Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ap%26ss.334..145m&link_type=abstract
Astrophysics and Space Science, Volume 334, Issue 1, pp.145-154
Astronomy and Astrophysics
Astrophysics
1
Canonical Coordinates, Superdense Star, General Relativity
Scientific paper
A family of well behaved perfect fluid balls has been derived starting with the metric potential g 44= B(1+ Cr 2) n for all positive integral values of n. For n≥4, the members of this family are seen to satisfy the various physical conditions e.g. c 2 ρ≥ p≥0, dp/ dr<0, dρ/ dr<0, along with the velocity of sound (sqrt{dp/c2dρ} )< 1 and the adiabatic index (( p+ c 2 ρ)/ p)( dp/( c 2 dρ))>1. Also the pressure, energy density, velocity of sound and ratio of pressure and energy density are of monotonically decreasing towards the pressure free interface ( r= a). The fluid balls join smoothly with the Schwarzschild exterior model at r= a. The well behaved perfect fluid balls so obtained are utilised to construct the superdense star models with their surface density 2×1014 gm/cm3. We have found that the maximum mass of the fluid balls corresponding to various values of n are decreasing with the increasing values of n. Over all maximum mass for the whole family turns out to be 4.1848 M Θ and the corresponding radius as 19.4144 km while the red shift at the centre and red shift at surface as Z 0=1.6459 and Z a =0.6538 respectively this all happens for n=4. It is interesting to note that for higher values of n viz n≥170, the physical data start merging with that of Kuchowicz superdense star models and hence the family of fluid models tends to the Kuchowicz fluid models as n→∞. Consequently the maximum mass of the family of solution can not be less than 1.6096 M Θ which is the maximum mass occupied by the Kuchowicz superdense ball. Hence each member of the family for n≥4 provides the astrophysical objects like White dwarfs, Quark star, typical neutron star.
Gupta Y. K.
Maurya Sunil Kumar
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