NO X-RAYS FROM THE VERY NEARBY TYPE Ia SN?2014J: CONSTRAINTS ON ITS ENVIRONMENT

摘要

Deep X-ray observations of the post-explosion environment around the very nearby Type Ia SN?2014J (d L = 3.5 Mpc) reveal no X-ray emission down to a luminosity Lx 7 × 1036 erg s–1 (0.3-10?keV) at δt ~ 20 days after the explosion. We interpret this limit in the context of inverse Compton emission from upscattered optical photons by the supernova shock and constrain the pre-explosion mass-loss rate of the stellar progenitor system to be (for wind velocity vw = 100 km s–1). Alternatively, the SN shock might be expanding into a uniform medium with density n CSM 3 cm–3. These results rule out single-degenerate (SD) systems with steady mass loss until the terminal explosion and constrain the fraction of transferred material lost at the outer Lagrangian point to be ≤1%. The allowed progenitors are (1) white dwarf-white dwarf progenitors, (2) SD systems with unstable hydrogen burning experiencing recurrent nova eruptions with recurrence time t 300 yr, and (3) stars where the mass loss ceases before the explosion.