J/AJ/151/106 Radial velocities in 2006-2014 for HD 89758 (Lee+, 2016)
Long-period variations in the radial velocity of spectroscopic binary M giant
µ Ursae Majoris.
Lee B.-C., Han I., Park M.-G., Mkrtichian D.E., Hatzes A.P., Jeong G.,
Kim K.-M.
<Astron. J., 151, 106 (2016)>
=2016AJ....151..106L 2016AJ....151..106L (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, spectroscopic ; Stars, M-type ; Stars, giant ;
Radial velocities
Keywords: stars: chromospheres - techniques: radial velocities -
stars: individual (µ Ursae Majoris (HD 89758)) - stars: rotation
Abstract:
We report that the spectroscopic binary µ Ursae Majoris (µ UMa)
has secondary RV variations of 471.2 days in addition to those of
230.0 days already known. Keplerian orbit analysis yields stellar mass
companions of 1.6M☉ for the 230 day period and 0.14M☉for
the 471 day period. However, the HIPPARCOS photometries show a period
similar to the stellar rotational period, which is one-quarter of the
RV period. Variations in the bisector velocity curvature show a period
of 463.6 days. We also find ∼473 day variations in the equivalent
width (EW) measurements of the Hα and Hβ lines, whose
origin is probably stellar activity. We note that the nature of 471
day variations is similar to one observed in "Sequence D" of
Asymptotic Giant Branch pulsating stars. We therefore conclude that
the RV and the EW variations in the spectroscopic binary M giant µ
UMa A originate from the complex pulsations and the chromospheric
activity.
Description:
Observations were carried out using the fiber-fed high-resolution
Bohyunsan Observatory Echelle Spectrograph (BOES) attached to the 1.8m
telescope at Bohyunsan Optical Astronomy Observatory (BOAO) in Korea.
One exposure with the BOES has a wavelength coverage 3500-10500Å
distributed over ∼80 spectral orders. In order to provide precise
radial velocity measurements, we used the 80µm diameter fiber which
yields a resolving power R=90000.
Over the eight-year period from 2006 November to 2014 November (56
nights in total), 112 spectra for µ UMa were collected. The
estimated signal-to-noise ratio (S/N) in the I2 region was about 250
with a typical exposure time ranging from 60 to 480s.
We report our radial velocity data for µ UMa in Table2.
Objects:
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RA (ICRS) DE Designation(s) (Period)
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10 22 19.74 +41 29 58.3 * mu. UMa = HD 89758 (P=230)
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 22 112 Radial velocity (RV) measurements for µ UMa
from 2006 November to 2014 November
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See also:
I/239 : The Hipparcos and Tycho Catalogues (ESA 1997)
J/AJ/135/209 : Rotational and radial velocities 761 HIP giants
(Massarotti+, 2008)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 F9.4 d JD Julian Date (JD-2450000)
11- 17 F7.4 km/s RV [-6.1/9.8] Radial velocity
19- 22 F4.1 m/s e_RV [4.9/13] 1σ uncertainty in RV
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History:
From electronic version of the journal
(End) Sylvain Guehenneux [CDS] 18-Jul-2016