2009A&A...506..845Z


C.D.S. - SIMBAD4 rel 1.7 - 2020.12.01CET01:15:12

2009A&A...506..845Z - Astronomy and Astrophysics, volume 506, 845-856 (2009/11-1)

The puzzling binary HD 143418.

ZVERKO J., ZIZNOVSKY J., MIKULASEK Z., KRTICKA J., ILIEV I.K., STATEVA I.K., ROMANYUK I.I. and KUDRYAVTSEV D.O.

Abstract (from CDS):

object{HD143418} was discovered recently to be a double-lined spectroscopic binary with a primary designated as a CP star. Its light displays an orbital phase coupled variability with a peak-to-peak amplitude up to 0.04 mag. The photometry available and new high dispersion spectra were investigated from a point of view of CP characteristics. A series of high resolution high S/N coude spectra was acquired from which 25 weak to strong unblended lines of FeI and II, TiII, CrII, ZrII, and BaII were selected to study spectral line variability. Two Zeeman spectra were obtained to search for a possible magnetic field of the star, and one echelle spectrum in a wide spectral region was analysed for abundance determination by means of synthetic spectra. The photometric observations were subjected to a PCA disentangling of the complex photometric behaviour. We identified spectral lines of the secondary in the yellow region on the echelle as well as on two coude spectra, whose occurence belongs to an F6V star and the intensity corresponds to the luminosity ratio 0.06. Equivalent widths of the selected spectral lines of the primary component do not change within the errors of measurements. The spectra taken with a Zeeman analyser do not indicate a magnetic field. The abundance pattern does not correspond to characteristics of a variable CP2 star. The only remarkable deviation is a more than 1.1dex deficit of scandium, one of the properties of non-variable Am stars. The photometric variability is tied to the orbital period and is due to ellipticity of the primary component and not to a putatively structured surface of the primary that is confirmed to rotate subsynchronously. The seasonal component of the light curve changes in amplitude as well as in shape. We conclude that the primary is a normal, mildly evolved A5V main sequence star. The seasonal variability of the orbitally modulated light curves may be related to an expected incidence of circumstellar matter originating in the tidally spinning up primary component. HD143418 may be a prototype of a rare detached interacting close binary containing a subsynchronously rotating primary passing through its synchronisation stage.

Abstract Copyright:

Journal keyword(s): binaries: spectroscopic - stars: variables: general - stars: chemically peculiar - stars: abundances - stars: evolution - stars: individual HD143418

VizieR on-line data: <Available at CDS (J/A+A/506/845): table5.dat table6.dat>

Simbad objects: 12

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Number of rows : 12

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 * 56 Ari a2* 03 12 14.2459541239 +27 15 25.093114957 5.22 5.64 5.76     B6IV-V 248 0
2 HD 27411 PM* 04 18 37.4919030999 -22 58 10.991833387   6.372 6.060     A3mA5-F2 48 0
3 V* HZ Aur a2* 05 06 08.3583752373 +33 55 07.279474095   7.03 7.07     B9p 172 0
4 * 20 Leo dS* 09 49 50.0942643 +21 10 45.919205   6.330 6.077     A7IVn 121 0
5 * o Leo SB* 11 55 40.5342459259 +15 38 48.556539104   5.632 5.522     A3V 154 0
6 V* CQ UMa a2* 13 40 21.3848513037 +57 12 27.377068970   6.380 6.273     A2IVpSrCr 105 0
7 * 4 Her Be* 15 55 30.5918031179 +42 33 58.287739693 5.23 5.64 5.75   5.82 B9pe 169 0
8 HD 143418 * 15 58 25.6764975855 +43 12 49.352719087   7.58 7.40     A3 19 0
9 * ome Oph a2* 16 32 08.1998273 -21 27 59.012005 4.69 4.56 4.45 4.32 4.30 ApSrEuCr 145 0
10 V* V624 Her Al* 17 44 17.2470660480 +14 24 36.243720020   6.398 6.194     A3m 154 0
11 V* EE Dra a2* 18 58 52.6265049377 +69 31 52.643645693   6.353 6.506     B9III 86 1
12 V* V1291 Aql a2* 19 53 18.7357390150 -03 06 52.065320660   5.837 5.619     F0VpSrCrEu 261 0

    Equat.    Gal    SGal    Ecl

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2020.12.01-01:15:12

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