2009A&A...503..929H


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST00:17:31

2009A&A...503..929H - Astronomy and Astrophysics, volume 503, 929-944 (2009/9-1)

Observation and modelling of main sequence star chromospheres. VIII. High resolution observations of M and K dwarf chromospheric lines.

HOUDEBINE E.R., JUNGHANS K., HEANUE M.C. and ANDREWS A.D.

Abstract (from CDS):

We report on high resolution observations of chromospheric lines for M and K dwarfs. We observed up to 13 spectral lines per star: the Hα, Hβ, Hε, Paε, Pa8, CaII H, CaII IR triplet, CaI 6572Å, NaI D1/D2 and HeI D3 lines. We observed two dMe stars, one dM(e) star, 5 dM stars and 3 dK stars. We observed a self-reversal in the emission core of the CaII H line for the brightest stars only, indicating a rather optically thick region of formation. We present original spectra of the NaI doublet and the CaII IR triplet for active dMe stars and less active dM stars. Core emission is detected in the Sodium lines and the CaII IR triplet lines for the most active M dwarf AU Mic. We investigate the difference spectra between active dMe stars and dM stars and show that these provide interesting new constraints for the NLTE-radiation transfer modelling of the chromospheres. In our sample, emission Hα profiles have a rather homogeneous FWHM of about 1.5Å. This, according to our previous modelling, can be interpreted as the signature of a rather constant temperature break in the chromosphere. We found that one of our targets (MCC 332) is a binary with a faint but active Hα emission component. For the first time we detect the Paε line for six dwarfs. It appears as weak absorption with possible weak wing emission in AU Mic. The region of the Pa8 line was observed but the line was not detected.

Abstract Copyright:

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

Simbad objects: 22

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Number of rows : 22

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 HD 8946 * 01 29 19.1609487952 +54 21 31.370762790   8.86 8.69     A0 4 0
2 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1697 1
3 V* V1005 Ori BY* 04 59 34.8341800543 +01 47 00.672080375   11.48 10.107 9.603 8.239 M0Ve 301 0
4 HD 36395 PM* 05 31 27.3958475290 -03 40 38.021551815 10.626 9.443 7.968 6.996 5.913 M1.5Ve 428 0
5 BD+20 2465 Er* 10 19 36.2808024653 +19 52 12.014037746   10.82 9.52 9.19   M4Vae 1146 0
6 HD 111631 PM* 12 50 43.5668069413 -00 46 05.267056898 11.187 9.892 8.470 7.59 6.752 M0V 200 0
7 HD 118100 Er* 13 34 43.2063348511 -08 20 31.335294003 11.578 10.552 9.372 8.602 7.930 K5Ve 324 0
8 HD 119850 Fl* 13 45 43.7754528655 +14 53 29.473195472 10.989 9.894 8.50 7.465 6.363 M2V 289 0
9 CD-40 9712 PM* 15 32 12.9326267337 -41 16 32.131578815 11.918 10.815 9.311 8.265 6.947 M2.5V 111 0
10 HD 152751 Er* 16 55 28.75758 -08 20 10.7876 11.647 10.593 9.023 7.937 6.565 M3.5Ve 484 1
11 * 36 Oph ** 17 15 20.9839376 -26 36 10.157115           K2V+K1V 116 0
12 V* V2215 Oph RS* 17 16 13.3627374963 -26 32 46.133091527   7.50 6.34   4.8 K5V 279 0
13 Ross 154 Er* 18 49 49.3638007809 -23 50 10.453568573 13.528 12.19 10.43 10.23 7.703 M3.5Ve 323 0
14 V* AU Mic BY* 20 45 09.5323695486 -31 20 27.241710746   10.05 8.627 9.078 6.593 M1VeBa1 893 0
15 * 61 Cyg ** 21 06 53.95 +38 44 57.9           ~ 158 0
16 * 61 Cyg B Fl* 21 06 55.2640651855 +38 44 31.362140913 8.63 7.40 6.03 4.86 3.55 K7V 667 1
17 BD-05 5480 ** 21 08 45.4902104001 -04 25 36.493307291   10.62 9.43     M1 46 0
18 V* AX Mic Er* 21 17 15.2688576495 -38 52 02.510022611   8.09 6.68     M1V 203 0
19 V* EV Lac Er* 22 46 49.7311740821 +44 20 02.372223230   11.85 10.26 9.89   M4.0V 801 2
20 HD 217357 PM* 23 00 16.1224771183 -22 31 27.651428500 10.494 9.251 7.869 7.014 6.238 K7+Vk 158 0
21 HD 217987 PM* 23 05 52.0354545522 -35 51 11.058757520   8.82 7.34     M2V 218 0
22 V* BR Psc BY* 23 49 12.5251391270 +02 24 04.403044891 11.532 10.427 8.993 8.029 6.946 M1VFe-1 282 0

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2020.07.14-00:17:31

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