V* 03 24 19.3700924 +49 51 40.245455 2.64 2.27 1.79     F5Ib 870 1
8 Cl Melotte 22 OpC 03 46 38.0 +24 10 41           ~ 3679 0
9 Cl Melotte 25 OpC 04 30 27.4 +16 46 43           ~ 3309 0
10 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4971 0
11 V* AB Dor TT* 05 28 44.8712165880 -65 26 55.199147208 8.259 7.856 6.999 6.496 5.993 K0V 1080 0
12 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2514 0
13 M 37 OpC 05 52 18.6 +32 32 36           ~ 436 0
14 * chi01 Ori SB* 05 54 22.9829893 +20 16 34.222038 5.08 5.00 4.40 3.90 3.59 G0V 895 0
15 NGC 2168 OpC 06 09 07.5 +24 20 15           ~ 604 0
16 NGC 2323 OpC 07 02 47.3 -08 22 07           ~ 212 0
17 V* YY Gem SB* 07 34 37.4474327544 +31 52 10.179641496 11.60 10.56 9.27 7.69 6.67 M0.5VeFe-2 882 0
18 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1925 0
19 V* YZ CMi PM* 07 44 40.1723046464 +03 33 08.875227574 13.761 12.831 11.225 9.958 8.263 M4.0Ve 957 0
20 NGC 2516 OpC 07 58 00.5 -60 46 36           ~ 793 0
21 NGC 2547 OpC 08 10 01.5 -49 12 08           ~ 445 0
22 * pi.01 UMa BY* 08 39 11.7046112880 +65 01 15.263122512 6.33 6.26 5.64 5.12 4.79 G0.5V 608 0
23 NGC 2632 OpC 08 39 58.4 +19 36 33           ~ 1733 0
24 NGC 2682 OpC 08 51 23.5 +11 48 54           ~ 2528 0
25 V* AD Leo PM* 10 19 36.2808181226 +19 52 12.010446571   10.82 9.52 9.19   dM3 1469 1
26 V* RS CVn RS* 13 10 36.9077924448 +35 56 05.584994412 8.57 8.51 7.93 7.7   F6IV+G8IV 753 0
27 NAME Proxima Centauri PM* 14 29 42.9461331854 -62 40 46.164680672 14.21 12.95 11.13 9.45 7.41 M5.5Ve 1483 0
28 V* EK Dra BY* 14 39 00.2104038120 +64 17 29.979649860   8.243 7.604     G5VFe-0.7CH-1(k) 500 0
29 * alf Cen A SB* 14 39 36.49400 -60 50 02.3737 0.96 0.72 0.01     G2V 1352 1
30 * alf Cen ** 14 39 36.50 -60 50 02.3   0.4 -0.1     G2V+K1V 1031 0
31 * ksi Boo A PM* 14 51 23.3884659504 +19 06 01.619801424   5.40 4.675     G7Ve 564 0
32 * sig CrB A SB* 16 14 40.8534439608 +33 51 31.011629868   6.14 5.55     F6V 68 1
33 NGC 6475 OpC 17 53 44.1 -34 49 36           ~ 413 0
34 NGC 6530 OpC 18 04 31 -24 21.5           ~ 443 0
35 * 70 Oph A SB* 18 05 27.2484131991 +02 30 00.526614953       3.6   K0V 252 0
36 NGC 6540 GlC 18 06 08.60 -27 45 55.0           ~ 145 0
37 NGC 6811 OpC 19 37 21.8 +46 22 43   7.47 6.8     ~ 435 0
38 NGC 6819 OpC 19 41 18.3 +40 11 19   8.21 7.3     ~ 719 0
39 V* AT Mic Er* 20 41 51.15925 -32 26 06.8283 12.753 11.909 10.343 9.098 7.383 M4.5Ve+M4.5Ve 371 0
40 HD 197481 BY* 20 45 09.5324974119 -31 20 27.237889841   10.05 8.627 9.078 6.593 M1VeBa1 1344 0
41 HD 204961 PM* 21 33 33.9751191976 -49 00 32.399427028 11.359 10.176 8.672 7.665 6.479 M1.5V 336 1
42 V* EV Lac PM* 22 46 49.7312610268 +44 20 02.374381562   11.85 10.26 9.89   M4.0Ve 993 2
43 BD+19 5116 ** 23 31 52.17898 +19 56 14.1505 12.737 11.749 10.165 8.982 7.446 M3.5V 469 0

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