Ամսագրի կամ հրապարակման վերնագիր:
Հրապարակման ամսաթիվ:
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Ստեղծողը:
Yeghikyan, A. ; Rah, M. ; Shamyar, S. ; Khachatryan, S.
Խորագիր:
Astrometry ; Space Sciences ; Archaeoastronomy and Astronomy in Culture
Չվերահսկվող բանալի բառեր:
shock waves, ISM ; clouds, ISM ; molecules, astrochemistry, methods ; numerical
Ծածկույթ:
Ամփոփում:
Water ice has been detected in several supernova remnants (SNRs) despite the highly excited and irradiated environment, challenging standard dust processing paradigms. Using two-dimensional magnetohydrodynamic (MHD) simulations with the PLUTO code, we model the early-time interaction between an SNR blast wave and a dense interstellar cloud to identify the physical conditions conducive to ice formation. Our adiabatic simulation (without radiative cooling) demonstrates that shock compression produces high-density regions (n ∼ 104 to 105 cm−3) with compression factors of 4 to 10, comparable to observations in IC 443. Although adiabatic temperatures remain elevated (T ∼ 107 to 108 K), we estimate radiative cooling timescales of ∼650 yr (for n = 104 cm−3) to ∼65 yr (n = 105 cm−3), much shorter than typical SNR ages. These results establish that the SNR shock-cloud interactions create the necessary dynamical preconditions (high density and strong compression) for the formation of H2O ice. Future simulations incorporating radiative cooling and grain surface chemistry will directly demonstrate ice mantle growth in these compressed clumps.