2009
DOI: 10.1007/s00033-009-0031-1
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Non-relativistic global limits of entropy solutions to the extremely relativistic Euler equations

Abstract: We are concerned in this paper with the non-relativistic global limits of the entropy solutions to the Cauchy problem of 3 × 3 system of relativistic Euler equations modeling the conservation of baryon numbers, momentum, and energy respectively. Based on the detailed geometric properties of nonlinear wave curves in the phase space and the Glimm's method, we obtain, for the isothermal flow, the convergence of the entropy solutions to the solutions of the corresponding classical non-relativistic Euler equations … Show more

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Cited by 24 publications
(13 citation statements)
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References 31 publications
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“…ÂdS D de C pd  1 n à with special entropy S, the state equations for polytropic gas can be given as (cf. [11]) We consider the Cauchy problem for Equations 1.1 and 1.10 with the following data:…”
Section: Combining the First Law Of Thermodynamics (Gibbs Equation)mentioning
confidence: 99%
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“…ÂdS D de C pd  1 n à with special entropy S, the state equations for polytropic gas can be given as (cf. [11]) We consider the Cauchy problem for Equations 1.1 and 1.10 with the following data:…”
Section: Combining the First Law Of Thermodynamics (Gibbs Equation)mentioning
confidence: 99%
“…n, , p are the baryon number, the mass-energy density and the pressure, respectively, and they satisfy the following relation: 11) equation in Equation (1.10). This has the effect of deleting the particle rest energy contribution from energy equation and makes the passage to the non-relativistic limit more straightforward.…”
Section: Introductionmentioning
confidence: 99%
“…We know that (5.1) is the formal limit of (1.1) as c → +∞, which can be derived similarly as in [11]. We need to take a look at the elementary waves to the Riemann problem of (5.1) and (1.8).…”
Section: Zampmentioning
confidence: 99%
“…T dS = de + p d 1 n with specific entropy S, the equations of state for polytropic gas can be given as [11] p = (γ − 1)c 2 (ρ − n), (1.4) and p = n γ exp (γ − 1)(S − S 0 ) R . (1.5) For simplicity, hereinafter we will take the speed of light c = 1.…”
Section: Introductionmentioning
confidence: 99%
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