2002A&A...389..524G


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.10CEST01:25:43

2002A&A...389..524G - Astronomy and Astrophysics, volume 389, 524-536 (2002/7-2)

Multiwavelength optical observations of chromospherically active binary systems. IV. The X-ray/EUV selected binary BK Psc (2RE J0039+103).

GALVEZ M.C., MONTES D., FERNANDEZ-FIGUEROA M.J., LOPEZ-SANTIAGO J., DE CASTRO E. and CORNIDE M.

Abstract (from CDS):

We present high resolution echelle spectra taken during four observing runs from 1999 to 2001 of the recently X-ray/EUV selected chromospherically active binary BK Psc (2RE J0039+103). Our observations confirm the single-lined spectroscopic binary (SB1) nature of this system and allow us to obtain, for the first time, the orbital solution of the system as in the case of a SB2 system. We have determined precise radial velocities of both components: for the primary by using the cross correlation technique, and for the secondary by using its chromospheric emission lines. We have obtained a circular orbit with an orbital period of 2.1663 days, very close to its photometric period of 2.24 days (indicating synchronous rotation). The spectral type (K5V) we determined for our spectra and the mass ratio (1.8) and minimum masses (Msin3i) resulting from the orbital solution are compatible with the observed K5V primary and an unseen M3V secondary. Using this spectral classification, the projected rotational velocity (vsini, of 17.1km/s) obtained from the width of the cross-correlation function and the data provided by Hipparcos, we have derived other fundamental stellar parameters. The kinematics and the non-detection of the Li I line indicate that it is an old star. The analysis of the optical chromospheric activity indicators from the Ca II H & K to Ca II IRT lines, by using the spectral subtraction technique, indicates that both components of the binary system show high levels of chromospheric activity. Hα emission above the continuum from both components is a persistent feature of this system during the period 1999 to 2001 of our observations as well as in previous observations. The Hα and Hβ emission seems to arise from prominence-like material, and the Ca II IRT emission from plage-like regions.

Abstract Copyright:

Journal keyword(s): stars: individual: BK Psc - stars: activity - stars: binaries: spectroscopic - stars: chromospheres - stars: late-type - stars: rotation

Simbad objects: 11

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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 V* BK Psc RS* 00 39 42.1677083682 +10 39 13.676526271   11.73 10.488 10.038 8.933 K5V+M3V 49 0
2 V* UX Ari RS* 03 26 35.3764089427 +28 42 54.211100955 7.76 7.28 6.37     K0IV 663 0
3 HD 22468 RS* 03 36 47.2911034958 +00 35 15.938962144 7.09 6.63   5.4   K2:Vnk 1124 0
4 HD 283750 BY* 04 36 48.2413370074 +27 07 55.898311812   9.354   7.4   K2.5Ve 254 2
5 HD 29697 BY* 04 41 18.8553438360 +20 54 05.447950758 10.064 9.12 7.985 7.313 6.666 K4V 150 0
6 V* YY Gem BY* 07 34 37.4475372002 +31 52 10.181030942 11.60 10.56 9.27 7.69 6.67 M0.5VeFe-2 818 0
7 V* DM UMa RS* 10 55 43.5440100939 +60 28 09.722249634   10.31 9.29     K0III-IV 153 0
8 V* HU Vir RS* 12 13 20.6903303051 -09 04 46.844857323   9.69 8.71   7.639 K1V 136 0
9 HD 154363 PM* 17 05 03.3947074782 -05 03 59.437237339 9.945 8.881 7.709 6.985 6.364 K4/5V 201 0
10 V* BY Dra BY* 18 33 55.7719224141 +51 43 08.903033617 10.22 9.23   8.733   K4Ve+K7.5Ve 594 0
11 * 61 Cyg A BY* 21 06 53.9396100677 +38 44 57.897024357 7.50 6.39 5.21 4.19 3.54 K5V 947 0

    Equat.    Gal    SGal    Ecl

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2020.08.10-01:25:43

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