2020A&A...640A..52F


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.26CET14:47:45

2020A&A...640A..52F - Astronomy and Astrophysics, volume 640A, 52-52 (2020/8-1)

The CARMENES search for exoplanets around M dwarfs. Variability of the He I line at 10 830 Å.

FUHRMEISTER B., CZESLA S., HILDEBRANDT L., NAGEL E., SCHMITT J.H.M.M., JEFFERS S.V., CABALLERO J.A., HINTZ D., JOHNSON E.N., SCHOFER P., ZECHMEISTER M., REINERS A., RIBAS I., AMADO P.J., QUIRRENBACH A., NORTMANN L., BAUER F.F., BEJAR V.J.S., CORTES-CONTRERAS M., DREIZLER S., GALADI-ENRIQUEZ D., HATZES A.P., KAMINSKI A., KURSTER M., LAFARGA M. and MONTES D.

Abstract (from CDS):

The HeI infrared (IR) triplet at 10830Å is known as an activity indicator in solar-type stars and has become a primary diagnostic in exoplanetary transmission spectroscopy. HeIIR lines are a tracer of the stellar extreme-ultraviolet irradiation from the transition region and corona. We study the variability of the HeI triplet lines in a spectral time series of 319 M dwarf stars that was obtained with the CARMENES high-resolution optical and near-infrared spectrograph at Calar Alto. We detect HeIIR line variability in 18% of our sample stars, all of which show Hα in emission. Therefore, we find detectable HeI variability in 78% of the sub-sample of stars with Hα emission. Detectable variability is strongly concentrated in the latest spectral sub-types, where the HeI lines during quiescence are typically weak. The fraction of stars with detectable HeI variation remains lower than 10% for stars earlier than M3.0 V, while it exceeds 30% for the later spectral sub-types. Flares are accompanied by particularly pronounced line variations, including strongly broadened lines with red and blue asymmetries. However, we also find evidence for enhanced HeI absorption, which is potentially associated with increased high-energy irradiation levels at flare onset. Generally, HeI and Hα line variations tend to be correlated, with Hα being the most sensitive indicator in terms of pseudo-equivalent width variation. This makes the HeI triplet a favourable target for planetary transmission spectroscopy.

Abstract Copyright: © ESO 2020

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

VizieR on-line data: <Available at CDS (J/A+A/640/A52): table2.dat>

Status at CDS : Tables of objects will be appraised for possible ingestion in SIMBAD.

Simbad objects: 33

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Number of rows : 33

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 BD+44 4548 PM* 00 05 10.8891772602 +45 47 11.639549811   11.45   9.2   M2Ve 136 0
2 G 158-27 PM* 00 06 43.1972293497 -07 32 17.024270968     13.837 13.605 10.15 M5.5V 170 0
3 G 32-7 PM* 00 16 16.1530833228 +19 51 50.471455734   14.82   12.904   M4.0V 51 0
4 V* GX And Er* 00 18 22.8849667932 +44 01 22.637271919   10.120   7.3   M2V 453 0
5 V* GQ And Er* 00 18 25.8244484426 +44 01 38.091239561   12.84 11.04 10.3   M3.5Ve 239 0
6 G 31-53 PM* 00 28 39.4645836819 -06 39 49.181275245   13.71 12.23 11.885   M4.18 43 0
7 Wolf 1056 PM* 00 38 59.0436387491 +30 36 58.387293197   12.60   10.6   M2.5V 74 0
8 G 172-30 PM* 00 57 02.6919576431 +45 05 09.790903101   13.19 11.972 11.568   M3.0Ve 26 0
9 BD+61 195 PM* 01 02 38.8679928575 +62 20 42.172837073   11.439   8.7   M1.5V 196 0
10 Barta 161 12 SB* 01 35 13.9238924192 -07 12 51.455163714   14.93 13.43 13.053 10.52 M4.3V 54 0
11 UCAC4 563-005808 PM* 02 51 54.0991275318 +22 27 29.947610553   14.84 13.28 12.95   M4 16 0
12 G 80-21 PM* 03 47 23.3412010775 -01 58 19.945342289 14.052 13.048 11.537 10.452 9.098 M3.0V 85 0
13 Karmn J05084-210 * 05 08 27.2968097001 -21 01 44.376570148           M5 23 0
14 G 99-49 Er* 06 00 03.5038608130 +02 42 23.596778811   12.97 11.31 10.92 8.43 M3.5Ve 105 0
15 LP 205-44 Er* 06 31 50.7385796193 +41 29 45.482463701   16.50   14.462   M5.84 35 0
16 PM J06574+7405 PM* 06 57 26.1369 +74 05 26.447   14.56 13.01 12.677   M4.0V 14 0
17 UCAC3 281-106425 PM* 07 47 13.8681380950 +50 20 38.500016456   14.75 13.09 12.752   M4.0V 14 0
18 G 236-1 PM* 09 42 34.8412757372 +70 02 01.965486742   11.86 10.58 9.53 8.24 M2.5V 74 0
19 BD-09 3070 PM* 10 25 10.8370935977 -10 13 43.289558706 12.834 11.631 10.139 9.161 8.051 M1V 116 0
20 LP 733-99 PM* 11 20 06.1044739405 -10 29 46.725680797   12.734 11.250 10.887   M2.0V 23 0
21 UCAC4 784-022124 PM* 11 47 28.5644526434 +66 44 02.637494319     14.589 14.064   M5.0V 11 0
22 NAME Ursa Major Moving Group MGr 12 32 +57.0           ~ 383 2
23 NLTT 35712 PM* 13 53 38.7950523163 +77 37 08.150607952   14.4   12.525   M4.0V 21 0
24 NAME beta Pic Moving Group MGr 14 30 -42.0           ~ 574 0
25 V* OT Ser Ro* 15 21 52.9325996324 +20 58 39.910979308 12.662 11.522 10.003 8.993 7.843 M1.0V 109 0
26 G 207-19 PM* 19 08 29.9254500552 +32 16 51.610673872   13.46   11.371   M3V 39 0
27 HD 189733 BY* 20 00 43.7130382888 +22 42 39.071811263 9.241 8.578 7.648 7.126 6.68 K2V 730 1
28 HD 189733b Pl 20 00 43.7130382888 +22 42 39.071811263           ~ 1105 1
29 L 788-34 Er* 22 23 06.9970953617 -17 36 26.334021970   15.09 13.30 11.87 10.04 M4.5Ve 76 0
30 V* EV Lac Er* 22 46 49.7311740821 +44 20 02.372223230   11.85 10.26 9.89   M4.0V 804 2
31 V* GT Peg BY* 22 51 53.5351541240 +31 45 15.195567260       11.281   M3.5V 138 0
32 NAME Castor Moving Group As* ~ ~           ~ 117 1
33 NAME Pleiades Moving Group MGr ~ ~           ~ 241 1

    Equat.    Gal    SGal    Ecl

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2020.10.26-14:47:45

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