2022A&A...657A.125F


Query : 2022A&A...657A.125F

2022A&A...657A.125F - Astronomy and Astrophysics, volume 657A, 125-125 (2022/1-1)

The CARMENES search for exoplanets around M dwarfs. Diagnostic capabilities of strong K I lines for photosphere and chromosphere.

FUHRMEISTER B., CZESLA S., NAGEL E., REINERS A., SCHMITT J.H.M.M., JEFFERS S.V., CABALLERO J.A., SHULYAK D., JOHNSON E.N., ZECHMEISTER M., MONTES D., LOPEZ-GALLIFA A., RIBAS I., QUIRRENBACH A., AMADO P.J., GALADI-ENRIQUEZ D., HATZES A.P., KURSTER M., DANIELSKI C., BEJAR V.J.S., KAMINSKI A., MORALES J.C. and ZAPATERO OSORIO M.R.

Abstract (from CDS):

There are several strong KI lines found in the spectra of M dwarfs, among them the doublet near 7700 Å and another doublet near 12500 Å. We study these optical and near-infrared doublets in a sample of 324 M dwarfs, observed with CARMENES, the high-resolution optical and near-infrared spectrograph at Calar Alto, and investigate how well the lines can be used as photospheric and chromospheric diagnostics. Both doublets have a dominant photospheric component in inactive stars and can be used as tracers of effective temperature and gravity. For variability studies using the optical doublet, we concentrate on the red line component because this is less prone to artefacts from telluric correction in individual spectra. The optical doublet lines are sensitive to activity, especially for M dwarfs later than M5.0 V where the lines develop an emission core. For earlier type M dwarfs, the red component of the optical doublet lines is also correlated with Hα activity. We usually find positive correlation for stars with Hα in emission, while early-type M stars with Hα in absorption show anti-correlation. During flares, the optical doublet lines can exhibit strong fill-in or emission cores for our latest spectral types. On the other hand, the near-infrared doublet lines very rarely show correlation or anti-correlation to Hα and do not change line shape significantly even during the strongest observed flares. Nevertheless, the near-infrared doublet lines show notable resolved Zeeman splitting for about 20 active stars which allows to estimate the magnetic fields B.

Abstract Copyright: © ESO 2022

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

VizieR on-line data: <Available at CDS (J/A+A/657/A125): table2.dat>

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

Simbad objects: 35

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Number of rows : 35
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 BD+44 4548 PM* 00 05 10.8891989003 +45 47 11.641457986   11.45   9.2   M2Ve 156 0
2 G 158-27 PM* 00 06 43.1973190107 -07 32 17.019101068     13.837 13.605 10.15 M5.5V 193 0
3 G 32-7 PM* 00 16 16.1530187091 +19 51 50.474211828   14.82   12.904   M4.0V 64 0
4 V* GX And Er* 00 18 22.8849799680 +44 01 22.637951588   10.120   7.3   M2V 511 0
5 V* GQ And Er* 00 18 25.8251408611 +44 01 38.092431857   12.84 11.04 10.3   M3.5V 270 0
6 G 31-53 PM* 00 28 39.4648750195 -06 39 49.179160254   13.71 12.23 11.885   dM4.0 56 0
7 Wolf 1056 PM* 00 38 59.0443396237 +30 36 58.387586417   12.60   10.6   M2.5V 91 0
8 G 172-30 PM* 00 57 02.6919355142 +45 05 09.788526472   13.19 11.972 11.568   M3.0V 39 0
9 Wolf 44 PM* 01 01 20.0492200601 +61 21 56.681648637   12.26 10.87     M2.0V 86 1
10 G 218-20 Er* 01 01 59.4949257485 +54 10 57.701837835   16.96   14.608   M5 32 0
11 G 268-110 PM* 01 04 53.8030982635 -18 07 28.625562071   16.34 14.47 14.81 10.97 dM5.0 52 0
12 V* YZ Cet Er* 01 12 30.6368826382 -16 59 56.358011559 15.315 13.885 12.074 10.696 8.938 M4.0Ve 244 0
13 LP 768-113 LM* 01 33 58.0018937952 -17 38 23.806416408   14.49 13.042 12.693 10.288 dM4.0 48 0
14 G 244-47 PM* 02 01 35.3407161312 +63 46 11.997406488       10.630   M2.5V 66 0
15 NAME Teegarden's Star LM* 02 53 00.8917932409 +16 52 52.632190137   17.21   14.1   dM6 141 0
16 HD 23453 Er* 03 46 20.1401305865 +26 12 55.820285692   11.05   9.237   M1V 123 0
17 G 7-4 PM* 03 47 20.8893274484 +08 41 47.092761989   16.38   14.233   M5V 35 0
18 G 109-35 PM* 06 59 28.8164986147 +19 20 55.857870053   16.78   10.6   M5.0Ve 72 0
19 PM J07001-1901 SB* 07 00 06.8330620992 -19 01 23.631397464     13.918 13.638   M5.0V 15 0
20 V* YZ CMi Er* 07 44 40.1723046464 +03 33 08.875227574 13.761 12.831 11.225 9.958 8.263 M4.0Ve 848 0
21 Ross 619 PM* 08 11 57.5691729379 +08 46 22.952885566   14.60 12.834 12.527   M4.5V 189 0
22 G 51-15 Er* 08 29 49.3527921926 +26 46 33.624143059   16.87   14.736   M6.5Ve 278 0
23 BD+20 2465 Er* 10 19 36.2808181226 +19 52 12.010446571   10.82 9.52 9.19   dM3 1262 0
24 Wolf 359 Er* 10 56 28.9208702274 +07 00 53.003285286 16.706 15.541 13.507 11.684 9.507 dM6 688 0
25 LP 731-76 PM* 10 58 27.9887062200 -10 46 30.497787012   16.20 14.50 14.175   M5.0V 37 0
26 WASP-31b Pl 11 17 45.3578468391 -19 03 17.216528280           ~ 115 1
27 PM J11474+6644 PM* 11 47 28.5708792648 +66 44 02.655237372     14.589 14.064   M5.0V 15 0
28 G 177-25 LM* 13 10 12.6292548340 +47 45 18.673788877   16.11   14.249   M5.0V 57 0
29 Ross 1020 PM* 13 22 56.7475808912 +24 28 03.598852682   14.55   12.577   M4V 64 0
30 NAME Proxima Centauri Er* 14 29 42.9461331854 -62 40 46.164680672 14.21 12.95 11.13 9.45 7.41 M5.5Ve 1190 0
31 Ross 154 Er* 18 49 49.3637762005 -23 50 10.447375350 13.528 12.19 10.43 10.23 7.703 M3.5Ve 361 0
32 VB 10 Er* 19 16 57.6109547886 +05 09 01.600923413     17.30     M8V 467 1
33 G 230-42 PM* 20 33 40.3194913707 +61 45 13.589938724   14.03   11.2   M4.0V 49 0
34 Ross 271 PM* 22 11 30.0941051758 +18 25 34.304669630 12.852 11.737 10.232 9.204 7.965 M2V 104 0
35 V* EV Lac Er* 22 46 49.7312610268 +44 20 02.374381562   11.85 10.26 9.89   M4.0Ve 865 2

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2023.01.27-19:10:02

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