Magnetars are strongly magnetized neutron stars with surface magnetic fields of ~10 14 G. Based on observational and theoretical studies, 7 soft gamma.

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Presentation transcript:

Magnetars are strongly magnetized neutron stars with surface magnetic fields of ~10 14 G. Based on observational and theoretical studies, 7 soft gamma repeaters and 9 anomalous X-ray pulsars are generally known as the magnetars. Their persistent emission consists of a thermal component ( 10 keV; e.g., Enoto et al. 2010). Some of them presented a flux increasing by a factor of 2  3 accompanied by high burst activities and/or enhanced emission with unusual spectral properties (e.g., [1]). Their continuous monitoring is crucial, since comparisons of properties between low and high flux phases give useful information in order to reveal radiation mechanisms. Thanks to a wide field of view and a better sensitivity than RXTE by a factor of a few in a 2-30 keV range of the MAXI/GSC, it is suitable for this purpose. We analyzed the magnetars, and detected at least AXP 4U (~3 mCrab; >10  ) and AXP 1E (~1.5 mCrab; >14  ) using 1 and 4 week data, respectively. We report the first MAXI/GSC view of the magnetars on long-term variability. The First MAXI/GSC View of Galactic Magnetars Yujin E. Nakagawa, Tatehiro Mihara, Mutsumi Sugizaki, Mitsuhiro Kohama, Takayuki Yamamoto, Motoko Suzuki, Masaru Matsuoka (Institute of Physical and Chemical Research), Nobuyuki Kawai, Mikio Morii, Ryuichi Usui, Kohsuke Sugimori (Tokyo Institute of Technology), Atsumasa Yoshida, Kazutaka Yamaoka, Satoshi Nakahira (Aoyama Gakuin University), Hitoshi Negoro, Motoki Nakajima (Nihon University), Naoki Isobe (Kyoto University) and MAXI Team ( 1. Magnetars 2. MAXI/GSC Views of Magnetars 3. AXP 4U AXP 1E References Highly magnetized neutron stars with B surface ~ G [2]. Emissions through magnetic energy dissipation. A typical cross-section of magnetars. B ~ G crust (neucleus, e  ) solid (e , n) e , p, n (superfluid) quark? R ~ 10 km  ~ g cm  3 X- and  -ray Emitting Magnetars ① Soft Gamma Repeaters (SGRs) : 7 Objects ② Anomalous X-ray Pulsars (AXPs) : 9 Objects Properties of SGRs and AXPs Pulse periods of P ~ 2  12 s. Located in the Galactic plane. X- and  -ray persistent emissions. Sporadic burst activities. Hard X-ray emission at >10 keV Energy (keV) Low Temp. BB High Temp. BB Hard X-ray Emission INTEGRAL [5] Low Temp. BB High Temp. BB Hard X-ray Emission ~100 ms SGR A typical light curve of short bursts Observed with HETE-2 [3]. A schematic view of a typical spectrum of persistent emission [4]. A spectrum of low fluence short bursts observed with Suzaku [6]. [1] Kaneko et al [2] Duncan & Thompson 1992 [3] Nakagawa et al AXP 4U SGR r = 1.5 deg SGR r = 1.5 deg SGR SGR r = 1.5 deg 2009/08/15—2010/06/24 r = 1.5 deg SGR (in the nearby galaxy) SGR (Candidate) r = 1.5 deg 2009/08/15—2010/07/ /08/15—2010/07/ /08/15—2010/07/ /08/15—2010/07/21 Images of SGRs in 2-10 keV Images of AXPs in 2-10 keV SGR SGR SGR (Candidate) AXP 1RXS J AXP 1E AXP 1E r = 1.5 deg AXP XTE J AXP 1E r = 1.5 deg AXP 4U r = 1.5 deg AXP 1E r = 1.5 deg ~31  ~44  2009/08/15—2010/07/ /08/15—2010/07/ /08/15—2010/07/ /08/15—2010/07/ /08/15—2010/06/24 AXP AX J AXP CXOU J AXP CXOU J (in the nearby galaxy) PSR J (Candidate) CXOU J (Candidate) 32BIT ETA CAR 32BIT 4U BIT 4U BIT GX /08/15—2010/07/ /08/15—2010/11/ /08/15—2010/07/ /08/15—2010/07/ /08/15—2010/07/15 32BIT 2009/08/15—2010/11/24 32BIT 2009/08/15—2010/11/23 64BIT 2009/10/30—2010/07/23 Model : 2BB (d = 2.5 kpc) kT LT = 0.58+/-0.04 [keV] R LT = 2.2 (-0.3, +1.4) [km] kT HT = 2.0(-0.3, +0.5) [keV] R HT = 0.14 (-0.05, +0.07) [km] F(2-10keV) = (8.3+/-1.2)× [erg cm -2 s -1 ]  2 (d.o.f.) = 86 (82) * The errors of kT and R are 90% C.L., while the erros of the flux are 68% C.L. A Long Term Light Curve Spectra Black : 32BIT data mode Red : 64BIT data mode A Long Term Light Curve Black : 32BIT data mode Red : 64BIT data mode (1bin = 7days) [4] Nakagawa et al [5] Kuiper et al [6] Nakagawa et al in prep. Spectra Black : 32BIT data mode Red : 64BIT data mode Black : 32BIT data mode Red : 64BIT data mode (1bin = 7days) Model : wabs*(BB+PL) (d = 9 kpc) NH = 3.5 (-1.5, +1.8)×10 22 [cm -2 ] kT = 1.3+/-0.2 [keV] R = 1.3 (-0.2, +0.5) [km]  ~ 0.7 F(2-10keV) = (4.9+/-0.5)× [erg cm -2 s -1 ]  2 (d.o.f.) = 115 (92) * The errors of kT and R are 90% C.L., while the erros of the flux are 68% C.L. Burst activity? * Among them, one SGR and one AXP are located in the nearby galaxy.