Gas Slit Camera (GSC) onboard MAXI on ISS

Mihara, T.; Nakajima, M.; Sugizaki, M.; Serino, M.; Matsuoka, M.; Kohama, M.; Kawasaki, K.; Tomida, H.; Ueno, S.; Kawai, N.; Kataoka, J.; Morii, M.; Yoshida, A.; Yamaoka, K.; Nakahira, S.; Negoro, H.; Isobe, Naoki; Yamauchi, M.; Sakurai, Ikuya

doi:10.1093/pasj/63.sp3.s623

Cited by 175 publications

(81 citation statements)

References 16 publications

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“…The outburst evolution of J0556 was observed using the MAXI/Gas Slit Camera (GSC; Mihara et al 2011). We downloaded the light curve from the MAXI archive 13 for the 2-4 keV range as Ho14 suggest that this energy range results in the highest signal-to-noise ratio.…”

Section: Maximentioning

confidence: 99%

Different Accretion Heating of the Neutron Star Crust during Multiple Outbursts in MAXI J0556–332

Parikh

Homan

Wijnands

et al. 2017

ApJL

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The transient neutron star (NS) low-mass X-ray binary MAXI J0556−332 provides a rare opportunity to study NS crust heating and subsequent cooling for multiple outbursts of the same source. We examine MAXI, Swift, Chandra, and XMM-Newton data of MAXI J0556−332 obtained during and after three accretion outbursts of different durations and brightnesses. We report on new data obtained after outburst III. The source has been tracked up to ∼1800 days after the end of outburst I. Outburst I heated the crust strongly, but no significant reheating was observed during outburst II. Cooling from ∼333 eV to ∼146 eV was observed during the first ∼1200 days. Outburst III reheated the crust up to ∼167 eV, after which the crust cooled again to ∼131 eV in ∼350 days. We model the thermal evolution of the crust and find that this source required a different strength and depth of shallow heating during each of the three outbursts. The shallow heating released during outburst I was ∼17 MeV nucleon −1 and outburst III required ∼0.3 MeV nucleon −1 . These cooling observations could not be explained without shallow heating. The shallow heating for outburst II was not well constrained and could vary from ∼0 to 2.2 MeV nucleon −1 , i.e., this outburst could in principle be explained without invoking shallow heating. We discuss the nature of the shallow heating and why it may occur at different strengths and depths during different outbursts.

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Section: Maximentioning

confidence: 99%

Different Accretion Heating of the Neutron Star Crust during Multiple Outbursts in MAXI J0556–332

Parikh

Homan

Wijnands

et al. 2017

ApJL

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“…Since the MAXI (Monitor of All-sky X-ray Image; Matsuoka et al 2009) experiment on board the International Space Station (ISS) started in 2009 August, the GSC (Gas Slit Camera; Mihara et al 2011;Sugizaki et al 2011), one of the two MAXI detectors, has been scanning almost the whole sky every 92-minute orbital cycle in the 2-30 keV band. Here we use the MAXI light curve of Sco X-1 during the period when the system was also observed by the K2 mission.…”

Section: Maxi Light Curvementioning

confidence: 99%

Sco X-1 revisited withKepler, MAXI and HERMES: outflows, time-lags and echoes unveiled

Scaringi

Maccarone

Hynes

et al. 2015

Mon. Not. R. Astron. Soc.

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Sco X-1 has been the subject of many multi-wavelength studies in the past, being the brightest persistent extra-solar X-ray source ever observed. Here we revisit Sco X-1 with simultaneous short cadence Kepler optical photometry and MAXI X-ray photometry over a 78 day period, as well as optical spectroscopy obtained with HERMES. We find Sco X-1 to be highly variable in all our datasets. The optical fluxes are clearly bimodal, implying the system can be found in two distinct optical states. These states are generally associated with the known flaring/normal branch X-ray states, although the flux distributions associated with these states overlap. Furthermore, we find that the optical power spectrum of Sco X-1 differs substantially between optical luminosity states. Additionally we find rms-flux relations in both optical states, but only find a linear relation during periods of low optical luminosity. The full optical/X-ray discrete correlation function displays a broad ≈ 12.5 hour optical lag. However during the normal branch phase the X-ray and optical fluxes are anti-correlated, whilst being correlated during the flaring branch. We also performed a Cepstrum analysis on the full Kepler light curve to determine the presence of any echoes within the optical light curve alone. We find significant echo signals, consistent with the optical lags found using the discrete cross-correlation. We speculate that whilst some of the driving X-ray emission is reflected by the disk, some is absorbed and re-processed on the thermal timescale, giving rise to both the observed optical lags and optical echoes.

