Volume 421, Number 2, July II 2004
|Page(s)||673 - 680|
|Section||Stellar structure and evolution|
|Published online||22 June 2004|
Discovery of the optical counterpart to the X-ray pulsar SAX J2103.5+4545
GACE, Instituto de Ciencias de los Materiales, Universitad de Valencia, 46071 Paterna-Valencia, Spain e-mail: [pere.blay; rachid.chato]@uv.es
2 University of Crete, Physics Department, PO Box 2208, 710 03 Heraklion, Crete, Greece e-mail: firstname.lastname@example.org
3 Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante, 03080 Alicante, Spain e-mail: email@example.com
4 Observatorio Astronómico de Valencia, Universitad de Valencia, 46071 Paterna-Valencia, Spain e-mail: firstname.lastname@example.org
Corresponding author: P. Reig, email@example.com
Accepted: 26 March 2004
We report optical and infrared photometric and spectroscopic observations that identify the counterpart to the 358.6-s X-ray transient pulsar SAX J2103.5+4545 with a moderately reddened B0Ve star. This identification makes SAX J2103.5+4545 the Be/X-ray binary with the shortest orbital period known, days. The amount of absorption to the system has been estimated to be , which for such an early-type star implies a distance of about 6.5 kpc. The optical spectra reveal major and rapid changes in the strength and shape of the Hα line. The Hα line was initially observed as a double peak profile with the ratio of the intensities of the blue over the red peak greater than one (). Two weeks later this ratio reversed (). Subsequently, in less than a month, the emission ceased and Hα appeared in absorption. This fast spectral variability is interpreted within the viscous decretion disc model and demonstrates the significant role of the neutron star on the evolution of the circumstellar disc around the Be star. The implications of the small orbit and moderate eccentricity on the spin period of the neutron star are discussed.
Key words: stars: individual: SAX J2103.5+4545 / X-rays: binaries / stars: neutron / stars: binaries: close / stars: emission-line, Be
© ESO, 2004
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