2018A&A...615A..14F


C.D.S. - SIMBAD4 rel 1.7 - 2021.06.23CEST13:36:30

2018A&A...615A..14F - Astronomy and Astrophysics, volume 615A, 14-14 (2018/7-1)

The CARMENES search for exoplanets around M dwarfs. Wing asymmetries of Hα, Na I D, and He I lines.

FUHRMEISTER B., CZESLA S., SCHMITT J.H.M.M., JEFFERS S.V., CABALLERO J.A., ZECHMEISTER M., REINERS A., RIBAS I., AMADO P.J., QUIRRENBACH A., BEJAR V.J.S., GALADI-ENRIQUEZ D., GUENTHER E.W., KURSTER M., MONTES D. and SEIFERT W.

Abstract (from CDS):

Stellar activity is ubiquitously encountered in M dwarfs and often characterised by the Hα line.In the most active M dwarfs, Hα is found in emission, sometimes with a complex line profile. Previous studies have reported extended wings and asymmetries in the Hα line during flares. We used a total of 473 high-resolution spectra of 28 active M dwarfs obtained by the CARMENES (Calar Alto high-Resolution search for M dwarfs with Exo-Earths with Near-infrared and optical Echelle Spectrographs) spectrograph to study the occurrence of broadened and asymmetric Hα line profiles and their association with flares, and examine possible physical explanations. We detected a total of 41 flares and 67 broad, potentially asymmetric, wings in Hα. The broadened Hα lines display a variety of profiles with symmetric cases and both red and blue asymmetries. Although some of these line profiles are found during flares, the majority are at least not obviously associated with flaring. We propose a mechanism similar to coronal rain or chromospheric downward condensations as a cause for the observed red asymmetries; the symmetric cases may also be caused by Stark broadening. We suggest that blue asymmetries are associated with rising material, and our results are consistent with a prevalence of blue asymmetries during the flare onset. Besides the Hα asymmetries, we find some cases of additional line asymmetries in HeI D3, NaI D lines, and the HeI line at 10830Å taken all simultaneously thanks to the large wavelength coverage of CARMENES. Our study shows that asymmetric Hα lines are a rather common phenomenon in M dwarfs and need to be studied in more detail to obtain a better understanding of the atmospheric dynamics in these objects.

