2014MNRAS.440.1674H

Query : 2014MNRAS.440.1674H

2014MNRAS.440.1674H - Mon. Not. R. Astron. Soc., 440, 1674-1679 (2014/May-2)

Amplitude variability in satellite photometry of the non-radially pulsating O9.5 V star ζ Oph.

HOWARTH I.D., GOSS K.J.F., STEVENS I.R., CHAPLIN W.J. and ELSWORTH Y.

Abstract (from CDS):

We report a time series analysis of satellite photometry of the non-radially pulsating Oe star ζ Oph, principally using data from the Solar Mass Ejection Imager obtained during 2003-2008, but augmented with Microvariability and Oscillations of STars and Wide-field InfraRed Explorer results. Amplitudes of the strongest photometric signals, at 5.18, 2.96 and 2.67/d, each vary independently over the 51/2-year monitoring period (from ∼ 50 to ≲ 2 mmag at 5.18/d), on time-scales of hundreds of days. Signals at 7.19 and 5.18/d have persisted (or recurred) for at least two decades. Supplementary spectroscopic observations show an Hα emission episode in 2006; this coincided with small increases in amplitudes of the three strongest photometric signals.

Abstract Copyright: © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2014)

Journal keyword(s): asteroseismology - techniques: photometric - stars: activity - stars: emission line, Be - stars: individual: ζ Oph - stars: oscillations

Simbad objects: 6

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Number of rows : 6
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 * alf Eri Be* 01 37 42.84548 -57 14 12.3101 -0.36 0.30 0.46 0.49 0.60 B6Vpe 495 1
2 * gam Dor gD* 04 16 01.5866224848 -51 29 11.932714356   4.55 4.20     F1V 337 0
3 V* CU Vir a2* 14 12 15.8055434051 +02 24 33.945178515 4.46 4.90 5.02 5.10 5.23 ApSi 411 0
4 * alf Boo RG* 14 15 39.67207 +19 10 56.6730 2.46 1.18 -0.05 -1.03 -1.68 K1.5IIIFe-0.5 2417 1
5 * bet UMi V* 14 50 42.32580 +74 09 19.8142 5.32 3.55 2.08 0.97 0.21 K4-III 344 1
6 * zet Oph Be* 16 37 09.5400587698 -10 34 01.509742704 1.73 2.58 2.56 2.46 2.50 O9.2IVnn 1908 0

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