Volume 612, April 2018
|Number of page(s)||8|
|Section||Stellar structure and evolution|
|Published online||13 April 2018|
Energy scaling of the “heartbeat” pulse width of GRS 1915+105, IGR J17091−3624, and MXB 1730−335 from Rossi-XTE observations
Università degli Studi di Cagliari – Dipartimento di Fisica, Complesso Universitario di Monserrato,
S.P. Monserrato-Sestu km 0,700,
Monserrato (CA), Italy
2 INAF, IAPS, via del Fosso del Cavaliere 100, 00113 Roma, Italy
3 INFN, Sezione Roma 1, Piazzale A. Moro 2, 00185 Roma, Italy
4 In Unam Sapientiam, Piazzale A. Moro 5, 00185 Roma, Italy
5 INAF, IASF Palermo, via U. La Malfa 153, 90146 Palermo, Italy
Accepted: 15 January 2018
We investigate some key aspects of the “heartbeat” variability consisting of series of bursts with a slow rise and a fast decay, thus far detected only in GRS 1915+105, IGR J17091−3624, and MXB 1730−335. A previous analysis based on BeppoSAX data of GRS 1915+105 revealed a hard-X delay (HXD), that is a lag of the burst rise at higher energies with respect to lower ones; this leads to narrower pulse widths, w, at higher energies. We here use some light curves of Rossi-XTE observations of GRS 1915+105 for a deeper analysis of this effect and search for its presence in those extracted from some IGR J17091−3624 and MXB 1730−335 observations performed with the same satellite. Our results show that, at variance with GRS 1915+105, no HXD is evident in the light curves of MXB 1730−335 and only a marginal HXD may be argued for IGR J17091−3624. For GRS 1915+105 we find a decreasing trend of the pulse width with energy following a power law w = A ⋅ E−s with an index s ≈ 0.8. Furthermore, we confirm the increase of the HXD with the recurrence time Trec of the bursts in each series that was already found in previous works using BeppoSAX data. Based on a spectral analysis of these three sources we conclude that the differences highlighted in the properties of the “heartbeat” variability are probably related to the different accreting compact object and the eventual presence of a corona in these binary interacting systems.
Key words: binaries: close / X-rays: stars / X-rays: individuals: GRS 1915+105 / X-rays: individuals: IGR J17091–3624 / X-rays: individuals: MXB 1730–335
© ESO 2018
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