Samenvatting
We present a systematic spectral-timing analysis of a fast
appearance/disappearance of a type-B quasi-periodic oscillation (QPO),
observed in four NICER observations of MAXI J1348-630. By comparing the
spectra of the period with and without the type-B QPO, we found that the
main difference appears at energy bands above ~2 keV, suggesting that
the QPO emission is dominated by the hard Comptonised component. During
the transition, a change in the relative contribution of the disk and
Comptonised emission was observed. The disk flux decreased while the
Comptonised flux increased from non-QPO to type-B QPO. However, the
total flux did not change too much in the NICER band. Our results reveal
that the type-B QPO is associated with a redistribution of accretion
power between the disk and Comptonised emission. When the type-B QPO
appears, more accretion power is dissipated into the Comptonised region
than in the disk. Our spectral fits give a hint that the increased
Comptonised emission may come from an additional component that is
related to the base of the jet.
Originele taal-2 | English |
---|---|
Pagina's (van-tot) | 3823-3843 |
Tijdschrift | Monthly Notices of the Royal Astronomical Society |
Volume | 505 |
Nummer van het tijdschrift | 3 |
DOI's | |
Status | Published - 31-mei-2021 |