Abstract Copyright: © ESO 2018

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

Simbad objects: 38

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Number of rows : 38

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 CPD-86 426 * 00 03 29.0377251436 -86 15 22.751729283   10.94 10.68     A2 2 0
2 Wolf 47 Er* 01 03 19.8342607685 +62 21 55.831198996   15.34 13.21 12.4   M5V 170 0
3 V* YZ Cet Er* 01 12 30.6367741360 -16 59 56.361313690 15.315 13.885 12.074 10.696 8.938 M4.0Ve 214 0
4 LP 768-113 LM* 01 33 58.0014115870 -17 38 23.808061656   14.49 13.042 12.693 10.288 dM4.0 37 0
5 Barta 161 12 SB* 01 35 13.9238924192 -07 12 51.455163714   14.93 13.43 13.053 10.52 M4.3V 58 0
6 V* TZ Ari Er* 02 00 12.9561933930 +13 03 07.021294655 15.406 14.100 12.298 10.943 9.195 M4.5V 248 0
7 * omi02 Eri C Er* 04 15 21.5389590304 -07 39 20.718136574   12.85 11.17     M4.5V 194 0
8 V* V2689 Ori RS* 05 36 30.9904303980 +11 19 40.331999226 11.508 10.276 8.898 7.963 7.140 K6V 121 0
9 G 99-49 Er* 06 00 03.5038608130 +02 42 23.596778811   12.97 11.31 10.92 8.43 M3.5Ve 112 0
10 BD-02 2198 PM* 07 36 07.0798477777 -03 06 38.791356409 12.551 11.347 9.871 8.925 7.891 M1.0V 43 0
11 V* YZ CMi Er* 07 44 40.1726285952 +03 33 08.877830321 13.761 12.831 11.225 9.958 8.263 M4.0Ve 801 0
12 V* LQ Hya BY* 09 32 25.5684079124 -11 11 04.687410738 9.316 8.761 7.891 7.288 6.815 K1Vp 412 0
13 G 236-2 Er* 09 42 51.7280326717 +70 02 21.879144922       10.6   M3.5V 91 0
14 BD+20 2465 Er* 10 19 36.2808024653 +19 52 12.014037746   10.82 9.52 9.19   dM3 1188 0
15 Wolf 359 Er* 10 56 28.826208 +07 00 52.34400 16.706 15.541 13.507 11.684 9.507 dM6 644 0
16 V* DS Leo BY* 11 02 38.3419263291 +21 58 01.704479733 12.246 11.049 9.572 8.638 7.634 M1.0V 188 0
17 BD+44 2051B Er* 11 05 30.8856443432 +43 31 17.884318012   16.45 14.45 13.4   M6.0V 214 0
18 StKM 2-809 PM* 12 15 39.3673552228 +52 39 08.720024785     12.564 12.197   M4.0V 27 0
19 V* GL Vir Er* 12 18 59.3999178645 +11 07 33.770248089   15.68 13.90 13.55   M4.5Ve 146 0
20 NAME Proxima Centauri Er* 14 29 42.9451234609 -62 40 46.170818907 14.21 12.95 11.13 9.45 7.41 M5.5Ve 1046 0
21 V* OT Ser PM* 15 21 52.9325996324 +20 58 39.910979308 12.662 11.522 10.003 8.993 7.843 M1.0V 115 0
22 G 180-60 Er* 16 31 18.7890545317 +40 51 51.704950897   16.5   14.550   M6V 50 0
23 VB 8 Er* 16 55 35.2561420232 -08 23 40.752903617   18.7 16.916 14.566 12.24 M7Ve 396 0
24 NAME Barnard's star BY* 17 57 48.4997994034 +04 41 36.111354228 12.497 11.24 9.511 8.298 6.741 M4V 695 2
25 G 227-22 PM* 18 02 16.6046894779 +64 15 44.238912144   14.74   13.010   M5.0V 58 0
26 1SWASP J181725.16+482201.8 BY* 18 17 25.1255751303 +48 22 02.331325999   12.81 11.37 10.91   dM2.0 29 0
27 2MASSI J1835379+325954 PM* 18 35 37.8803560459 +32 59 53.311357837   20.0   17.1   M8.5V 106 0
28 Ross 149 PM* 18 36 19.2320093190 +13 36 26.372435490   13.8 12.46 12.112 9.69 M4V 49 0
29 G 141-36 PM* 18 48 17.5370354652 +07 41 21.177453364   15.6   13.817   M5.0V 31 0
30 2MASS J19064801+4011089 BD* 19 06 48.0750641777 +40 11 08.594820357           L1 24 0
31 VB 10 Er* 19 16 57.6103282334 +05 09 01.588675251     17.30     M8V 443 1
32 V* V374 Peg Er* 22 01 13.1233106147 +28 18 24.913041858       11.602   M3.5Ve 179 0
33 V* EV Lac Er* 22 46 49.7311740821 +44 20 02.372223230   11.85 10.26 9.89   M4.0V 819 2
34 V* GT Peg BY* 22 51 53.5351541240 +31 45 15.195567260       11.281   M3.5V 142 0
35 Ross 248 BY* 23 41 55.0361186415 +44 10 38.825189497   14.19   11.1   M5.0V 281 0
36 RX J2354.8+3831 PM* 23 54 51.4574111640 +38 31 36.200571993   14.78   12.94   M3.1V 34 0
37 HD 224085 RS* 23 55 04.0516465022 +28 38 01.248194500 8.88 8.20   6.9   K2+IVeFe-1 692 0
38 NAME Castor Moving Group As* ~ ~           ~ 117 1

    Equat.    Gal    SGal    Ecl

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2021.06.23-13:36:30

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