2006A&A...451..999F


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.15CEST08:20:35

2006A&A...451..999F - Astronomy and Astrophysics, volume 451, 999-1008 (2006/6-1)

A comprehensive study of the SX Phoenicis star BL Camelopardalis.

FAUVAUD S., RODRIGUEZ E., ZHOU A.Y., SAREYAN J.-P., RIBAS I., REED M.D., KLINGENBERG G., FARRELL J., MICHELET J., ROBINSON S.E., SANTACANA G. and RIVES J.J.

Abstract (from CDS):

BL Cam is an extreme field multiperiodic short-period low-metallicity high-amplitude SX Phe-type variable where its probably complex pulsational content is subject of controversies. A comprehensive study has been carried out to investigate the nature and pulsational properties of this object. The analysis is based on new photometric data collected during the last few years at different sites, as well as on all available previously published data. Frequency analyses have been performed on a number of reliable data sets to analyse the pulsational content. In addition, the classical O-C method was used to study the behaviour of the main period. Our frequency analysis confirms some aspects on the multiperiodicity of BL Cam, previously found by other authors, showing a number of secondary modes close to the main frequency f0=25.5769/cd. The secondary modes present eventual amplitude variations. However, the main frequency exhibits no significant changes in its amplitude and seems to correspond to the fundamental mode of radial pulsation. Abrupt changes sometimes observed in the light curves could be due to spurious activity on or close to the star's photosphere. We confirm the existence of a secondary frequency at 31.6 or 32.6/cd, with variable amplitude, and with the possibility of both frequencies being intrinsic to the star. More than one hundred of new times of light maxima have been determined in the present work. These together with those available in the literature allow us a more discriminating analysis of the O-C diagram. This shows that the observed variations of the main period can be described by two terms: (i) a secular increase of the main period at a rate of dP/Pdt=117(±3)x10–9yr–1; and (ii) a perturbation from a companion star in a rather eccentric orbit with a period of 10.5(±0.2)yr causing a light time semi-amplitude of 148(±12)s.

Abstract Copyright:

Journal keyword(s): stars: variables: delta Sct - stars: individual: BL Cam - stars: oscillations - techniques: photometric

Simbad objects: 10

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Number of rows : 10

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* RV Ari dS* 02 15 07.5020716546 +18 04 27.916736220   11.78       A 68 0
2 GD 428 SX* 03 47 19.8771931141 +63 22 42.147345302   13.10   13.26   ~ 98 0
3 V* RY Lep dS* 05 48 10.2617974702 -20 01 24.925632678   8.60 8.25     A9V 54 0
4 V* AI Vel dS* 08 14 05.1458681791 -44 34 32.852065552   6.98 6.70     A9IV/V 178 0
5 NGC 5139 GlC 13 26 47.28 -47 28 46.1   6.12 5.33     ~ 2997 0
6 * del Sct dS* 18 42 16.4270465894 -09 03 09.200429056   5.04 4.71     F2II-III 447 0
7 V* XX Cyg SX* 20 03 15.6422423360 +58 57 16.525128223   11.99 11.86     A5-F5 110 0
8 V* DY Peg SX* 23 08 51.1855512550 +17 12 55.998206149   10.56 10.26     F5 191 1
9 V* BX Scl SX* 23 43 54.4552644084 -28 18 34.625979560   13.82 13.56     A 40 0
10 V* SX Phe SX* 23 46 32.8929064612 -41 34 54.770795675   7.40 7.12     A3V 313 0

    Equat.    Gal    SGal    Ecl

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2020.07.15-08:20:35

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