Figure 7 - uploaded by Xiang Liu
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Distribution of the jet efficiency versus the 1-10 keV X-ray Eddington ratio L X /L Edd in the 'outlier' track. The blue circles represent H1743-322 and orange squares represent MAXI J1348-630.
Source publication
In this paper, we investigate the black hole (BH) spin contribution to jet power, especially for the magnetic arrested disk (MAD), where only inner accretion disk luminosity is closely coupled with the spin-jet power, and try to explain the ‘outliers’ track of the radio LR to X-ray luminosity LX in two black hole X-ray binaries (BHXBs). Our results...
Context in source publication
Context 1
... we use the total bolometric luminosity L bol instead of the inner-disk luminosity L in , as L in is a function of the jet power P jet from Equation (4). Figure 7 shows the plot of the relationship between jet efficiency, η jet , and L X /L Edd for both sources in their 'outlier' track; the blue circles represent H1743-322 and the orange squares represent MAXI J1348-630, as labeled in the plot. Here, we estimate the bolometric luminosity L bol from the X-ray bolometric correction factor f X = 5, as in Section 3. First, those two sources show different tendencies; H1743-322 shows an uptrend correlation, while the η jet of MAXI J1348-630 is negatively correlated with L X /L Edd when L X /L Edd 10 −2 and is not correlated with L X /L Edd when L X /L Edd 10 −2 . ...
Citations
... Another component that is missing in this classical picture is the collimated jet [17], which can be a significant source of the X-ray emission in the hard state, and it is shown to dominate the X-ray emission in the quiescent state [18]. Recent studies showed that the jet contribution itself depends on the BH spin [19]. Reproduced with permission from Ramesh Narayan and ApJ. ...
... Another component that is missing in this classical picture is the collimated jet [17], which can be a significant source of the X-ray emission in the hard state, and it is shown to dominate the X-ray emission in the quiescent state [18]. Recent studies showed that the jet contribution itself depends on the BH spin [19]. ...
Low-mass X-ray binaries (LMXB) serve as natural laboratories, where the predictions of general relativity can be tested in the strong field regime. The primary object of such sources can be a neutron star (NS) or a black hole (BH), and this object captures material from the secondary object through the inner Lagrange point via a process called Roche lobe overflow. Because of the angular momentum of the infalling matter, an accretion disk is formed, in which viscous effects transport the angular momentum radially outward. In the high/soft state of these sources, the accretion disk can extend all the way to the innermost stable circular orbit (ISCO); therefore, when the primary object is a BH, its X-ray spectrum contains information about the region very close to the event horizon. This paper aims to review the theoretical and observational works related to the X-ray spectroscopy of such sources via the example of GX 339-4, which is one of the most well-known and well-studied LMXBs.
