Wire satellite photometry of eclipsing binary stars
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WIRE SATELLITE PHOTOMETRY OF ECLIPSING BINARY STARS. John Southworth H Bruntt D L Buzasi. The WIRE satellite. Launched in 1999 for an IR galaxy survey electronics problem caused loss of coolant. The WIRE satellite. Launched in 1999 for an IR galaxy survey

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WIRE SATELLITE PHOTOMETRY OF ECLIPSING BINARY STARS

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Wire satellite photometry of eclipsing binary stars

WIRE SATELLITE PHOTOMETRY OF ECLIPSING BINARY STARS

John Southworth H Bruntt D L Buzasi


The wire satellite

The WIRE satellite

  • Launched in 1999 for an IR galaxy survey

    • electronics problem caused loss of coolant


The wire satellite1

The WIRE satellite

  • Launched in 1999 for an IR galaxy survey

    • electronics problem caused loss of coolant

  • Star tracker used since 1999 as a high-speed photometer

    • aperture: 5 cm

    • cadence: 2 Hz

    • 5 targets at once


Eclipsing binaries with wire centauri

Eclipsing binaries with WIRE: ψ Centauri

  • V = 4.0 spectral type = B9 V + A2 V

  • Previously known to be a spectroscopic binary

  • WIRE light curve: 41 000 points with 2 mmag scatter


Wire satellite photometry of eclipsing binary stars

Eclipsing binaries with WIRE: ψ Centauri

  • Orbital period = 38.8 days Total eclipses

  • Light curve fitted with JKTEBOP: fractional radii to 0.1%

  • See Bruntt et al., 2006, A&A, 456, 651


Eclipsing binaries with wire aurigae

Eclipsing binaries with WIRE: β Aurigae

  • V = 1.9 Orbital period = 3.960 days

  • Spectral type = A1m + A1m

  • Eclipses discovered in 1911

  • WIRE light curve: 30 000 points with 0.3 mmag scatter


Eclipsing binaries with wire aurigae1

Eclipsing binaries with WIRE: β Aurigae

  • JKTEBOP fit (nonlinear LD):(r1+r2) to 0.1%

    r1 and r2 to 5 %

  • Add in spectroscopic light ratio:r1 and r2 to 0.5%


Eclipsing binaries with wire aurigae2

Eclipsing binaries with WIRE: β Aurigae

  • M1 = 2.376 ± 0.027 M R1 = 2.762± 0.017 R

  • M2 = 2.291± 0.027 M R2 = 2.568± 0.017 R

  • Southworth et al., 2007, A&A, in press (astro-ph/0703634)


Wire satellite photometry of eclipsing binary stars

Eclipsing binaries with WIRE: AR Cas

  • Period = 6.07 days B4 V + A6 V V = 4.9

  • Light curve contains 2 mmag variation at primary star rotation period and several pulsation frequencies


Wire satellite photometry of eclipsing binary stars

Eclipsing binaries with WIRE: δCap

  • V = 2.9 Orbital period = 1.02 days

  • Spectral type = Am + F

  • X-ray source: coronal activity?


Wire satellite photometry of eclipsing binary stars

Eclipsing binaries with WIRE: δCap

  • Primary component is variable, perhaps a δ Scuti star


Wire satellite photometry of eclipsing binary stars1

WIRE satellite photometry of eclipsing binary stars

John Southworth Hans Bruntt Derek L Buzasi


Wire satellite photometry of eclipsing binary stars

John Southworth

University of Warwick

[email protected]

http://www.astro.keele.ac.uk/~jkt


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