2007A&A...471..941L


Query : 2007A&A...471..941L

2007A&A...471..941L - Astronomy and Astrophysics, volume 471, 941-949 (2007/9-1)

The helium weak silicon star HR7224. II. Doppler Imaging analysis.

LEHMANN H., TKACHENKO A., FRAGA L., TSYMBAL V. and MKRTICHIAN D.E.

Abstract (from CDS):

We investigate the abundance distributions of silicon and iron on the surface of HR7224 and check for the presence of magnetic fields. We try further to find an explanation for the observed Balmer line variations, alternative to that by surface temperature gradients given in a previous article. Based on time series of more than 570 high-resolution spectra we investigate the abundance distribution of silicon and iron using the Doppler Imaging technique applying two independent program codes and using single and multiple components atmosphere models. We further calculate the combined effect of abundance changes of Si, Fe, and He on the Hβ line profile and compare it with the observations. The mean longitudinal magnetic field strength of HR7224 is measured spectropolarimetrically. The Doppler Imaging analysis of HR7224 shows the presence of large silicon and iron spots on the star's surface, large gradients of the abundances of these elements, and hints to enhanced line strengths near the visible pole of the star. The explanation of the observed Balmer line variations by inhomogeneous abundance distributions alone requires unrealistic large gradients of the helium abundance. Magnetic field measurements gave no definite results, a field strength of the order of +400G is likely. We can exclude the hypothesis that the hydrogen line profile variations of HR7224 are caused by inhomogeneous abundance distributions of Fe, Si, and He alone or by pressure gradients like in the case of Ap stars. Still the observed variations can be described only by the combined effect of abundance and temperature gradients. In this case, the derived Doppler imaging maps will reflect also the temperature gradients and the surface will be cooler in regions of enhanced line strength like at the visible pole. At present state, the physical origin of possible surface temperature gradients remains unknown.

Abstract Copyright:

Journal keyword(s): stars: chemically peculiar - stars: variables: general - stars: atmospheres - stars: abundances

Simbad objects: 3

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Number of rows : 3
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 * alf02 CVn a2* 12 56 01.6662171 +38 19 06.154110 2.44 2.76 2.88 2.98 3.05 A0VpSiEu 661 0
2 V* CU Vir a2* 14 12 15.8054758 +02 24 33.953395 4.46 4.90 5.02 5.10 5.23 ApSi 371 0
3 V* EE Dra a2* 18 58 52.6267962600 +69 31 52.648832568   6.353 6.506     B9III 90 1

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2022.05.28-21:52:02

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