Optical photometry and spectroscopy of the accretion-powered millisecond pulsar HETE J1900.1 − 2455

We present phase resolved optical photometry and spectroscopy of the accreting millisecond pulsar HETE J1900.1−2455. Our R-band light curves exhibit a sinusoidal modulation, at close to the orbital period, which we initially attributed to X-ray heating of the irradiated face of the secondary star. H...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2008-02, Vol.383 (4), p.1581-1587
Main Authors: Elebert, P., Callanan, P. J., Filippenko, A. V., Garnavich, P. M., Mackie, G., Hill, J. M., Burwitz, V.
Format: Article
Language:English
Subjects:
accretion
accretion discs
accretion, accretion discs
Astronomy
Earth, ocean, space
Exact sciences and technology
Pulsars
pulsars: individual: HETE J1900.1−2455
Spectrum analysis
techniques: photometric
techniques: spectroscopic
Tomography
X-rays: binaries
Citations: Items that cite this one
Online Access:Get full text
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Summary:We present phase resolved optical photometry and spectroscopy of the accreting millisecond pulsar HETE J1900.1−2455. Our R-band light curves exhibit a sinusoidal modulation, at close to the orbital period, which we initially attributed to X-ray heating of the irradiated face of the secondary star. However, further analysis reveals that the source of the modulation is more likely due to superhumps caused by a precessing accretion disc. Doppler tomography of a broad Hα emission line reveals an emission ring, consistent with that expected from an accretion disc. Using the velocity of the emission ring as an estimate for the projected outer disc velocity, we constrain the maximum projected velocity of the secondary to be 200 km s−1, placing a lower limit of 0.05 M⊙ on the secondary mass. For a 1.4 M⊙ primary, this implies that the orbital inclination is low, ≲20°. Utilizing the observed relationship between the secondary mass and the orbital period in short-period cataclysmic variables, we estimate the secondary mass to be ∼0.085 M⊙, which implies an upper limit of ∼2.4 M⊙ for the primary mass.
ISSN:0035-8711
1365-2966
DOI:10.1111/j.1365-2966.2007.12667.x