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The accreting millisecond pulsar XTE J1807-294 was observed by XMM-Newton onMarch 22, 2003 after its discovery on February 21, 2003 by RXTE. The source wasdetected in its bright phase with an observed average count rate of 33.3 cts/sin the EPIC-pn camera in the 0.5-10 keV energy band (3.7 mCrab). Using theearlier established best-fit orbital period of 40.0741+/-0.0005 minutes fromRXTE observations and considering a circular binary orbit as firstapproximation, we derived a value of 4.8+/-0.1 lt-ms for the projected orbitalradius of the binary system and an epoch of the orbital phase of MJD52720.67415(16). The barycentric mean spin period of the pulsar was derived as5.2459427+/-0.4 ms. The pulsar's spin-pulse profile showed a prominent(1.5 ms FWHM) pulse, with energy and orbital phase dependence in the amplitudeand shape. The measured pulsed fraction in four energy bands was found to be3.1+/-0.2 % (0.5-3.0 keV), 5.4+/-0.4 % (3.0-6.0 keV), 5.1+/-0.7 % (6.0-10.0keV) and 3.7+/-0.2 % (0.5-10.0 keV), respectively. Studies of spin-profileswith orbital phase and energy showed significant increase in its pulsedfraction during the second observed orbit of the neutron star, graduallydeclining in the subsequent two orbits, which was associated with sudden butmarginal increase in mass accretion. From our investigations of orbitalparameters and estimation of other properties of this compact binary system, weconclude that XTE J1807-294 is very likely a candidate for a millisecond radiopulsar.Comment: 4 pages, 4 figures, Accepted for publication in Astronomy and  Astrophysics letter

Studies of orbital parameters and pulse profile of the accreting millisecond pulsar XTE J1807–294