Dependence of STM Images οn Bias Polarity for Sm Layers οn Mo(110) and Mo(211) Surfaces

Kuchowicz, M.; Szukiewicz, R.; Grodzińska, D.

doi:10.12693/aphyspola.114.s-59

Cited by 1 publication

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“…c 2 ρ ≥ p ≥ 0, dp/dr < 0, dρ/dr < 0, along with the causality condition (dp/c 2 dρ) < 1 and the adiabatic index ((p + c 2 ρ)/p)(dp/(c 2 dρ)) > 1 for 0 ≤ r ≤ a, such that p = 0 at r = a. Some of the remarkable perfect fluid solution by assuming metric potential g 11 are due to Schwarzschild (1916) interior solution, Tolman (1939), Wyman (1949, Patwardhan and Vaidya (1943), Buchdahl (1959), Kuchowich (1967b, 1968a, 1968b, Bayin (1978), Vaidya and Tikekar (1982), Finch and Skea (1989), Mukherjee et al (1997), and Gupta and Jasim (2000).…”

Section: Introductionmentioning

confidence: 99%

On a family of well behaved perfect fluid balls as astrophysical objects in general relativity

Maurya

Gupta

2011

Astrophys Space Sci

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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 ( dp/c 2 dρ) < 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 × 10 14 gm/cm 3 . 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 4.1848M 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 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.

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