2020A&A...638A.115H


Query : 2020A&A...638A.115H

2020A&A...638A.115H - Astronomy and Astrophysics, volume 638A, 115-115 (2020/6-1)

The CARMENES search for exoplanets around M dwarfs. The He I infrared triplet lines in PHOENIX models of M 2-3 V stars.

HINTZ D., FUHRMEISTER B., CZESLA S., SCHMITT J.H.M.M., SCHWEITZER A., NAGEL E., JOHNSON E.N., CABALLERO J.A., ZECHMEISTER M., JEFFERS S.V., REINERS A., RIBAS I., AMADO P.J., QUIRRENBACH A., ANGLADA-ESCUDE G., BAUER F.F., BEJAR V.J.S., CORTES-CONTRERAS M., DREIZLER S., GALADI-ENRIQUEZ D., GUENTHER E.W., HAUSCHILDT P.H., KAMINSKI A., KURSTER M., LAFARGA M., LOPEZ DEL FRESNO M., MONTES D. and MORALES J.C.

Abstract (from CDS):

The HeI infrared (IR) line at a vacuum wavelength of 10833Å is a diagnostic for the investigation of atmospheres of stars and planets orbiting them. For the first time, we study the behavior of the HeIIR line in a set of chromospheric models for M-dwarf stars, whose much denser chromospheres may favor collisions for the level population over photoionization and recombination, which are believed to be dominant in solar-type stars. For this purpose, we use published PHOENIX models for stars of spectral types M2 V and M3 V and also compute new series of models with different levels of activity following an ansatz developed for the case of the Sun. We perform a detailed analysis of the behavior of the HeIIR line within these models. We evaluate the line in relation to other chromospheric lines and also the influence of the extreme ultraviolet (EUV) radiation field. The analysis of the HeIIR line strengths as a function of the respective EUV radiation field strengths suggests that the mechanism of photoionization and recombination is necessary to form the line for inactive models, while collisions start to play a role in our most active models. Moreover, the published model set, which is optimized in the ranges of the NaI D2, Hα, and the bluest CaIIIR triplet line, gives an adequate prediction of the HeIIR line for most stars of the stellar sample. Because especially the most inactive stars with weak HeIIR lines are fit worst by our models, it seems that our assumption of a 100% filling factor of a single inactive component no longer holds for these stars.

