ULTRACAM photometry of the eclipsing cataclysmic variables XZ Eri and DV UMa

W. J. Feline; V. S. Dhillon; T. R. Marsh; C. S. Brinkworth

doi:10.1111/j.1365-2966.2004.08302.x

ULTRACAM photometry of the eclipsing cataclysmic variables XZ Eri and DV UMa

W. J. Feline, V. S. Dhillon, T. R. Marsh, C. S. Brinkworth

Research output: Contribution to journal › Article › peer-review

36 Scopus citations

Abstract

We present high-speed, three-colour photometry of the faint eclipsing cataclysmic variables XZ Eri and DV UMa. We determine the system parameters through two techniques: first, timings of the eclipse contact phases of the white dwarf and bright-spot using the derivative of the light curve; and secondly, a parametrized model of the eclipse fitted to the observed light curve by χ² minimization. For both objects, we prefer the latter method, as it is less affected by photon noise and rapid flickering. For XZ Eri we obtain a mass ratio q = 0.1098 ± 0.0017 and an orbital inclination i = 80°.16 ± 0°.09. For DV UMa we derive figures of q = 0.1506 ± 0.0009 and i = 84°.24 ± 0°.07. The secondary star in XZ Eri has a very low mass M_r/M⊙ = 0.0842 ± 0.0024, placing it close to the upper limit on the mass of a brown dwarf.

Original language	English
Pages (from-to)	1-10
Number of pages	10
Journal	Monthly Notices of the Royal Astronomical Society
Volume	355
Issue number	1
DOIs	https://doi.org/10.1111/j.1365-2966.2004.08302.x
State	Published - Nov 21 2004
Externally published	Yes

Keywords

Binaries: close
Binaries: eclipsing
Novae, cataclysmic variables
Stars: dwarf novae
Stars: individual: DV UMa
Stars: individual: XZ Eri

Access to Document

10.1111/j.1365-2966.2004.08302.x

Cite this

@article{2fcebed6c39d4cb4aad7baa814868c0c,

title = "ULTRACAM photometry of the eclipsing cataclysmic variables XZ Eri and DV UMa",

abstract = "We present high-speed, three-colour photometry of the faint eclipsing cataclysmic variables XZ Eri and DV UMa. We determine the system parameters through two techniques: first, timings of the eclipse contact phases of the white dwarf and bright-spot using the derivative of the light curve; and secondly, a parametrized model of the eclipse fitted to the observed light curve by χ2 minimization. For both objects, we prefer the latter method, as it is less affected by photon noise and rapid flickering. For XZ Eri we obtain a mass ratio q = 0.1098 ± 0.0017 and an orbital inclination i = 80°.16 ± 0°.09. For DV UMa we derive figures of q = 0.1506 ± 0.0009 and i = 84°.24 ± 0°.07. The secondary star in XZ Eri has a very low mass Mr/M⊙ = 0.0842 ± 0.0024, placing it close to the upper limit on the mass of a brown dwarf.",

keywords = "Binaries: close, Binaries: eclipsing, Novae, cataclysmic variables, Stars: dwarf novae, Stars: individual: DV UMa, Stars: individual: XZ Eri",

author = "Feline, \{W. J.\} and Dhillon, \{V. S.\} and Marsh, \{T. R.\} and Brinkworth, \{C. S.\}",

year = "2004",

month = nov,

day = "21",

doi = "10.1111/j.1365-2966.2004.08302.x",

language = "English",

volume = "355",

pages = "1--10",

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

issn = "0035-8711",

publisher = "Oxford University Press",

number = "1",

}

TY - JOUR

T1 - ULTRACAM photometry of the eclipsing cataclysmic variables XZ Eri and DV UMa

AU - Feline, W. J.

AU - Dhillon, V. S.

AU - Marsh, T. R.

AU - Brinkworth, C. S.

PY - 2004/11/21

Y1 - 2004/11/21

N2 - We present high-speed, three-colour photometry of the faint eclipsing cataclysmic variables XZ Eri and DV UMa. We determine the system parameters through two techniques: first, timings of the eclipse contact phases of the white dwarf and bright-spot using the derivative of the light curve; and secondly, a parametrized model of the eclipse fitted to the observed light curve by χ2 minimization. For both objects, we prefer the latter method, as it is less affected by photon noise and rapid flickering. For XZ Eri we obtain a mass ratio q = 0.1098 ± 0.0017 and an orbital inclination i = 80°.16 ± 0°.09. For DV UMa we derive figures of q = 0.1506 ± 0.0009 and i = 84°.24 ± 0°.07. The secondary star in XZ Eri has a very low mass Mr/M⊙ = 0.0842 ± 0.0024, placing it close to the upper limit on the mass of a brown dwarf.

AB - We present high-speed, three-colour photometry of the faint eclipsing cataclysmic variables XZ Eri and DV UMa. We determine the system parameters through two techniques: first, timings of the eclipse contact phases of the white dwarf and bright-spot using the derivative of the light curve; and secondly, a parametrized model of the eclipse fitted to the observed light curve by χ2 minimization. For both objects, we prefer the latter method, as it is less affected by photon noise and rapid flickering. For XZ Eri we obtain a mass ratio q = 0.1098 ± 0.0017 and an orbital inclination i = 80°.16 ± 0°.09. For DV UMa we derive figures of q = 0.1506 ± 0.0009 and i = 84°.24 ± 0°.07. The secondary star in XZ Eri has a very low mass Mr/M⊙ = 0.0842 ± 0.0024, placing it close to the upper limit on the mass of a brown dwarf.

KW - Binaries: close

KW - Binaries: eclipsing

KW - Novae, cataclysmic variables

KW - Stars: dwarf novae

KW - Stars: individual: DV UMa

KW - Stars: individual: XZ Eri

UR - https://www.scopus.com/pages/publications/9744285791

U2 - 10.1111/j.1365-2966.2004.08302.x

DO - 10.1111/j.1365-2966.2004.08302.x

M3 - Article

AN - SCOPUS:9744285791

SN - 0035-8711

VL - 355

SP - 1

EP - 10

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 1

ER -

ULTRACAM photometry of the eclipsing cataclysmic variables XZ Eri and DV UMa

Abstract

Keywords

Access to Document

Other files and links

Fingerprint

Cite this