Abstract



Radiative blast waves (BW) in supernova remnants (SNR) remain a difficult subject nowadays. The SNR expansion is usually decomposed in three stages [1, 2]. First the ballistic phase where the radius, R(t), of the SNR is proportional to the time [3], second the SedovTaylor regime [4] described by a well understood selfsimilar expansion, 2/5 R(t) ?t (in spherical geometry), and third a radiative stage with ( ) q R t ? t and 1 / 4 ? q ? 2 / 5 , where the radiative cooling of the expanding flow produces the formation of a thin dense cold shell until thermal energy of all the swept gas is rapidly radiated and as consequence the thin shell enters in a MomentumConserving (MC) phase, with 1/4 R(t) ?t [1,2]. In this former stage the internal pressure of the shell produces its expansion and the end of BW. One of the main difficulty describing theoretically and selfconsistently BW is that adiabatic shocked shell selfsimilar solutions do not exists for q ? 2 / 5 [5]. Hence in order to take into account, phenomenologically, the cooling rate, the ratio of specific heats, ? , for the gas behind the shock, has been chosen in the literature close to unity [6]. However, following this approach, even for the very small and unrealistic values of ? , the growth rate of instability is much weaker than the RayleighTaylor growth rate and hence cannot explain in our opinion the instability and fragmentation observed in SNR. In order to cover this lack of selfsimilar solutions in the third stage of SNR expansions we have relaxed the adiabatic assumption by including a cooling function ? , only depending on time, ( ) r ? t ?t . The rigorous 1D selfsimilar solution is derived provided the exponent satisfy r ? 2q ? 3 where the expansion rate, q , can be less than 2 / 5. The solution is governed by a dimensionless cooling parameter 0 0 / c p? ? v t Bo . Here Bo is the Boltzmann number of the flow, p ? is a mean volume Planck opacity, and 0 v and 0 t are the characteristic velocity and the hydrodynamic time, respectively, of the BW. Two main results arise. First, even with energy losses, the dynamics with q = 2/5 (Sedov exponent) still exists and, second, for c ? larger than unity the profile of density decreases with radial coordinate, in contrast to the adiabatic case, and the growth rate of the instability becomes much larger than the one derived by Ryu and Vishniac [6]. [1] Chevalier, R. A. 1977, Annual Review of Astronomy and Astrophysics, 15, 175. [2] Woltjer, L. 1972, Annual Review of Astronomy and Astrophysics, 10, 129. [3] Truelove, J. K. & McKee, C. F. 1999, Astrophys. J. Suppl. Ser., 120, 299. [4] Sedov, L. I. 1959, Similarity and Dimensional Methods in Mechanics, ed. Sedov, L. I.; Taylor, G. 1950, Royal Society of London Proceedings Series A, 201, 159; von Neumann, J. 1947, The Point Source Solution. Blast Wave, ch. 2 (Los Alamos Sci. Lab Tech Series, VII Pt. II). [5] Sanz, J., Bouquet, S. & Murakami, M. 2011, App&SS, 363, 195. [6] Ryu, D. & Vishniac, E. T. 1987, Astrophys. J., 313, 820.  
International

Si 
Place

CEA  París 
Type

Miembros en el extranjero 
Start Date

01/09/2011 
End Date

31/10/2012 