On the mass defect of strange stars

On the anomalous mass defect of strange stars in the Field Correlator Method

“…The stellar sequence present three branches delimited at the labeled points 1 and 2, where the solid and dashed curves cross itself, and in which M = M A , as shown in panel (a). In the intermediate branch we have M < M A , required by the stability conditions against transition to diffuse matter.We have M > M A at densities ∼ 10 15 g cm −3 in the first branch 2 , and > 5.5 × 10 16 g cm −3 in the third branch.An investigation of strange stars within BM, for the values of the bag constant in the range 50 MeV fm −3 ≤ B ≤ 70 MeV fm −3 , showed the absence of the anomalous mass defect in strange stars[50]. Anomalous mass defects does not have been obtained because of the low used values of B, which numerically correspond (in our calculation with V 1 = 0) to lower values of ∆|ε vac.…”

“…The total energy of the observed neutrinos was found to be ∼ 3×10 53 erg. It was pointed out that one signal might have been originated in the formation of a neutron star after the supernova explosion and the other signal in a possible formation of a strange star [50]. It is inquisitive that the values of |∆ 2 M| along the tail in panel (b) of Fig.…”

“…For the sake of comparison with the BM, the open circles along the V 1 = 0 curve correspond to the values of B used in Refs. [12][13][14][15][49][50][51].…”

“…There is some freedom to choose the baryonic mass. In earlier texts, the baryonic mass was taken as the mass m H of the hydrogen atom [3]; the 56 F e mass per baryon m 0 ≡ m( 56 Fe)/56 [14,[47][48][49][50]; or the neutron mass m n [4,5,38,46]. We here assume m A = m n , as in Ref.…”

On Schwarzschild’s Interior Solution and Perfect Fluid Star Model

“…That spherically symmetric solutions such as {g a : −2m < a < a 1 } where a 1 = 9r 2 0 4 (r 0 − 2m) − 2m, cf. (51) are appropriate for the calculation of mass defect of strange stars appears to be accounted for by [11].…”