Abstract Copyright: © ESO 2020

Journal keyword(s): stars: activity - stars: chromospheres - stars: late-type

Simbad objects: 50

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Number of rows : 50
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 Wolf 1056 PM* 00 38 59.0436387491 +30 36 58.387293197   12.60   10.6   M2.5V 82 0
2 Wolf 44 PM* 01 01 20.0490626127 +61 21 56.681939701   12.26 10.87     M2.0Ve 75 1
3 BD+70 68a * 01 01 29.6446211340 +71 41 02.410499669   11.39 10.28     ~ 4 0
4 G 3-14 PM* 01 43 20.1788090313 +04 19 17.962195740 13.64 12.45 10.915 9.879 8.614 M2V 130 0
5 G 244-47 PM* 02 01 35.3406953145 +63 46 11.995703079       10.630   M2.5Ve 57 0
6 V* VX Ari Er* 02 44 15.5094178798 +25 31 24.117029188 13.363 12.141 10.563 9.49 8.115 dM3 198 0
7 Ross 567 PM* 03 53 10.4353664994 +62 34 08.067755803       11.084   M3.0Ve 34 0
8 HD 285968 PM* 04 42 55.7753203198 +18 57 29.394344631 12.668 11.49 9.951 8.931 7.702 M2.5V 280 2
9 G 222-11 PM* 06 10 19.8463571757 +82 06 24.324656398   12.214   9.5   M2.5V 103 0
10 G 250-33 PM* 07 04 25.9411009163 +68 17 19.657102324     11.99 11.460   M3.0Ve 49 0
11 G 112-21 PM* 07 28 45.4390299123 -03 17 53.305913300 14.298 13.023 11.456 10.351 8.954 M3V 67 0
12 GJ 3452 PM* 07 35 21.8791845108 +54 50 58.972178689   12.93 11.325 10.868   M2.5Ve 47 0
13 G 234-57 ** 09 13 23.849448 +68 52 30.70416   12.767 11.168 10.760   M2.5V 34 0
14 L 678-39 PM* 09 36 01.6372518187 -21 39 38.878281901 13.647 12.48 10.906 9.858 8.577 M2.5V 115 0
15 G 236-1 PM* 09 42 34.8412757372 +70 02 01.965486742   11.86 10.58 9.53 8.24 M2.5V 82 0
16 MCC 573 PM* 10 16 45.9486115574 -11 57 42.403013223 13.559 12.464 10.998 9.953 8.624 dM3.0 79 0
17 G 162-70 PM* 10 35 01.1173228615 -09 24 38.577977895   13.66 12.110 11.02 9.63 dM3.0 22 0
18 G 55-35 PM* 10 39 40.5642980607 -06 55 25.501668469 13.939 12.79 11.281 10.244 8.961 dM2.5 71 0
19 Ross 104 PM* 11 00 04.2569699829 +22 49 58.646653116 12.826 11.584 10.020 8.952 7.646 M4V 157 0
20 LP 733-99 LM* 11 20 06.1044739405 -10 29 46.725680797   12.734 11.250 10.887   M2.0V 38 0
21 Ross 905 PM* 11 42 11.0933874353 +26 42 23.658083337   12.06 10.613 10.272 8.24 M3V 551 1
22 LP 733-71 PM* 11 46 42.9130951977 -14 00 51.781505601 14.331 13.19 11.700 10.639 9.287 M3V 70 0
23 Ross 690 PM* 12 23 00.1606524678 +64 01 50.963777117   13.23 13.481 10.9   M3V 62 0
24 Ross 695 PM* 12 24 52.5025942844 -18 14 32.249916666 13.954 12.863 11.272 10.243 8.991 dM2.0 107 0
25 * tau Boo B * 13 47 15.3324773299 +17 27 26.432463096     11.1     M3V 33 0
26 Ross 992 PM* 14 15 16.9799784942 +45 00 53.280496927       11.499   M3V 44 0
27 Ross 1047 PM* 15 09 35.5922330748 +03 10 00.551602913 14.131 12.986 11.473 10.405 9.052 M2V 65 0
28 G 152-50 PM* 15 47 24.5487998193 -10 53 47.266942275 14.179 12.88 11.279 10.213 8.907 M2.5V 52 1
29 G 137-84 PM* 16 09 16.2650052525 +09 21 07.544852145   11.5   11.398   M3.0V 21 0
30 V* EW Dra BY* 16 16 45.3148932337 +67 15 22.477858090   12.20   10.310   M3.0Ve 122 0
31 G 202-48 PM* 16 25 24.6233091302 +54 18 14.765751243   11.78 10.07 9.66   M1.5V 175 0
32 G 138-39 PM* 16 32 45.1913887678 +12 36 45.997723476 14.65 13.642 12.158 11.115 9.771 M3.0Ve 44 0
33 G 138-64 PM* 16 46 13.7425123184 +16 28 40.789650707 14.346 13.15 11.68 11.28 9.272 M3.0Ve 54 0
34 Ross 863 PM* 17 07 07.4898932675 +21 33 14.469160807 14.435 13.248 11.677 10.579 9.239 M3V 82 0
35 G 139-27 PM* 17 16 40.9809926333 +08 03 30.204061380 14.301 13.087 11.529 10.48 9.219 M2.5Ve 62 0
36 G 181-39 PM* 17 19 52.7126409684 +41 42 49.698739005   11.423   10.4   M2V 82 0
37 G 204-39 PM* 17 57 50.9662241511 +46 35 19.125367930   13.97 11.64 11.3   M2.5V 71 0
38 1SWASP J181725.16+482201.8 BY* 18 17 25.1255751303 +48 22 02.331325999   12.81 11.37 10.91   dM2.0 33 0
39 Ross 145 PM* 18 41 59.0356870572 +31 49 49.761626262   12.84 13.126 10.845   M2V 73 0
40 G 155-42 PM* 18 48 01.2690305953 -14 34 51.201707472   13.64 12.13 11.738   dM2.5 27 0
41 Ross 730 PM* 19 07 05.5652386812 +20 53 16.917224360 13.54 12.397 10.774 9.745 8.543 M2.0V 138 0
42 HD 349726 PM* 19 07 13.2038777698 +20 52 37.255872400 13.553 12.383 10.771 9.739 8.531 M2V 142 0
43 G 262-15 PM* 20 30 32.0455058633 +65 26 58.410103877   12.00   10.124   M3V 143 0
44 Wolf 896 PM* 20 56 46.5970399407 -10 26 54.749213101 14.112 12.999 11.487 10.428 9.106 dM2.5 90 0
45 Wolf 906 PM* 21 01 58.6409832639 -06 19 07.476988654 13.883 12.748 11.276 10.912 8.86 M2.5V 75 0
46 LSPM J2116+0234 PM* 21 16 27.2842864538 +02 34 51.390823638   13.4   11.639   M3.0Ve 25 0
47 BD-05 5715 PM* 22 09 40.3443754647 -04 38 26.651267098 13.006 11.868 10.366 9.279 7.877 M3.5V 244 1
48 Wolf 1014 PM* 22 12 35.9443794622 +08 33 11.599447209 14.713 13.545 11.982 10.913 9.581 M3.0Ve 56 0
49 BD-17 6785 PM* 23 38 08.1567743770 -16 14 10.202600605   12.830 11.288 11.079 9.08 M2V 43 0
50 Wolf 1051 PM* 23 58 32.6570994325 +07 39 30.124696331 14.382 13.258 11.739 10.654 9.277 M3.0Ve 51 0

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2021.11.30-20:26:35

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