Insight-HXMT science operations

Jia, S.; Ma, Xiang; Huang, Y.; Zhang, W. Z.; Ou, G.; Song, Liming; Qu, J. L.; Zhang, S.; Chen, L.

doi:10.1117/12.2315175

Cited by 3 publications

(1 citation statement)

References 2 publications

(3 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…1 • × 6 • (FWHM, full-width half maximum) (also called the small FoV), 6 • × 6 • (large FoV), and the blind FoV used to estimate the particle induced instrumental background (see 55 or The Insight-HXMT Data Reduction Guide for details). Since its launch, Insight-HXMT went through a series of performance verification tests by observing blank sky, standard sources and sources of interest.…”

Section: Data Reductionmentioning

confidence: 99%

Insight-HXMT observations of jet-like corona in a black hole X-ray binary MAXI J1820+070

You,

Tuo,

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

A black hole X-ray binary produces hard X-ray radiation from its corona and disk when the accreting matter heats up. During an outburst, the disk and corona co-evolves with each other. However, such an evolution is still unclear in both its geometry and dynamics. Here we report the unusual decrease of the reflection fraction in MAXI J1820+070, which is the ratio of the coronal intensity illuminating the disk to the coronal intensity reaching the observer, as the corona is observed to contrast during the decay phase. We postulate a jet-like corona model, in which the corona can be understood as a standing shock where the material flowing through. In this dynamical scenario, the decrease of the reflection fraction is a signature of the corona's bulk velocity. Our findings suggest that as the corona is observed to get closer to the black hole, the coronal material might be outflowing faster.

show abstract

Section: Data Reductionmentioning

confidence: 99%

Insight-HXMT observations of jet-like corona in a black hole X-ray binary MAXI J1820+070

You,

Tuo,

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

Insight-HXMT observations of jet-like corona in a black hole X-ray binary MAXI J1820+070

You

Tuo

et al. 2021

Nat Commun

View full text Add to dashboard Cite

A black hole X-ray binary produces hard X-ray radiation from its corona and disk when the accreting matter heats up. During an outburst, the disk and corona co-evolves with each other. However, such an evolution is still unclear in both its geometry and dynamics. Here we report the unusual decrease of the reflection fraction in MAXI J1820+070, which is the ratio of the coronal intensity illuminating the disk to the coronal intensity reaching the observer, as the corona is observed to contrast during the decay phase. We postulate a jet-like corona model, in which the corona can be understood as a standing shock where the material flowing through. In this dynamical scenario, the decrease of the reflection fraction is a signature of the corona’s bulk velocity. Our findings suggest that as the corona is observed to get closer to the black hole, the coronal material might be outflowing faster.

show abstract

Study on the Energy Limits of kHz QPOs in Sco X-1 with RXTE and Insight-HXMT Observations

Jia

et al. 2021

ApJ

View full text Add to dashboard Cite

We present a detailed spectral-timing analysis of the Kilohertz quasiperiodic oscillations (kHz QPOs) in Sco X-1 using the data of the Rossi X-ray Timing Explorer (RXTE) and the Hard X-ray Modulation Telescope (Insight-HXMT). The energy band with detectable kHz QPOs is studied for the first time: on the horizontal branch, it is ∼6.89–24.01 and ∼8.68–21.78 keV for the upper and lower kHz QPOs, respectively, detected by the RXTE, and ∼9–27.5 keV for the upper kHz QPOs by the Insight-HXMT; on the lower normal branch, the energy band is narrower. The fractional root mean square (rms) of the kHz QPOs increases with energy at a lower energy, reaches a plateau at about 16 and 20 keV for the lower and upper peaks, and then levels off though with a large uncertainty. The simulation of the deadtime effect of RXTE/PCA shows that the deadtime does not affect much the search of the kHz QPOs but makes the rms amplitude underestimated. No significant QPO is detected below ∼6 keV as shown by the RXTE data, implying that the kHz QPOs do not originate from the blackbody emission of the accretion disk and neutron star surface. In addition, with the combined analysis of the energy spectra and the absolute rms spectra of kHz QPOs, we suggest that the kHz QPOs in Sco X-1 originate from the Comptonization of the inner part of the transition layer, where the rotation sets the frequency and the inward bulk motion makes the spectrum harder.

show abstract

Insight-HXMT science operations

Cited by 3 publications

References 2 publications

Insight-HXMT observations of jet-like corona in a black hole X-ray binary MAXI J1820+070

Insight-HXMT observations of jet-like corona in a black hole X-ray binary MAXI J1820+070

Insight-HXMT observations of jet-like corona in a black hole X-ray binary MAXI J1820+070

Study on the Energy Limits of kHz QPOs in Sco X-1 with RXTE and Insight-HXMT Observations

Contact Info

Product

Resources

About