Two new variable sdB stars, HE 0218-3437 and LB 1516

C. Koen; D. Kilkenny; M. L. Pretorius; D. J. Frew

doi:10.1111/j.1365-2966.2009.15761.x

Two new variable sdB stars, HE 0218-3437 and LB 1516

C. Koen^*, D. Kilkenny, M. L. Pretorius, D. J. Frew

^*Corresponding author for this work

Department of Physics and Astronomy

Research output: Contribution to journal › Article

9 Citations (Scopus)

Abstract

We present photometry which shows that two known hot subdwarf stars, HE 0218-3437 and LB 1516, are variable. LB 1516 exhibits several frequencies in the range 12-25 cycles d^-1 (periods of about 1-2 h) with amplitudes less than about 0.003 mag and appears to be a typical slowly pulsating sdB star. Results from a multisite campaign on HE 0218-3437 show the presence of two frequencies only, the lower amplitude variation an apparent subharmonic of the higher amplitude periodicity. It is likely that the star is in a binary system, and that the variability is due to ellipsoidal deformation of the primary star.

Original language	English
Pages (from-to)	1850-1856
Number of pages	7
Journal	Monthly Notices of the Royal Astronomical Society
Volume	401
Issue number	3
DOIs	https://doi.org/10.1111/j.1365-2966.2009.15761.x
Publication status	Published - Jan 2010

Keywords

Stars: individual (HE 0218-3437; LB 1516)
Stars: oscillations
Stars: variables: other

Access to Document

10.1111/j.1365-2966.2009.15761.x

Link to publication in Scopus

Fingerprint Dive into the research topics of 'Two new variable sdB stars, HE 0218-3437 and LB 1516'. Together they form a unique fingerprint.

Cite this

@article{cf72b56b51e44f9ca0d671a4ff69ecf4,

title = "Two new variable sdB stars, HE 0218-3437 and LB 1516",

abstract = "We present photometry which shows that two known hot subdwarf stars, HE 0218-3437 and LB 1516, are variable. LB 1516 exhibits several frequencies in the range 12-25 cycles d-1 (periods of about 1-2 h) with amplitudes less than about 0.003 mag and appears to be a typical slowly pulsating sdB star. Results from a multisite campaign on HE 0218-3437 show the presence of two frequencies only, the lower amplitude variation an apparent subharmonic of the higher amplitude periodicity. It is likely that the star is in a binary system, and that the variability is due to ellipsoidal deformation of the primary star.",

keywords = "Stars: individual (HE 0218-3437; LB 1516), Stars: oscillations, Stars: variables: other",

author = "C. Koen and D. Kilkenny and Pretorius, {M. L.} and Frew, {D. J.}",

year = "2010",

month = "1",

doi = "10.1111/j.1365-2966.2009.15761.x",

language = "English",

volume = "401",

pages = "1850--1856",

journal = "Monthly Notices of the Royal Astronomical Society: Letters",

issn = "1745-3925",

publisher = "Oxford University Press",

number = "3",

}

TY - JOUR

T1 - Two new variable sdB stars, HE 0218-3437 and LB 1516

AU - Koen, C.

AU - Kilkenny, D.

AU - Pretorius, M. L.

AU - Frew, D. J.

PY - 2010/1

Y1 - 2010/1

N2 - We present photometry which shows that two known hot subdwarf stars, HE 0218-3437 and LB 1516, are variable. LB 1516 exhibits several frequencies in the range 12-25 cycles d-1 (periods of about 1-2 h) with amplitudes less than about 0.003 mag and appears to be a typical slowly pulsating sdB star. Results from a multisite campaign on HE 0218-3437 show the presence of two frequencies only, the lower amplitude variation an apparent subharmonic of the higher amplitude periodicity. It is likely that the star is in a binary system, and that the variability is due to ellipsoidal deformation of the primary star.

AB - We present photometry which shows that two known hot subdwarf stars, HE 0218-3437 and LB 1516, are variable. LB 1516 exhibits several frequencies in the range 12-25 cycles d-1 (periods of about 1-2 h) with amplitudes less than about 0.003 mag and appears to be a typical slowly pulsating sdB star. Results from a multisite campaign on HE 0218-3437 show the presence of two frequencies only, the lower amplitude variation an apparent subharmonic of the higher amplitude periodicity. It is likely that the star is in a binary system, and that the variability is due to ellipsoidal deformation of the primary star.

KW - Stars: individual (HE 0218-3437; LB 1516)

KW - Stars: oscillations

KW - Stars: variables: other

UR - http://www.scopus.com/inward/record.url?scp=73949087908&partnerID=8YFLogxK

U2 - 10.1111/j.1365-2966.2009.15761.x

DO - 10.1111/j.1365-2966.2009.15761.x

M3 - Article

VL - 401

SP - 1850

EP - 1856

JO - Monthly Notices of the Royal Astronomical Society: Letters

JF - Monthly Notices of the Royal Astronomical Society: Letters

SN - 1745-3925

IS - 3

ER -