SIMBAD references

2015MNRAS.452L..31L - Mon. Not. R. Astron. Soc., 452, L31-L35 (2015/September-1)

Revisiting the dynamical case for a massive black hole in IC10 X-1.

LAYCOCK S.G.T., MACCARONE T.J. and CHRISTODOULOU D.M.

Abstract (from CDS):

The relative phasing of the X-ray eclipse ephemeris and optical radial velocity (RV) curve for the X-ray binary IC10 X-1 suggests that the He [λ4686] emission line originates in a shadowed sector of the stellar wind that avoids ionization by X-rays from the compact object. The line attains maximum blueshift when the wind is directly towards us at mid X-ray eclipse, as is also seen in Cygnus X-3. If the RV curve is unrelated to stellar motion, evidence for a massive black hole (BH) evaporates because the mass function of the binary is unknown. The reported X-ray luminosity, spectrum, slow QPO and broad eclipses caused by absorption/scattering in the Wolf-Rayet (WR) wind are all consistent with either a low-stellar-mass BH or a neutron star (NS). For an NS, the centre of mass lies inside the WR envelope whose motion is then far below the observed 370 km/s RV amplitude, while the velocity of the compact object is as high as 600 km/s. The resulting 0.4 per cent Doppler variation of X-ray spectral lines could be confirmed by missions in development. These arguments also apply to other putative BH binaries whose RV and eclipse curves are not yet phase-connected. Theories of BH formation and predicted rates of gravitational wave sources may need revision.

Abstract Copyright: © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2015)

Journal keyword(s): accretion, accretion discs - black hole physics - circumstellar matter - stars: neutron - X-rays: binaries

Status at CDS:  

Simbad objects: 10

goto Full paper

goto View the reference in ADS

To bookmark this query, right click on this link: simbad:2015MNRAS.452L..31L and select 'bookmark this link' or equivalent in the popup menu


2020.06.07-01:06:02

© Université de Strasbourg/CNRS

    • Contact