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“…Although MAXI does not have any moving parts, it can scan the whole sky because the ISS itself rotates with an orbital rotation around the Earth. MAXI has two kinds of instruments: the Gas Slit Camera (GSC, Mihara et al, 2011) and Solid-state Slit Camera (SSC, Tomida et al, 2011). GSC is a slit camera using a Xe-gas proportional counter, and SSC is one using 32 X-ray CCD chips.…”

Section: Maximentioning

confidence: 99%

Latest Results of the Maxi Mission

Mihara¹

2015

Publications of The Korean Astronomical Society

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Monitor of All-sky X-ray Image (MAXI) is a Japanese X-ray all-sky surveyer mounted on the International Space Station (ISS). It has been scanning the whole sky since 2009 during every 92-minute ISS rotation. X-ray transients are quickly found by the real-time nova-search program. As a result, MAXI has issued 133 Astronomer's Telegrams and 44 Gamma-ray burst Coordinated Networks so far. MAXI has discovered six new black holes (BH) in 4.5 years. Long-term behaviors of the MAXI BHs can be classified into two types by their outbursts; a fast-rise exponential-decay type and a fast-rise flat-top one. The slit camera is suitable for accumulating data over a long time. MAXI issued a 37-month catalog containing 500 sources above a ∼0.6 mCrab detection limit at 4-10 keV in the region |b| > 10• . The SSC instrument utilizing an X-ray CCD has detected diffuse soft X-rays extending over a large solid angle, such as the Cygnus super bubble. MAXI/SSC has also detcted a Ne emission line from the rapid soft X-ray nova MAXI J0158-744. The overall shapes of outbursts in Be X-ray binaries (BeXRB) are precisely observed with MAXI/GSC. BeXRB have two kinds of outbursts, a normal outburst and a giant one. The peak dates of the subsequent giant outbursts of A0535+26 repeated with a different period than the orbital one. The Be stellar disk is considered to either have a precession motion or a distorted shape. The long-term behaviors of low-mass X-ray binaries (LMXB) containing weakly magnetized neutron stars are investigated. Transient LMXBs (Aql X-1 and 4U 1608-52) repeated outbursts every 200-1000 days, which is understood by the limit-cycle of hydrogen ionization states in the outer accretion disk. A third state (very dim state) in Aql X-1 and 4U 1608-52 was interpreted as the propeller effect in the unified picture of LMXB. Cir X-1 is a peculiar source in the sense that its long-term behavior is not like typical LMXBs. The luminosity sometimes decreases suddenly at periastron. It might be explained by the stripping of the outer accretion disk by a clumpy stellar wind. MAXI observed 64 large flares from 22 active stars (RS CVns, dMe stars, Argol types, young stellar objects) over 4 years. The total energies are 10 34 − 10 36 erg s −1 . Since MAXI can measure the spectrum (temperature and emission measure), we can estimate the size of the plasma and the magnetic fields. The size sometimes exceeds the size of the star. The magnetic field is in the range of 10-100 gauss, which is a typical value for solar flares.

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Gas Slit Camera (GSC) onboard MAXI on ISS

Cited by 175 publications

References 16 publications

Different Accretion Heating of the Neutron Star Crust during Multiple Outbursts in MAXI J0556–332

Different Accretion Heating of the Neutron Star Crust during Multiple Outbursts in MAXI J0556–332

Sco X-1 revisited withKepler, MAXI and HERMES: outflows, time-lags and echoes unveiled

Latest Results of the Maxi Mission

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