Probing the nova shock physics with future gamma-ray observations of the upcoming outburst from T Coronae Borealis
arxiv(2024)
摘要
Nova shocks behave like scaled-down supernova remnant shocks with a lifetime
of only a few weeks or months, thereby providing a unique opportunity to study
the dynamics of non-relativistic shocks as well as the shock acceleration
physics.Recently, GeV and TeV gamma-ray emissions from an outburst of the
recurrent nova RS Ophiuchi have been observed. The light curves of the
gamma-ray emissions suggest that they arise from an external shock, which is
formed as the nova ejecta interacts with the ambient medium. The shock is
thought to transit from an adiabatic shock to a radiative one at later times,
but no such later observations are available for RS Ophiuchi. In addition, the
spectral evolution of the gamma-ray outburst of RS Ophiuchi was not well
measured, and hence the related particle acceleration mechanisms are not well
understood. T Coronae Borealis (T CrB) is another recurrent nova in Milky Way
and its last outburst was nearly ten times brighter than RS Ophiuichi. Recently
the optical light curve of T CrB displayed a state transition behavior before
the eruption, and it was predicted that T CrB will undergo an outburst in the
near future. By performing a theoretical investigation, we find that Fermi-LAT
could capture the transition of the shock from the adiabatic phase to the
radiative phase at the GeV band, thanks to a longer detectable time than that
of RS Ophiuchi.Due to its higher brightness, we also find that imaging
atmospheric Cherenkov telescopes (IACTs) such as MAGIC and VERITAS, and
extensive air shower experiments such as LHAASO could detect the nova outburst
and measure the gamma-ray spectrum in the very-high-energy (VHE, energy above
0.1 TeV) band more precisely. This can be used to constrain the high-energy
cutoff index in the accelerated proton spectrum and the acceleration
efficiency, which will shed light on the particle acceleration physics in nova
shocks.
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