EDP Sciences
Free access
Volume 479, Number 2, February IV 2008
Page(s) 301 - 306
Section Astrophysical processes
DOI http://dx.doi.org/10.1051/0004-6361:20078721

A&A 479, 301-306 (2008)
DOI: 10.1051/0004-6361:20078721

Recent RXTE/ASM and ROTSEIIId observations of EXO 2030+375 (V2246 Cygni)

A. Baykal, Ü. Kiziloglu, N. Kiziloglu, E. Beklen, and M. Özbey

Physics Department, Middle East Technical University, Ankara 06531, Turkey
    e-mail: altan@astroa.physics.metu.edu.tr

(Received 23 September 2007 / Accepted 2 December 2007)

Aims.Using the archival RXTE/ASM and SWIFT/BAT observations, the new orbital phases of type I outbursts of EXO 2030+375 are estimated. A possible correlation between the type II outburst and optical brightness variations is investigated.
Methods.In order to estimate the phases of type I outbursts, we fitted Gaussian profiles to the RXTE/ASM and SWIFT/BAT light curves. The time corresponding to the maximum value of the profiles is treated as the arrival time of type I outburst. We used differential magnitudes in the time-series analysis of the optical light curve. MIDAS and its suitable packages were used to reduce and analyze the spectra.
Results.Prior to the type II outburst, orbital phases of type I outbursts were delayed for ~6 days after the periastron passage, which is consistent with findings of Wilson et al. (2002, ApJ, 570, 287; 2005, ApJ, 620, L99). After the giant type II outburst, the phase of type I outbursts underwent a sudden shift of ~13 days after the periastron passage. The amplitudes of type I outbursts were increased between MJD ~ 52 500 and ~53 500. These amplitudes then decreased for 10 orbital cycles until the type II outburst was triggered. If the change of outburst amplitudes correlated with the mass accretion, then during the decrease of these amplitudes mass should be deposited in a disk around neutron star temporarily. The release of this stored mass may ignite the type II outburst. We report that the optical light curve became fainter by 0.4 mag during the decrease of amplitude of the type I outbursts. The observed H$\alpha$ profiles and their equivalent widths during the decay and after the giant outburst are consistent with previous observations of the system.

Key words: accretion, accretion disks -- X-rays: stars

© ESO 2008