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Orbital evolution and search for eccentricity and apsidal motion in the eclipsing HMXB 4U 1700-37

Islam, Nazma and Paul, Biswajit (2016) Orbital evolution and search for eccentricity and apsidal motion in the eclipsing HMXB 4U 1700-37. In: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 461 (1). pp. 816-824.

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Official URL: http://dx.doi.org/10.1093/mnras/stw1299


In the absence of detectable pulsations in the eclipsing high-mass X-ray binary 4U 1700-37, the orbital period decay is necessarily determined from the eclipse timing measurements. We have used the earlier reported mid-eclipse time measurements of 4U 1700-37 together with the new measurements from long-term light curves obtained with the all sky monitors RXTE-ASM, Swift-BAT and MAXI-GSC, as well as observations with RXTE-PCA, to measure the long-term orbital evolution of the binary. The orbital period decay rate of the system is estimated to be (P)over dot/P = -(4.7 +/- 1.9) x 10(-7) yr(-1), smaller compared to its previous estimates. We have also used the mid-eclipse times and the eclipse duration measurements obtained from 10-years-long X-ray light curve with Swift-BAT to separately put constraints on the eccentricity of the binary system and attempted to measure any apsidal motion. For an apsidal motion rate greater than 5 deg yr(-1), the eccentricity is found to be less than 0.008, which limits our ability to determine the apsidal motion rate from the current data. We discuss the discrepancy of the current limit of eccentricity with the earlier reported values from radial velocity measurements of the companion star.

Item Type: Journal Article
Additional Information: Copy right for this article belongs to the OXFORD UNIV PRESS, GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
Department/Centre: Division of Physical & Mathematical Sciences > Joint Astronomy Programme
Date Deposited: 28 Oct 2016 07:19
Last Modified: 28 Oct 2016 07:19
URI: http://eprints.iisc.ac.in/id/eprint/55155

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