2021MNRAS.503.6045D

Query : 2021MNRAS.503.6045D

2021MNRAS.503.6045D - Mon. Not. R. Astron. Soc., 503, 6045-6058 (2021/June-1)

QPOs and orbital elements of X-ray binary 4U 0115+63 during the 2017 outburst observed by Insight-HXMT.

DING Y.Z., WANG W., ZHANG P., BU Q.C., CAI C., CAO X.L., ZHI C., CHEN L., CHEN T.X., CHEN Y.B., CHEN Y., CHEN Y.P., CUI W.W., DU Y.Y., GAO G.H., GAO H., GE M.Y., GU Y.D., GUAN J., GUO C.C., HAN D.W., HUANG Y., HUO J., JIA S.M., JIANG W.C., JIN J., KONG L.D., LI B., LI C.K., LI G., LI T.P., LI W., LI X., LI X.B., LI X.F., LI Z.W., LIANG X.H., LIAO J.Y., LIU B.S., LIU C.Z., LIU H.X., LIU H.W., LIU X.J., LU F.J., LU X.F., LOU Q., LUO T., MA R.C., MA X., MENG B., NANG Y., NIE J.Y., QU J.L., REN X.Q., SAI N., SONG L.M., SONG X.Y., SUN L., TAN Y., TAO L., TUO Y.L., WANG C., WANG L.J., WANG P.J., WANG W.S., WANG Y.S., WEN X.Y., WU B.Y., WU B.B., WU M., XIAO G.C., XIAO S., XIONG S.L., XU Y.P., YANG R.J., YANG S., YANG Y.J., YI Q.B., YIN Q.Q., YOU Y., ZHANG F., ZHANG H.M., ZHANG J., ZHANG P., ZHANG S., ZHANG S.N., ZHANG W.C., ZHANG W., ZHANG Y.F., ZHANG Y.H., ZHAO H.S., ZHAO X.F., ZHENG S.J., ZHENG Y.G. and ZHOU D.K.

Abstract (from CDS):

In this paper, we presented a detailed timing analysis of a prominent outburst of 4U 0115+63 detected by Insight-HXMT in 2017 August. The spin period of the neutron star was determined to be 3.613 98 ± 0.000 02 s at MJD 57978. We measured the period variability and extract the orbital elements of the binary system. The angle of periastron evolved with a rate of 0.048○±0.003○yr-1^. The light curves are folded to sketch the pulse profiles in different energy ranges. A multipeak structure in 1-10 keV is clearly illustrated. We introduced wavelet analysis into our data analysis procedures to study quasi-periodic oscillation (QPO) signals and perform a detailed wavelet analysis in many different energy ranges. Through the wavelet spectra, we report the discovery of a QPO at the frequency of ∼10 mHz. In addition, the X-ray light curves showed multiple QPOs in the period of ∼16-32 and ∼67-200 s. We found that the ∼100 s QPO was significant in most of the observations and energies. There exist positive relations between X-ray luminosity and their Q-factors and S-factors, while the QPO periods have no correlation with X-ray luminosity. In wavelet phase maps, we found that the pulse phase of ∼67-200 s QPO is drifting frequently while that of ∼16-32 s QPO is scarcely drifting. The dissipation of oscillations from high energy to low energy was also observed. These features of QPOs in 4U 0115+63 provide a new challenge to our understanding of their physical origins.

Abstract Copyright: © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society

Journal keyword(s): stars: individual: 4U 0115+63 - X-rays: binaries - X-rays: stars

Simbad objects: 3

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Number of rows : 3
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 V* V635 Cas HXB 01 18 31.9704955824 +63 44 33.072603144 17.05 16.64 15.19 14.34 13.22 B0.2Ve 791 0
2 MAXI J1535-571 XB* 15 35 19.73 -57 13 48.1           ~ 214 0
3 MAXI J1820+070 LXB 18 20 21.9423816480 +07 11 07.284859440           ~ 511 0

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