2006A&A...460..855W


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.18CET16:13:17

2006A&A...460..855W - Astronomy and Astrophysics, volume 460, 855-864 (2006/12-4)

Tests of stellar model atmospheres by optical interferometry. IV. VINCI interferometry and UVES spectroscopy of Menkar.

WITTKOWSKI M., AUFDENBERG J.P., DRIEBE T., ROCCATAGLIATA V., SZEIFERT T. and WOLFF B.

Abstract (from CDS):

We present coordinated near-infrared K-band interferometric and optical spectroscopic observations of the M1.5 giant {alpha} Cet (Menkar) obtained with the instruments VINCI and UVES at the Paranal Observatory. Spherically symmetric PHOENIX stellar model atmospheres are constrained by comparison to our interferometric and spectroscopic data, and high-precision fundamental parameters of Menkar are obtained. Our high-precision VLTI/VINCI observations in the first and second lobes of the visibility function directly probe the model-predicted strength of the limb darkening effect in the K-band and the stellar angular diameter. The high spectral resolution of UVES of R=80000-110000 allows us to confront in detail observed and model-predicted profiles of atomic lines and molecular bands. We show that our derived PHOENIX model atmosphere for Menkar is consistent with both the measured strength of the limb-darkening in the near-infrared K-band and the profiles of spectral bands around selected atomic lines and TiO bandheads from 370 nm to 1000 nm. At the detailed level of our high spectral resolution, however, noticeable discrepancies between observed and synthetic spectra exist. We obtain a high-precision Rosseland angular diameter of ΘRoss=12.20mas±0.04mas. Together with the Hipparcos parallax of 14.82mas±0.83mas, it corresponds to a Rosseland radius of RRoss=89±5R, and together with the bolometric flux based on available spectrophotometry, to an effective temperature of Teff=3795K±70K. The luminosity based on these values is L=1460L±300L. Relying on stellar evolutionary tracks, these values correspond to a mass M=2.3M±0.2M and a surface gravity logg=0.9±0.1 (cgs). Our approach illustrates the power of combining interferometry and high-resolution spectroscopy to constrain and calibrate stellar model atmospheres. The simultaneous agreement of the model atmosphere with our interferometric and spectroscopic data increases confidence in the reliability of the modelling of this star, while discrepancies at the detailed level of the high resolution spectra can be used to further improve the underlying model.

Abstract Copyright:

Journal keyword(s): techniques: interferometric - stars: late-type - stars: atmospheres - stars: fundamental parameters - stars: pulsars individual: α Ceti

Simbad objects: 32

goto Full paper

goto View the reference in ADS

Number of rows : 32

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 * iot Cet * 00 19 25.6741634 -08 49 26.111055 5.94 4.77 3.55 2.70 2.11 K1+IIICN0.5 165 0
2 * bet Cet PM* 00 43 35.37090 -17 59 11.7827 3.90 3.02 2.01 1.29 0.78 G9.5IIICH-1 495 0
3 * eta Cet HB* 01 08 35.3914827 -10 10 56.156955 5.80 4.61 3.45 2.61 2.03 K2-IIIb 196 0
4 * psi Phe LP* 01 53 38.7410337 -46 18 09.604795 7.71 6.00 4.41 2.68 1.17 M4III 96 0
5 * chi Phe PM* 02 01 42.3769730947 -44 42 48.626974441 8.45 6.63 5.14 3.92 3.03 K5IV 53 0
6 * 19 Ari PM* 02 13 03.3043219962 +15 16 47.511166052 9.20 7.25 5.70 4.48 3.50 M0III 67 0
7 * iot Eri PM* 02 40 40.0350054 -39 51 19.354141   5.114 4.116     K0IIIb 75 0
8 * eta Eri PM* 02 56 25.6494839 -08 53 53.322099 5.97 4.99 3.87 3.08 2.50 K1+IIIb 176 0
9 * alf Cet LP? 03 02 16.77307 +04 05 23.0596 6.10 4.17 2.53 1.18 0.02 M1.5IIIa 437 0
10 * 93 Cet * 03 02 22.5177188806 +04 21 10.390176694 5.11 5.51 5.607     B8V 64 0
11 * gam Cae ** 05 04 24.40218 -35 28 58.7161 6.94 5.75 4.55 3.64 2.99 K2.5IIIb+G8IV 42 0
12 * eta02 Pic PM* 05 04 58.0143319993 -49 34 40.203357685 8.35 6.47 5.01 3.81 2.90 K5III 44 0
13 * e Ori * 05 23 56.8276764 -07 48 29.033204 5.78 5.08 4.12 3.40 2.90 G8+III 132 0
14 HD 35536 * 05 25 01.7442296144 -10 19 43.986835247   7.126 5.586     K4III 25 0
15 * 31 Ori V* 05 29 43.9814689897 -01 05 32.058230061   6.28 4.71     K4III 85 0
16 HD 45018 * 06 23 55.9110668632 -25 34 39.441089133   7.162 5.600     K5III 28 0
17 * alf Car * 06 23 57.10988 -52 41 44.3810 -0.49 -0.59 -0.74 -0.96 -1.13 A9II 413 0
18 * nu.02 CMa PM* 06 36 41.0375756 -19 15 21.165905 5.96 5.011 3.91 3.13 2.61 K1.5III-IVFe1 236 1
19 * 30 Gem PM* 06 43 59.2869703486 +13 13 40.818795627 6.82 5.65 4.49 3.63 3.03 K0+IIICa1 131 0
20 * alf CMa SB* 06 45 08.91728 -16 42 58.0171 -1.51 -1.46 -1.46 -1.46 -1.43 A1V+DA 1374 0
21 * 17 Mon * 06 47 19.8294628711 +08 02 14.123889454 7.82 6.17 4.77 3.74 3.04 K4III 110 0
22 * 18 Mon SB* 06 47 51.6475157606 +02 24 43.840168370 6.62 5.58 4.47 3.68 3.13 K0+III 147 0
23 * tet CMa PM* 06 54 11.3997692336 -12 02 19.061054441 7.20 5.51 4.08 2.95 2.17 K3/4III 207 0
24 * 28 Mon Ro* 08 01 13.3357402 -01 23 33.393493   6.147 4.680     K4III 70 1
25 * zet Hya PM* 08 55 23.6261352 +05 56 44.035380 4.92 4.10 3.10 2.39 1.90 G8.5III 225 0
26 * 6 Leo * 09 31 57.5763848558 +09 42 56.765156324 7.97 6.44 5.07     K2.5IIIFe-0.5 72 0
27 * iot Hya PM* 09 39 51.3614457 -01 08 34.113491 6.68 5.23 3.91 2.92 2.25 K2.5III 164 0
28 * 31 Leo PM* 10 07 54.2705662 +09 59 51.023021 7.57 5.82 4.38 3.26 2.49 K3.5IIIbFe-1: 125 0
29 * B Cen PM* 11 51 08.6914879300 -45 10 24.488999847 7.22 5.76 4.46 3.52 2.85 K3III 70 0
30 HD 168592 PM* 18 22 18.5735335091 -38 39 24.831468681   6.579 5.073     K4/5III 23 0
31 HD 174387 V* 18 52 27.2291396679 -46 35 42.436364562   7.121 5.490     M0III 23 0
32 * gam Sge PM* 19 58 45.4286265 +19 29 31.728079 6.97 5.04 3.47 2.27 1.35 M0-III 239 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2006A&A...460..855W and select 'bookmark this link' or equivalent in the popup menu


2019.11.18-16:13:17

© Université de Strasbourg/CNRS

    • Contact