摘要
We present new observations of the 'supernova impostor' SN 2010da using the Chandra X-ray Observatory and the Hubble Space Telescope. During the initial 2010 outburst, the 0.3-10 keV luminosity was observed by Swift to be ~5 × 10 38 erg s -1 and faded by a factor of ~25 in a four month period. Our two new Chandra observations show a factor of ~10 increase in the 0.35-8 keV X-ray luminosity, from~4×10 36 to 4×10 37 erg s -1 in~6months, and the X-ray spectrum is consistent in both observations with a power-law with a photon index of Γ ~0. We find evidence of X-ray spectral state changes: When SN 2010da is in a high-luminosity state, the X-ray spectrum is harder (Γ ~0) compared to the low-luminosity state (Γ ~ 1.2 ± 0.8). Using our Hubble observations, we fit the colour-magnitude diagram of the coeval stellar population to estimate a time since formation of the SN 2010da progenitor system of ≲5 Myr. Our observations are consistent with SN 2010da being a high-mass X-ray binary (HMXB) composed of a neutron star and a luminous blue variable-like companion, although we cannot rule out the possibility that SN 2010da is an unusually X-ray bright massive star. The ≲5 Myr age is consistent with the theoretically predicted delay time between the formation of a massive binary and the onset of the HMXB phase. It is possible that the initial 2010 outburst marked the beginning of X-ray production in the system, making SN 2010da possibly the first massive progenitor binary ever observed to evolve into an HMXB.