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Firm detection of 7-year X-ray periodicity from X Persei

Published online by Cambridge University Press:  30 December 2019

Motoki Nakajima ,
Hitoshi Negoro ,
Tatehiro Mihara ,
Mutsumi Sugizaki ,
Fumiaki Yatabe  and
Kazuo Makishima
Motoki Nakajima
Affiliation:
School of Dentistry at Matsudo,Nihon University, 2-870-1, Sakaecho-nishi, Matsudo, Chiba 271-8587, JAPAN email: nakajima.motoki@nihon-u.ac.jp
Hitoshi Negoro
Affiliation:
Department of Physics, Nihon University, 1-8 Kanda-Surugadai, Chiyoda-ku, Tokyo 101-8308, Japan
Tatehiro Mihara
Affiliation:
MAXI team, Institute of Physical and Chemical Research (RIKEN), 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
Mutsumi Sugizaki
Affiliation:
MAXI team, Institute of Physical and Chemical Research (RIKEN), 2-1 Hirosawa, Wako, Saitama 351-0198, Japan Department of Physics, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan
Fumiaki Yatabe
Affiliation:
MAXI team, Institute of Physical and Chemical Research (RIKEN), 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
Kazuo Makishima
Affiliation:
MAXI team, Institute of Physical and Chemical Research (RIKEN), 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
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Abstract

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We report on the detection of long-term X-ray periodicity from the Be/X-ray binary pulsar X Persei. Based on over 23 years of X-ray data observed using RXTE/ASM, Swift/BAT and MAXI/GSC, we confirmed that X Persei exhibits quasi-periodic X-ray flares with a period of ∼7 years. The recurrence timescale corresponds to approximately 10 times its binary orbital period of 250 days. Spectral and hardness ratio changes were not detected along with long-term periodic activity. If we interpret the observed 7 year periodicity of X-ray band flux as a superorbital modulation, then this would be the first observation among the Be/X-ray binaries.

Keywords

pulsars:individual(X Persei)X-rays:stars

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