2008A&A...492..841R


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.15CEST22:34:27

2008A&A...492..841R - Astronomy and Astrophysics, volume 492, 841-855 (2008/12-4)

Granulation in K-type dwarf stars. I. Spectroscopic observations.

RAMIREZ I., ALLENDE PRIETO C. and LAMBERT D.L.

Abstract (from CDS):

We seek to detect and quantify the effects of surface convection (granulation) on the line spectra of K-dwarfs as a first step towards a rigorous testing of hydrodynamic models for their atmospheres. Very high-resolution (R≃160000-210000), high signal-to-noise ratio (S/N>300) spectra of nine bright K-dwarfs were obtained with the 2dcoude spectrograph on the 2.7m telescope at McDonald Observatory to determine wavelength shifts and asymmetries of Fe i lines. Spectra of the same stars acquired with the High Resolution Spectrograph (R≃120,000) on the 9.2m Hobby Eberly Telescope were used as radial velocity templates to calibrate the wavelength scale of the 2dcoude spectra. The observed shapes and positions of Fe i lines reveal asymmetries and wavelength shifts that indicate the presence of granulation. In particular, line bisectors show characteristic C-shapes while line core wavelengths are blueshifted by an amount that increases with decreasing equivalent width (EW). On average, Fe i line bisectors have a span that ranges from nearly 0 for the weakest lines (residual core flux >0.7) to about 75m/s for the strongest lines (residual core flux ≃0.3), while wavelength shifts range from about -150m/s in the weakest (EW≃10mÅ) lines to 0 in the strongest (EW>100mÅ) features. A more detailed inspection of the bisectors and wavelength shifts reveals star-to-star differences that are likely associated with differences in stellar parameters, projected rotational velocity, and stellar activity. While the first two are understood and confirmed by our data, the relation to stellar activity, which is based on our finding that the largest departures from the expected behavior are seen in the most active stars, requires further investigation. For the inactive, slow projected rotational velocity stars, we detect, unequivocally, a plateau in the line-shifts at high EW values (EW> 100mÅ), a behavior that had been identified before only in the solar spectrum. The detection of this plateau allows us to determine the zero point of the convective blueshifts, which is useful to determine absolute radial velocities. Thus, we are able to measure such velocities with a mean uncertainty of about 60m/s for four of our sample stars.

Abstract Copyright:

Journal keyword(s): stars: atmospheres - stars: late-type - techniques: spectroscopic - Sun: granulation

Simbad objects: 11

goto Full paper

goto View the reference in ADS

Number of rows : 11

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 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1704 1
2 HD 32147 PM* 05 00 48.9991346145 -05 45 13.220341956 8.27 7.27 6.21 5.36 4.87 K3+V 415 1
3 HD 37394 BY* 05 41 20.3357283721 +53 28 51.810629854 7.58 7.07 6.23 5.54 5.11 K1 296 0
4 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1760 0
5 HD 61606 BY* 07 39 59.3285412183 -03 35 51.026043193 8.89 8.136 7.169 6.626 6.15 K3V 162 0
6 HD 115404 PM* 13 16 51.0517063595 +17 01 01.840304856   7.69 6.66     K2V 255 0
7 HD 160346 SB* 17 39 16.9163262 +03 33 18.875718   7.48   5.9   K3-V 270 0
8 HD 160263 * 17 41 16.2422185479 -46 55 18.613101509 5.72 5.78 5.79     A0V 52 0
9 * 70 Oph Ro* 18 05 27.28518 +02 30 00.3558 5.40 4.89 4.03 3.38 2.92 K0-V 607 0
10 * sig Dra PM* 19 32 21.5902990 +69 39 40.234737 5.860 5.460 4.680 4.04 3.63 K0V 582 0
11 HD 219134 Fl* 23 13 16.9747821012 +57 10 06.076520993 7.460 6.560 5.570 4.76 4.23 K3V 517 1

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2008A&A...492..841R and select 'bookmark this link' or equivalent in the popup menu


2020.08.15-22:34:27

© Université de Strasbourg/CNRS

    • Contact