## 5. Discussion and conclusionThe aim of this paper was the investigation of the properties of
rapidly rotating PNS's consisting of nuclear matter (n, p,
e An investigation of this kind should investigate the properties of PNS's and HNS's for the whole range of possible masses. So far lepton concentration profiles and entropy per baryon profiles were derived only for one fixed mass in simulations of PNS evolution (e.g. Burrows & Lattimer 1986; Keil & Janka 1995; Burrows et al. 1995). In our calculation, the extension to the whole range of masses was done by assuming that the lepton concentration and the entropy per baryon does not depend on the mass of the PNS. As a result we find that the minimum gravitational mass of a NS is determined at the earliest stage of a PNS, so that the mass of a NS formed in a Type-II supernova is larger than 0.89-1.13 , which confirms similar results of a recent investigation by Goussard et al. (1998). The exact lower limit of the NS mass depends on the used entropy per baryon in the EPNS model. The quoted mass range was obtained by using and as lower and upper limit of the entropy per baryon in the envelope of the EPNS (Burrows et al. 1995). The minimum mass of EPNS's is approximately by a factor of ten larger than the minimum stable mass of CNS's. The maximum possible baryonic mass of a CNS is always larger than the maximum possible baryonic mass of the PNS's, this means that once a PNS was formed, it cannot collapse into a black hole, if further accretion is neglected (see also Takatsuka 1995; Bombaci 1996). One exception is the case of the most massive stars rotating near or at its Kepler frequency, which possibly collapse to a black hole during their time evolution, for a discussion, see Cook et al. (1994) and Salgado et al. (1994). This statement holds for stars with a pure nucleonic/leptonic composition. If one includes hyperons and/or quarks, the maximum baryonic mass of a CNS decreases (e.g. Huber et al. 1998; Balberg et al. 1999) and may be smaller than the maximum baryonic mass of a PNS. Then, a sufficiently massive PNS may collapse to a black hole during deloptonization (Prakash et al. 1997). The maximum gravitational mass increases slightly with increasing entropy per baryon in contrast to the maximum baryonic mass (see also Prakash et al. 1997). As it was pointed out, Goussard et al. (1997) got a different result due to the use of the EOS derived by Lattimer & Swesty (1991). It turned out that the influence of rotation has several impacts on properties of PNS's and NS's. Whereas the minimum mass changes only slightly due to rotation, the effect on the maximum mass is rather large, particularly for CNS's. The central baryon density is nearly unaffected by rotation at the early stages of the evolution, whereas the impact on the the later stages is rather large. The effect on the circumferential radius decreases with increasing mass and the impact on EPNS's and LPNS's is slightly larger than the impact on CNS's. We investigated the influence of different shapes of the neutrino sphere on the structure of LPNS's. As expected, we obtained considerable differences (up to 10 %) in the circumferential radii and, due to this, in the Kepler frequency. Other properties, as the central density, are barely changed by the location of the neutrino sphere. We have also considered different temperatures in the envelope of LPNS's and HNS's. If a very high temperature of 0.6 MeV is used in the envelope instead of a constant entropy per baryon, the gross properties of the LPNS change by less than 1 %. Larger deviations were obtained if the envelope is assumed to be cold. The finite temperature effects should therefore not be neglected in the envelope. Furthermore, we obtain that the thermal effects are comparable to the effects due to trapped neutrinos. This is in contrast to the results of Prakash et al. (1997), who found the thermal effects to be much smaller than the effect of high lepton numbers. In our model we assumed that accretion onto the emerging NS stopped after the formation of the EPNS (see Burrows et al. 1995). Furthermore, we kept the angular momentum constant during the deleptonization and the thermal cooling period. Under these presumptions, we obtain a lower limit on the periods of young NS's with a typical baryonic mass of 1.5 between 1.56 and 2.22 ms, which is in accordance with similar values obtained by Goussard et al. (1997, 1998). These results support strongly the hypothesis that millisecond pulsars were accelerated due to accretion. With the same reasoning, one obtains an upper limit of the stability parameter , which is smaller, for almost all NS's, than the critical value for the onset of dynamical and secular instabilities. Kepler rotating massive CNS's possess stability parameter values up to and might therefore be secular unstable against and non-axisymmetric perturbations. Though we have assumed uniform rotation, it seems to be very reasonable that PNS's and young NS's rotate differentially (e.g. Janka & Mönchmeyer 1989). As it was found by Schaab (1998) and Goussard et al. (1998), differential rotation may considerably effect the structure of PNS's and NS's, and we will pursue our investigations to differential rotation in the future. Another issue that will be addressed in a future work is the effect of additional degrees of freedom (e.g. hyperons) on the evolution of PNS's. © European Southern Observatory (ESO) 1999 Online publication: October 4, 1999 |